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User's guide for the APOLLO procedure (version 1.0)

1. 3 4 ballo t models i 52 do OSA EA Y S Y 3 4 HAZMAP model as Deep cese Tete e TEC dee M a EUN UR 3 4 2 EALDL3D model goat sp Ie gh Gh aia ee E W 3 4 3 TEPHRA model il ii eee pee ella hk heb wl ai 3 5 The runtinputvtiles css s ss W EOS ee E Gow e 2 0 The run script tiles nte oo E ES ee dS Postprocess of models AN Overview oe OUR bu ua dae ds e We der es 4 2 The program MODELPOSTP The library LIBAPOLLO 5 1 Routines to read an input 5 2 Routines to read a database es 5 3 Routines to read a source 5 4 Routines to read a granulometry file 5 5 Routines to read a wind profile file 5 6 Routines to output model results File formats 6 1 The terrain file format some Robb Ree eR he A eR bo Rh 6 2 The wind profile file 6 3 The granulometry file format 6 4 PDhe so rce tle formats a uo piper na wee hae wo 9 Rea d X ea hes 6 5 The model output file format 6 6 lt
2. e subroutine APOLLO_get_granulometry_value PURPOSE Gets a granulometric property nc values SINTAX call APOLLO_get_granulometry_value fname word val istat message length Description Variable fname word val istat message INPUT INPUT OUTPUT OUTPUT OUTPUT kind char char real nc int char Path including name of the file Code of the property to read Possibilities are DIAMETER Returns diameters in mm DENSITY Returns densities in kg m FRACTION Returns mass fractions nc values of the property defined by word Execution status 0 means no error Output message only if istat Z 0 5 5 Routines to read a wind profile file A wind profile file contains wind velocity and temperature at different heights and time intervals See section 6 2 for details on file format e subroutine APOLLO_get_wind_profile_point PURPOSE Gets wind properties at a height 2 SINTAX call APOLLO_get_wind_profile_point fname timesec z ux uy endsec istat message Variable fname timesec endsec istat message INPUT INPUT INPUT OUTPUT OUTPUT OUTPUT OUTPUT OUTPUT OUTPUT kind char int real real real real int int char length Description any Path including name of the file Time s after 00UTC at which data is read Height at which data is read Wind z velocity m s Wind y velocity m s Air temperature in K Time in s after OOUTC until which d
3. Pfeiffer T Costa A Macedonio G 2005 A model for the numerical simulation of tephra fall deposits J Volcanol Geotherm Res 140 273 294 Pielke R Cotton W Walko R Tremback C Nicholls M Moran M Wesley D Lee Copeland J 1992 A comprehensive meteorological modeling system RAMS Meteor Atmos Phys 49 69 91 Small C Naumann T 2001 The global distribution of human population and recent volcan ism Environ Haz 3 93 109 Ulke A 2000 New turbulent parameterization for a dispersion model in atmospheric boundary layer Atmos Environ 34 1029 1042 49 Wilson L Huang 1979 The influence of shape on the atmospheric settling velocity of volcanic ash particles Earth Planet Sci Lett 44 311 324 Scire J Robe F Yamartino R 2000 A User s Guide for the CALMET Meteorological Model Tech Rep Version 5 Earth Tech Inc 196 Baker Avenue Concord MA01742 Suzuki T 1983 A theoretical model for dispersion of tephra In D Shimozuru I Yokoyama Eds Arc Volcanism Physics and Tectonics Terra Scientific Publishing Company TER RAPUB Tokyo
4. p 2 2 1 2 KUxZ 1 1 137 i h L lt 0 unstable Note that in the neutral case L oo both expressions coincide Finally in the free atmosphere above the ABL z h gt 1 K is considered a function of the local vertical wind gradient a characteristic length scale le and a stability function F depending on the Richardson number Ri OV Oz For le and F the model adopts the relationship used by the CAM3 model Collins et al 2004 of the National Center for Atmospheric Research NCAR b_ 13 bel 13 7 x 13 table Ri gt 0 i F Ri 24 151084158 1 18 unstable Ri lt 0 where A is the so called asymptotic length scale Ae zz 30m while the Richardson number is g 00 0z 6 0V Oz On the other hand for the horizontal eddy diffusivity K Ky FALL3D assumes a large eddy parameterisation Azad and Kitada 1998 Ov es dv 2 2 EU p 15 Oy at H 2 Ox S Oy ou where a is a dimensionless constant of the order of unity that ranges from 0 1 to 5 depending on the size of the domain and Ax and Ay are the horizontal grid spacings commonly a 0 5 K F Ri 12 14 calculated as Ri with 0 being virtual potential temperature Ky aAxAy 20 The model permits also to use other K parametisations such as a constant value for a constant value for Ky or to estimate Ky using a Smagorinsky model as that
5. e POSTPROCESS TIME INTERVAL HOURS Time interval in h of postprocess plots starting from the database initial time BEGIN METEO DATA HOURS AFTER 00 e Z CUTS Terrain following heights in m at which maps are produced Table 1 Example of a meteorological database input file In this example a database of 60x60x8 km is created It contains 61x61x22 81862 points with hourly meteorological data from 19 Gen 2006 at OOUTC to 21 Gen at 00UTC TIME UTC YEAR 2006 MONTH 1 DAY 19 BEGIN_METEO_DATA_ HOURS_AFTER_00 0 END_METEO_DATA_ HOURS_AFTER_00 48 TIME_STEP_METEO_DATA_ MIN 60 DATABASE_GRID UTM_ZONE 33 UTM_HEMISPHERE N X ORIGIN UTM M 485000 Y ORIGIN UTM M 4131000 CELL SIZE KM 1 0 NX 61 NY 61 Z LAYER_ M 0 10 50 250 500 1000 2000 4000 6000 CALMET MESOSCALE MODEL AMITA MESOSCALE TIME INCREMENT HOURS 3 MESOSCALE_RANGE_OF_LATITUDES 35 0 40 0 MESOSCALE_RANGE_OF_LONGITUDES 12 0 15 0 POSTPROCESS_DBS OUTPUT FILES IN GRD FORMAT YES OUTPUT FILES IN PS FORMAT YES POSTPROCESS TIME INTERVAL HOURS 6 Z CUTS_ M 3000 7000 14 2 4 database script files In order to automate the creation update of databases the APOLLO procedure contains a series of script files that control the flow of a database construction These files are obviously oper ating system dependent and are located in the folder Scripts Dbs The default folder structure a
6. itime INPUT int Time in s after O0UTC var INPUT real nx ny nz Variable to output istat OUTPUT int Execution status 0 means no error message OUTPUT char Output message only if istat 4 0 e subroutine APOLLO_out_model_structuredgrid PURPOSE Outputs model geometry for postprocess Grid is assumed to be structured with uniform spacings along x and y directions Spacing along the vertical direction z can vary SINTAX call APOLLO_out_model_structuredgrid fname nx ny nz xo yo dx dy dz top istat message Variable yo dx dy dz top istat message INPUT INPUT INPUT INPUT INPUT INPUT INPUT INPUT INPUT INPUT OUTPUT OUTPUT length char int int int real real real real real nz real nx ny int char 38 Description Path including name of the file Number of points in the x direction Number of points in the y direction Number of points in the z direction z coordinate UTM in m of the origin bottom left corner y coordinate UTM in m of the origin bottom left corner Grid spacing in m along the x direction Grid spacing in m along the y direction Grid spacings in m along the z direction Topography Execution status 0 means no error Output message only if istat Z 0 39 6 File formats 6 1 The terrain file format DESCRIPTION ASCII file containing terrain information at discrete points of a regular 2D grid Points a ordered in lines of
7. 5000 FALL_TIME_THRESHOLD 200 0 EDDY_CONSTANT 0 03 POSTPROCESS_MODELS OUTPUT FILES IN GRD FORMAT YES OUTPUT FILES IN PS FORMAT NO MAP_TOTAL_LOAD YES UNITS KG M2 CONTOUR_LEVELS 0 1 0 25 0 5 1 5 10 50 MAP_CLASS_LOAD NO UNITS KG M2 CONTOUR LEVELS 0 1 0 25 0 5 1 5 10 50 MAP_DEPOSIT_THICKNESS NO UNITS MM COMPACTATION_FACTOR 0 7 CONTOUR LEVELS 0 11 5 10 50 MAP_TOTAL_CONCENTRATION YES UNITS KG M3 Z CUTS_ M 1000 2000 CONTOUR_LEVELS 1e 5 1e 4 MAP_Z_CUMMULATIVE_CONCENTRATION YES UNITS KG M2 CONTOUR LEVELS 0 01 0 1 1 10 MAP_Z_MAXIMUM_CONCENTRATION YES UNITS KG M3 CONTOUR_LEVELS 1e 4 1e 3 27 Only used if OUTPUT_FILES_IN_PS_FORMAT YES Only used if OUTPUT_FILES_IN_PS_FORMAT YES Only used if OUTPUT_FILES_IN_PS_FORMAT YES Only used if OUTPUT_FILES_IN_PS_FORMAT YES Only used if OUTPUT_FILES_IN_PS_FORMAT YES Only used if OUTPUT_FILES_IN_PS_FORMAT YES 28 3 6 The run script files In order to automate the execution of models the APOLLO procedure contains a series of script files that control the run flow These files are obviously operating system dependent The default folder structure and file names defined in section 7 are assumed e Scripts APOLLO Run ProblemName These scripts located in the folder Scripts Runs control the run of a problem named ProblemName There must exist a different script for each problem The scripts update firs
8. C Density pJ Source Term S SJ Table 2 Summary of the scaling factors for the terrain following domain coordinate system z X y Y 2 Z J indicates the Jacobian of the coordinate system transformation 21 3 4 3 TEPHRA model DESCRIPTION TEPHRA Connor et al 2001 is an Eulerian model based on an analytical solution of eq 1 The particle fall time depends on particle properties density diameter and atmospheric density Settling velocity is determined assuming spherical particles and considering different regimes depending on the Reynolds number and atmospheric density as Pas Re lt 6 laminar 18u Ag py V xm 6 Re lt 500 intermediate 17 3 1gd at Re gt 500 turbulent Pa where pa and pp stand respectivelly for the air and particle densities d is the particle diameter u is air viscosity and Re is the Reynolds number Note that in the turbulent regime this coincides with equation 2 spherical particles On the other hand diffusion of particles in the atmosphere is estimated using a bivariate Gaussian probability density function to approximate turbulence with the variance c given by AKt 0 012822 t gt to coarse particles 5 2 18 t 0 222 5 t lt to fine particles 19 where t is the total particle fall time is a threshold time 2 is the particle release height and c is a constant PROGRAM CALL normally included in a script
9. SIMILARITY See section 3 4 2 and Costa et al 2005 for details e VERTICAL DIFFUSION COEFFICIENT M2 S Value of the diffusion coefficient in m s Only used if VERTICAL TURBULENCE MODEL CONSTANT e HORIZONTAL TURBULENCE MODEL Type of model for horizontal diffusion Possibilities are CONSTANT PIELKE or RAMS See section 3 4 2 and Costa et al 2005 for details 24 e HORIZONTAL_DIFFUSION_COEFFICIENT_ M2 S Value of the diffusion coefficient m s Only used if HORIZONTAL_TURBULENCE_MODEL CONSTANT e SAFETY_FACTOR Safety factor This is a factor that multiplies the critical time step It should be equal or lower than 1 0 typically 0 8 0 9 to ensure stability e USE LIMITER METHOD Flag to indicate the use of limiter Possibilities are YES or NO If YES the algoritm uses a limiter method See Costa et al 2005 for details e POSTPROCESS TIME INTERVAL HOURS Time interval to output results in h Results are also output at the end of the run Block HAZMAP read by the HAZMAP model This block contains labels that define the HAZMAP input data e ZLAYER Heights in m of the z layers in terrain following coordinates i e above the vent It is not necessary to specify the number of vertical layers since it is automatically calculated by the program e NUMBER OF CLASSES Numbner of granulometric classes e TERMINAL VELOCITY MODEL Type of terminal settling velocity model Possibilities are ARASTOOPOU
10. ZLAYER M Heights in m of the database z layers If TypeData is PROFILE then BUILD DBS interpolates the measured values of velocity and temperature at these heights If TypeData is CALMET62 the heights represent the CALMET cell faces Block CALMET read by programs MESOINP CALMETINP and BUILDDBs This block contains labels that define some variables needed by CALMET e MESOSCALE MODEL Alias of the mesoscale model used Possibilities are AMITA LAMIB ARPASIM NOAA and ECMWF e MESOSCALE TIME INCREMENT HOURS Time increment in A of the mesoscale data This is usually 3 or 6 Normally each time interval corresponds to a GRIB file e MESOSCALE RANGE OF LATITUDES An interval of latitudes that contains the database This is just to speed up the algorithm that searches which points of the mesoscale model grid lay within the domain of the database e MESOSCALE_RANGE_OF_LONGITUDES An interval of longitudes that contains the database This is just to speed up the algorithm that searches which points of the mesoscale model grid lay within the domain of the database 13 Block POSTPROCESS_DBS read by program PosrPDBs This block contains labels that define the variables needed by the optional database postprocessor program e OUTPUT_FILES_IN_GRD_FORMAT Possibilities are YES or NO If YES plots maps in GRD file format e OUTPUT_FILES_IN_PS_FORMAT Possibilities are YES or NO If YES plots maps in PS file for mat
11. advection takes place all particles falling from the same initial height remain at all times at the same altitude While the centre of each cloud is translated by wind the cloud spreads horizontally due to diffusion and settles by gravity until it reaches the ground where it forms the deposit The model outputs therefore accumulations on the ground for each granulometric class For further details see Macedonio et al 2005 and Pfeiffer et al 2005 Settling velocity fits contemplated by HAZMAP include e ARASTOOPOUR Arastoopour et al 1982 4gdpy D chmod 2 di 2 24 een desi 4 Re 1 15Re0687 gt 3 0 44 Re gt 10 where pa and pp stand respectivelly for the air and particle densities d is the particle diameter Re is the Reynolds number and Cy is a drag coefficient Agdpp 4 d 4 e GANSER Ganser 1993 24 0 6567 0 4305 K gt 1 0 1118 1 2 04305 K 5 Ki 3 1 20 95 K 101 84148 Logy 0 5748 where w is the particle sphericity 1 for spherical particles Agdpp V 6 e WILSON Wilson and Wang 1979 24 me 2 1 07 Re lt 10 rper Ca re 1000 1 10 lt Re lt 10 7 1 Re gt 10 where is the aspect ratio b c 2a b c ellipsoidal semi axes e DELLINO Dellino et al 2005 1 2065 Vo 0 5206 2 0 Pp pa pa V 9 u 8 where is the
12. and decode the necessary GRIB format files produced by the mesoscale mete orological models and subsequently merge them into a single ASCII file written in a CALMET readable format The number of GRIB files required results from the ratio between the database time interval selected by the user in the database input file to the mesoscale model output time interval For instance to store data for the next 48 hours using meteorological data provided by a mesoscale model which supplies data every 6 hours it is necessary to decode up to 8 GRIB files PROGRAM CALL normally included in a script file Path of the executable 6 arguments MesoInp exe FileLog FileDbsInp FileMesoLst BaseGrib FileMesoGrid FileMesoRes FileLog Path including name of the log file It is an ASCII file that contains information about the program execution FiledbsInp Path including name of the database input file see section 2 3 FileMesoLst Path including name of the MesoLst file It is a MESOINP output ASCII file that contains run information BaseGrib Path including name but not file extension hh grb of the GRIB files to be decoded FileMesoGrid Path including name of the file that contains the grid of the mesoscale model see section FileMesoRes Path including name of the MesoRes file It is a MESOINP output ASCII file that is used by CALMET as input 10 2 2 3 The program CALMETINP DESCRIPTION The program CALMETINP alias
13. constant y from W to E In turn lines are ordered from N to S It normally covers a large area e g 1000x1000 km A database may always lay within the bounds of the terrain file It must be created by the user or downloaded from the APOLLO project website FORMAT Line 1 Free header Line 2 nx ny xo yo dx dy Line 3 Free header Lines 4 to 4 x x yz ldu zo alb bow shf ahf leaf where e nx Number of cells in the x direction e ny Number of cells in the y direction e xo x coordinate of the grid bottom left corner UTM coordinates in m e xf x coordinate of the grid top right corner UTM coordinates in e yo y coordinate of the grid bottom left corner UTM coordinates in m e yf y coordinate of the grid top right corner UTM coordinates in m e z topography In m e ldu Land use according to the USGS convention e alb Albedo at point z y e shf Soil heat flux at point x y e ahf Antropogenic heat flux at point x y e leaf Leaf index at point x y 6 2 The wind profile file format DESCRIPTION ASCII file containing the definition of the vertical wind profile and air tem perature at different time intervals This file can be read using LIBAPOLLO routines see section 5 5 FORMAT itimel itime2 nz z 1 ux 1 ux 1 T 1 zt ux nz ux nz T nz 40 where e itimei Starting time in sec after OOUTC of the meteo data time slice e itime2 End time in sec after OOUT
14. for Calmet Input file generator writes the CALMET control file This file contains all the information necessary to define a CALMET run PROGRAM CALL normally included in a script file Path of the executable 3 arguments CalmetInp exe FileLog FileDbsInp FileCalInp e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FiledbsInp Path including name of the database input file see section 2 3 e FileCalInp Path including name of the file It is a CALMETINP output ASCII file that is used by CALMET as input 2 2 4 The program CALMET DESCRIPTION CALMET program see Scire et al 2000 for details assimilates terrain information and an initial guess wind field on a coarse mesh to compute a zero divergence wind field and other diagnostic variables on a finer grid using a terrain following coordinate system For each time interval the initial guess wind field in our case the output of a meteorological prognostic model is first adjusted for i kinematic effects of terrain lifting and acceleration of the air flow over terrain obstacles ii thermodynamically generated slope flows and iii blocking effects in order to obtain after a divergence minimisation procedure a step 1 mass consistent wind field After that meteorological observations if available at the time under consideration can be added to the step 1 field and an objective analy
15. format ASCII file that contains data at regular spaced points Terrain data files should ideally cover several hundreds of kilometres around the volcano or volcanic area of interest and in principle can have an arbitrary spatial resolution The default spacing is 1km Note that in general the terrain file and the database can have different extensions and or spatial resolutions The only requirement is that the domain of the database typically of the order of 100x100 km must lay within the bounds of the terrain file typically of the order of 1000x1000 km PROGRAM CALL normally included in a script file Path of the executable 5 arguments GeoInp exe FileLog FileDbsInp FileCalGeo FileTerr FileDbsGrd FileLog Path including name of the log file It is an ASCII file that contains information about the program execution FiledbsInp Path including name of the database input file see section 2 3 FileCalGeo Path including name of the CalGeo file It is a GEOINP output ASCII file that is used by CALMET as an input FileTerr Path including name of the terrain file see section 6 1 FileDbsGrd Path including name of the DbsGrd file It is a GEOINP output file written in GRD format that contains the domain and topography of the database It serves just for optional visualization purposes 2 2 2 The program MESOINP DESCRIPTION The purpose of the MESOINP alias for MESOscale INPut generator pro gram is to read
16. gz from the APOLLO site 2 Decompress type gunzip apollo 1 0 tar gz and then untar type tar xvf apollo 1 0 tar to obtain the directory apollo 3 Go to the folder Scripts Master and run the script APOLLO Install specifying the compiler you want to use This script does successive calls to the Makefiles of the different programs and models On a Unix Linux Mac X OS the APOLLO Install script assumes that either INTEL ifort or GNU gfortran as well as GNU gcc are available to compile using other compilers you will need to change the affected Makefiles and launch them manually Type APOLLO Install fcompiler ifort for INTER ifort compiler APOLLO Install fcompiler gfortran for GNU gfortran compiler e On a Windows operating system 1 Download the compressed file named apollo 1 0 tar gz from the site 2 Decompress to obtain the directory apollo 3 Compile the different programs and models using your favourite FORTRAN and C compilers No automatic installation is provided under Windows OS 2 Generation of a meteorological database 2 1 Overview Fallout models need meteorological data as input simplest models may require only a verti cal wind field profile more elaborated models normally need 3D time dependent wind fields as well as other micrometeorological variables The APOLLO procedure builds a meteorological database for each region of interest A database contains the topography of the regi
17. origin of meteorological data Possibilities are PROFILE or CALMET62 e FileTop Name including path of the GRD topography file Only used if TypeData is PROFILE 2 2 6 The program PosTPDBs DESCRIPTION This program does an optional simple postprocess of a database It plots horizontal cuts of meteorological variables in this version only wind vector field and air tem perature PROGRAM CALL normally included in a script file Path of the executable 4 arguments Postpdbs exe FileLog FileDbsInp FileDbs BaseName e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileDbsInp Path including name of the database input file see section 2 3 e FileDbs Path including name of the Dbs file It is a binary file created by the BUILDDBS program Contains the meteorological database stored in a direct access binary file e BaseName Path for the PoSTPDBS program output files 2 3 The database input file A database input file see Table 1 is an ASCII file composed by a series of blocks and labels that define all the characteristics of a database Labels are case sensitive and can be placed in any order within a block Comments and extra lines can be inserted anywhere with no particular syntax This file controls the input parameters needed by the different programs described in the previous section There must exist a single input file for each meteorolo
18. sec after OOUTC of the time interval e itime2 End time in sec after OOUTC of the time interval e nsrc Number of source points can vary from one interval to another e nc Number of granulometric classes e MFR Mass flow rate in kg s e x x coordinate of the source isrc UTM coordinates e y y coordinate of the source isrc UTM coordinates m e z z coordinate of the source isrc terrain following coordinates in m i e above the vent e src Mass flow rate in kg s of each granulometric class for this point source It must be verified that src isrc ic MFR 6 5 The model output file format DESCRIPTION This is a binary file with the results from models It is assumed that results are output at the nodes of a regular 2d or 3d grid Models must output results in this format if they are be processed by the MODELPOSTP utility These can be done using LIBAPOLLO routines see section 5 6 FORMAT The file contains first a model grid block followed by number of results blocks one block for each output quantity and time instant in the case of transient models The model grid block contains three records with the following quantities record 1 nx ny nz xo yo dx dy record 2 zlayer nz record topg nx ny whereas each block of results contains 4 records with record 1 idime icode itime lenh1 lenh2 record 2 header1 record 3 header2 record 4 Results where e nx Number of cells in
19. speeds up the production of results and precludes from user manipulation errors 4 Data sharing All the models run using the same input data and can share also the same postprocess It ensures that outcomes maps from different models in the same run are directly comparable 5 Model data independency Models and data interface through a library the LIBAPOLLO It guarantees that future changes in the formats of files will not affect models and vice versa 6 Open source All the programs of the procedure are distributed freely for non commercial purposes A user can add also new models or functionalities and optionally make them accessible The APOLLO procedure flows by means of simple scripts which can be launched either manu ally or automatically with a user defined periodicity The script files located by default in the folder scripts see section 7 for details on the APOLLO tree structure define the name and location of the files and call the programs in the appropriate order Any program is called pass ing the path including name of the required input and output files as an argument Output files are created with the name and location specified by the argument 1 4 Download and installation Requirements A FORTRAN and a C compiler In addition MPI version 2 0 is also necessary to run the parallel version of the FALL3D model e On a Unix Linux Mac X operating system 1 Download the compressed file named apollo 1 0 tar
20. used by RAMS model for Az A 1 Pielke et al 1992 Kg Rmax Kma A 2 16 Kman 0 075K 4 A4 3 where A A A is a dimensionless constant ranging from 0 135 to 0 32 KA is a user defined parameter close to one and R 3 PROGRAM CALL serial version Path of the executable 7 arguments Fall3d_ser exe FileLog FileRunInp FileSrc FileGrn FileDbs FileLst FileRes PROGRAM CALL parallel version Path of the executable 4 8 arguments Fall3d par exe FileLog FileRunInp FileSrc FileGrn FileDbs FileLst FileRes Ncpu FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileRunInp Path including name of the run input file see Section 3 5 that contains the FALL3D block e FileSrc Name including path of the source file e FileGrn Name including path of the granulometry file e FileDbs Path including name of the Dbs file It is a binary file created by the BuUILDDBS program e FileLst Path including name of the Lst file It is an output ASCII file with information about the FALL3D run e FileRes Path including name of the Res file This is binary output file with the results of FALL3D For file format see section 6 5 e Ncpu Number of CPU groups Parameter Scaling Coordinates X x Y y Z z h z y Velocities U ux V u W u J Vsj Diffusion Coefficients Kx K Ky Kz BRI Concentration
21. ALMETINP output file 2 2 5 The program BUILDDBS DESCRIPTION This program generates the database files using as input either a veritcal profile sounding plus a topography file in format GRD or an output of the meteorological 11 processor CALMET version 6 2 The latter option is prefereable because CALMET generates a 3D wind field that accounts for topographic effects and determines values for micrometeorological variables in the Atmospheric Boundary Layer ABL PROGRAM CALL normally included in a script file Path of the executable 7 arguments BuildDbs exe FileLog FileDbsInp FileDat FileDbs FileDbsLst TypeData FileTop e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileDbsInp Path including name of the database input file see section 2 3 e FileDat Name including path of the meteo data file This is either the vertical profile file see section 6 2 or the binary output from CALMET version 6 2 depending on the value of TypeData e FileDbs Path including name of the Dbs file It is a binary file created by the BuILDDBS program Contains the meteorological database stored in a direct access binary file e FileDbsLst Path including name of the DbsLst file It is an ASCII file created by the BUILDDBS program Contains the explanation of each record of the database file in human readable form e TypeData Flag to indicate the
22. C of the meteo data time slice e nz Number of vertical layers e z Vertical coordinate of the layer in m terrain following e ux wind x velocity in m s e uy wind y velocity in m s e T Air temperature in C 6 3 The granulometry file format DESCRIPTION The granulometry file is an ASCII file containing particle densities and gran ulometric distribution This file can be created by the utility program SETGRN and read using LIBAPOLLO routines see section 5 4 FORMAT nc diam 1 rho 1 fc 1 diam nc rho nc fc nc where e nc Number of granulometric classes e diam Class diameter in mm e rho Class density in kg m e fc Class mass fraction 0 1 If must verify that fc 1 6 4 The source file format DESCRIPTION The source file is an ASCII file containing the definition of the source term The source is defined at time intervals during which source values are kept constant The num ber position and values e g Mass Flow Rate of the source points can however vary from one time slice to another There is no restriction on the number and duration of the time intervals It allows in practise to discretize any type of source term This file can be created by the utility program SETSRC and read using LIBAPOLLO routines see section 5 3 FORMAT itimel itime2 nsrc nc MFR xyzsrc 1 1 src 1 nc 1 src nsrc nc 41 where e itimei Starting time in
23. GRANULOMETRY DISTRIBUTION GAUSSIAN FIMIN 0 FI MAX 5 GAUSSIAN DISTRIBUTION MEAN 2 5 FI DISP 1 5 LINEAR DISTRIBUTION FI SLOPE 0 5 MINIMUM DENSITY MAXIMUM DENSITY 1080 3 2300 5 FALL3D ZLAYER M 0 500 1000 2000 3000 4000 5000 NUMBER OF CLASSES 6 TERMINAL VELOCITY MODEL GANSER TERMINAL VELOCITY MODEL FACTOR 0 8 VERTICAL TURBULENCE MODEL SIMILARITY VERTICAL_DIFFUSION_COEFFICIENT_ M2 S 100 HORIZONTAL TURBULENCE MODEL PIELKE HORIZONTAL_DIFFUSION_COEFFICIENT_ M2 S 1000 SAFETY_FACTOR 0 9 USE_LIMITER_METHOD yes POSTPROCESS_TIME_INTERVAL_ HOURS 2 One value for each source time interval Variables below used if SOURCE TYPE POINT Variables below used if SOURCE TYPE SUZUKI One value for each source time interval One value for each source time interval One value for each source time interval Variables below used if SOURCE TYPE PLUME Variables used if DISTRIBUTION GAUSSIAN Variables used if DISTRIBUTION LINEAR if VERTICAL TURBULENCE MODEL CONSTANT if HORIZONTAL TURBULENCE MODEL CONSTANT HAZMAP Z LAYER M 0 100 500 1000 2000 3000 4000 5000 NUMBER_OF_CLASSES 12 TERMINAL_VELOCITY_MODEL Ganser TERMINAL_VELOCITY_MODEL_FACTOR 1 0 HORIZONTAL_DIFFUSION_COEFFICIENT_ M2 S 1000 POSTPROCESS TIME INTERVAL HOURS 3 TEPHRA ZLAYER_ M 0 100 500 1000 2000 3000 4000 5000 NUMBER_OF_CLASSES 12 DIFFUSION_COEFFICIENT_ M2 S
24. IBUTION GAUSSIAN e FI SLOPE Slope of the linear distribution Only used if DISTRIBUTION LINEAR e MINIMUM DENSITY Minimium value of density in kg m and associated value of For values of lower than this value larger particles density is assumed to be constant and equal to the minimum value e MAXIMUM DENSITY Maximum value of density in kg m and associated value of For values of larger than this value smaller particles density is assumed to be constant and equal to the maximum value Block FALL3D read by the FALL3D model This block contains labels that define the FALL3D input data e ZLAYER Heights in m of the z layers in terrain following coordinates i e above the vent It is not necessary to specify the number of vertical layers since it is automatically calculated by the program e NUMBER OF CLASSES Numbner of granulometric classes e TERMINAL VELOCITY MODEL of terminal settling velocity model Possibilities are ARASTOOPOUR Arastoopour et al 1982 GANSER Ganser 1993 WILSON Wilson and Wang 1979 and DELLINO Dellino et al 2005 e TERMINAL VELOCITY MODEL FACTOR Model dependent factor For ARASTOOPOUR it is not used For GANSER it is the sphericity v see eq 5 For WILSON it is the aspect ratio see eq 7 Finally for DELLINO it is the shape factor V see eq 8 e VERTICAL TURBULENCE MODEL Type of model for vertical diffusion Possibilities are CONSTANT or
25. Once installed the apollo directory contains 6 folders Data Documents Master Models Pro grams and Runs The location and names of files created during the execution of programs and models is set in the scripts scripts call the programs and pass the full paths of files to be created as a program call argument It is recommended to keep the default APOLLO tree structure However if a user wishes to change file names and locations is it sufficient to modify the scripts accordingly C Apollo LJ Data 1 Documents Scripts Models 1 Programs J Runs 1 Folder Data Contains the terrain and meteorological data a Folder Terrain Contains the terrain files Area terrain dat see section 6 1 and the symbols files see section 6 7 b Folder Mesoscale Contains the mesoscale meteorological predictions Each mesoscale model has its own folder which in turn can have different Area folders The latter contain the mesoscale meteorological grid for the Mesomodel Area mesogrid dat c Folder Meteo Contains the results of the CALMET runs including CALMET input and output files It is not necessary to keep these files since the meteorological data are in practice stored in the database d Folder Dbs Contains the meteorological databases Each area has its own folder where the database input file Area dbs inp for this particular area resides By default periodic daily updates are not deleted Thus a folder Area YYMMDD is creat
26. R Arastoopour et al 1982 GANSER Ganser 1993 WILSON Wilson and Wang 1979 and DELLINO Dellino et al 2005 e TERMINAL VELOCITY MODEL FACTOR Model dependent factor For ARASTOOPOUR it is not used For GANSER it is the sphericity v see eq 5 For WILSON it is the aspect ratio see eq 7 Finally for DELLINO it is the shape factor V see eq 8 e HORIZONTAL_DIFFUSION_COEFFICIENT_ M2 S Value of the diffusion coefficient K in m s e POSTPROCESS TIME INTERVAL HOURS Time interval to output results in h Block TEPHRA read by the TEPHRA model This block contains labels that define the TEPHRA input data e ZLAYER_ M Heights in m of the z layers in terrain following coordinates i e above the vent It is not necessary to specify the number of vertical layers since it is automatically calculated by the program e NUMBER_OF_CLASSES Numbner of granulometric classes e DIFFUSION_COEFFICIENT_ M2 S Value of the diffusion coefficient K in m s e FALL TIME THRESHOLD Value of fall time threshold to see eq 18 e EDDY CONSTANT Value of constant c see eq 18 Block POSTPROCESS MODELS read by MopELPosrP This block contains labels used to define the postprocess of models and production of maps It is only read if the optional program MODELPOSTP runs e OUTPUT_FILES_IN_GRD_FORMAT Possibilities are YES or NO If YES MODELPOSTP plots files in GRD format Files in GRD format see section 6 6 for det
27. The GRD fil format c sos ode ROW ete e e Ren ommo beum qe hl d en d 6 7 The symbols file format aede ee TUS e a p EE a The default APOLLO tree References 1 Foreground 1 1 About this manual This manual has been prepared by Arnau Folch and Antonio Costa It gives general instructions to install and run the APOLLO procedure The software is freely distributed for non comertial purposes The authors decline any responsability for any error or incorrect use Please note that this version of APOLLO is a beta version still under test If you find any bug please report it to us 1 2 Introduction Explosive volcanic eruptions can eject into the atmosphere large amounts of blocks lapilli and ash during sustained periods of time These products globally known as tephra represent a serious threat for communities settled around active volcanoes It is estimated that half a billion people live nowadays close to active volcanoes Small and Naumann 2001 Several tens of cities and urban areas near volcanoes exceed one million inhabitants including just to mention some relevant examples Mexico City Tokyo Manila Quito Seattle or Naples Chester et al 2001 Approximately 500 airports lie within 100 km of volcanoes that have erupted during the last hundred years and tens of thousands of passengers fly over volcanically active regions such as the North Pacific which has more than 100 active volcanoes and fo
28. User s guide for the APOLLO procedure version 1 0 Arnau Folch afolch ov ingv it Antonio Costa costa ov ingv it Giovanni Macedonio macedon ov ingv it Istituto Nazionale di Geofisica e Vulcanologia Sezione Osservatorio Vesuviano Via Diocleziano 326 I 80124 Napoli Italy June 2007 Contents 1 Foreground Lia About thissimaniall a mirar ape aoe a deel eke ere Seen os meter er e Ru 152 INtioduction 520 ie S dte und d MOM EL ded Va dee dete hcg SE 1 3 Overview of the APOLLO procedure 1 4 Download and installation oo a a 2 Generation of a meteorological database Dil OVerview eea uu ers RUE SS Rb quse Na Madaha ded 2 2 Description of programs 4 ll lll es 2 21 phe program GEOINPD 5555 Bae ee BAe a XXI xe 2 2 2 bhe program MESOINP a poo 40 R dose n eee EORR Y IP 22243 The program CALMETINP i 22 3 ee aR Ra m BOR 2 2 4 The program GALMET 65222 i Uy uv Rh UR 2 2 5 The program BUILDDBS 2 2 6 The program POSTPDBS 2 3 The database input 2 4 The database script Run generation 3 1 Overview re baile eat SU eh ae ee ed 3 2 Generation of a granulometry file The program SETGRN 3 3 Generation of a source file The program SETSRO 2
29. X call APOLLO get_input_cha fname block line value istat message Variable length Description fname INPUT char any Path including name of the file block INPUT char any Block header line INPUT char any Line header nval INPUT int 4 Number of values to read value OUTPUT char nval Values of the nval strings to read istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 5 2 Routines to read a database A database is composed by properties and meteorological variables Properties which can be integer or real numbers define characteristics of the database like date location number of 32 points etc Meteorological variables are the contents of the database and are stored in a direct access file There exists a file record for each variable at a particular time instant and for each vertical layer The length of a record is therefore nz x ny 8 bytes e subroutine APOLLO get dbs property int4 PURPOSE Gets the value of an integer type property from a database SINTAX call APOLLO_get_dbs_property_int4 fname word value istat message Variable kind length Description fname INPUT char Path including name of the file word INPUT char any Code of the property to read Possibilities are DATE Date of the database YY YYMMDD BEGIN Initial time of data h after 00UTC END Final time of data h after 00UTC NX Number of poi
30. ails can be readed directly by several plotting programs like the commercial software GRAPHER Alternativelly the user may also generate its own plots using functons from several free packages e g gnuplot in FORTRAN 25 OUTPUT_FILES_IN_PS_FORMAT Possibilities are YES or NO If YES MODELPOSTP plots files in PS format MAP TOTAL LOAD Possibilities are YES or NO If YES MoDELPOSTP plots the total ground load UNITS Units of MAP TOTAL LOAD It must be KG M2 CONTOUR LEVELS Values of the contour levels for MAP TOTAL LOAD Only used when OUTPUT FILES IN PS FORMAT is YES MAP CLASS LOAD Possibilities are YES or NO If YES MODELPOSTP plots the class ground load UNITS Units of MAP CLASS LOAD It must be KG M2 CONTOUR LEVELS Values of the contour levels for MAP CLASS LOAD Only used when OUTPUT FILES IN PS FORMAT is YES MAP_DEPOSIT_THICKNESS Possibilities are YES NO If YES MODELPOsTP plots total deposit thickness UNITS Units of MAP_DEPOSIT_THICKNESS Possibilities are MM for mm CM for cm and M for m COMPACTATION FACTOR Deposit compactation factor CONTOUR LEVELS Values of the contour levels for MAP DEPOSIT THICKNESS Only used when OUTPUT FILES IN PS FORMAT is YES MAP TOTAL CONCENTRATION Possibilities are YES or NO If YES MODELPOSTP plots the total concentration at certain z levels UNITS Units of MAP TOTAL CONCENTRATION It must be KG M3 72 CUTS M z coordinates of th
31. air viscosity and V is the shape factor sphericity to circularity ratio 18 PROGRAM CALL normally included in a script file Path of the executable 7 arguments Hazmap exe FileLog FileRunInp FileSrc FileGrn FileDbs FileLst FileRes e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileRunInp Path including name of the run input file see Section 3 5 that contains the HAZMAP block e FileSrc Name including path of the source file e FileGrn Name including path of the granulometry file e FileDbs Path including name of the Dbs file It is a binary file created by the BUILDDBS program e FileLst Path including name of the Lst file It is an output ASCII file with information about the HAZMAP run e FileRes Path including name of the Res file This is binary output file with the results of For file format see section 6 5 3 4 2 FALL3D model DESCRIPTION FALL3D is a 3D time dependent Eulerian model which circumvents most of the simplifications behind the simpler fallout models The model solves the advection diffusion sedimentation equation using a finite differences explicit scheme using a regular mesh Costa et al 2005 It uses the gradient transport theory to evaluate the atmospheric turbulent diffusion within and above the ABL and experimental fits for the particle settling velocities in addition to the values o
32. ata is valid Execution status 0 means no error Output message only if istat Z 0 5 6 Routines to output model results e subroutine APOLLO_out_model_result2d PURPOSE Writes model results deposit load or thickness at surface SINTAX call APOLLO_out_model_result2d fname header0 header1 icode nx ny itime var istat message 37 Variable length Description fname INPUT Path including name of the file headerO INPUT Free header headerl INPUT Free header icode INPUT i Variable code Possibilities are 0 for TOTAL DEPOSIT LOAD 1 for DEPOSIT THICKNESS i for CLASS i DEPOSIT LOAD nx INPUT int Number of points in the x direction ny INPUT int Number of points in the y direction itime INPUT int Time in s after OOUTC var INPUT real nx ny Variable to output istat OUTPUT Execution status 0 means no error message OUTPUT char Output message only if istat 4 0 e subroutine APOLLO_out_model_result3d PURPOSE Writes 3D model results concentration on air SINTAX call APOLLO_out_model_result3d fname header0 headerl icode nx ny nz itime var istat message Variable length Description fname INPUT char Path including name of the file headerO INPUT char Free header headerl INPUT char Free header icode INPUT int Variable code Possibilities are 1 for AIR CONCENTRATION nx INPUT int Number of points in the x direction ny INPUT int Number of points in the y direction nz INPUT int Number of points in the z direction
33. domain e z Value of z at each grid point 6 7 The symbols file format DESCRIPTION ASCII file that contains the symbols and legends added to the PS format postprocess files This file is used optionally by the program MODELPOsTP and specifies the coordinates of relevant geographyic features e g cities airports etc If these fall within the bounds of the computational domain the program MODELPOSTP adds the legend and the asso ciated symbol to the PS files FORMAT x y legend code flag x y legend code flag where e x x coordinate e y y coordinate e legend Word that defines the geographyic feature e g Catania e code An integer number that defines the code of the symbol associated to the feature see Figure below e flag Integer flag to switch on off this particular feature If flag is 1 MODELPOSTP adds the feature to the PS file EXAMPLE To add a squared symbol with the legend Catania add the following line to the file 507000 4152000 Catania 157 1 Characters and octal codes for Font ZapfDingbats x 102 x 122 123 124 x 141 142 143 144 162 411 241 242 243 244 O 9 262 2 606 gt 321 322 323 324 gt gt eb gt gt 341 342 343 344 346 347 350 353 354 gt gt gt gt gt gt gt 5 gt 360 361 362 363 364 365 366 367 370 371 372 373 374 375 45 7 The default APOLLO tree
34. duration of each time interval is constant and given by RUN START HOURS AFTER 00 minus ERUPTION END HOURS AFTER 00 divided by the number of time intervals automat ically computed by the program from the number of values e SOURCE TYPE Type of source distribution Possibilities are POINT SUZUKI or PLUME e HEIGHT ABOVE VENT M Heights of the plume in m above the vent One value for each time interval e A Parameter A in the Suzuki distribution One value for each time interval Used only if SOURCE_TYPE SUZUKI e L Parameter L in the Suzuki distribution One value for each time interval Used only if SOURCE_TYPE SUZUKI 23 e EXIT_VELOCIY_ MS Magma exit velocity in m s at the vent One value for each time interval Used only if SOURCE TYPE PLUME e EXIT TEMPERATURE K Magma exit temperature in K at the vent One value for each time interval Used only if SOURCE TYPE PLUME e EXIT VOLATILE FRACTION INA Magma volatile mass fraction at the vent One value for each time interval Used only if SOURCE TYPE PLUME Block GRANULOMETRY read by SETGRN This block contains labels that define the granulometric characteristics e DISTRIBUTION Type of distribution It can be LINEAR or GAUSSIAN e FI MIN Minimum value of e FI MAX Maximum value of e FI MEAN Mean value of Only used if DISTRIBUTION GAUSSIAN e FI DISP Value of o in the Gaussian distribution Only used if DISTR
35. e layers at which concentration is output CONTOUR LEVELS Values of the contour levels for MAP TOTAL CONCENTRATION Only used when OUTPUT FILES IN PS FORMAT is YES MAP Z CUMMULATIVE CONCENTRATION Possibilities are YES or NO If YES MODELPOSTP plots the z cummulative concentration vertical integration UNITS Units of MAP Z CUMMULATIVE CONCENTRATION It must be KG M2 CONTOUR LEVELS Values of the contour levels for MAP Z CUMMULATIVE CONCENTRATION Only used when OUTPUT_FILES_IN_PS_FORMAT is YES MAP Z MAXIMUM CONCENTRATION Possibilities are YES or NO If YES MODELPOSTP plots the maximum value of concentration along the vertical for each point This variable can be useful for flight safety concentration tresholds UNITS Units of MAP Z MAXIMUM CONCENTRATION It must be KG M3 CONTOUR LEVELS Values of the contour levels for MAP Z MAXIMUM CONCENTRATION Only used when OUTPUT FILES IN PS FORMAT is YES 26 Table 3 Example of a run input file TIME_UTC YEAR 2006 MONTH 12 DAY 5 ERUPTION START HOURS AFTER OO 10 ERUPTION END HOURS AFTER 00 20 RUN_END_ HOURS_AFTER_00 24 SOURCE X_VENT_ UTM_M 500080 Y_VENT_ UTM_M 4177690 MASS_FLOW_RATE_ KGS 5d4 4d4 SOURCE_TYPE SUZUKI POINT_SOURCE HEIGHT_ABOVE_VENT_ M SUZUKI_SOURCE HEIGHT_ABOVE_VENT_ M sodi 74 5 PLUME_SOURCE EXIT_VELOCIY_ MS 100 EXIT_TEMPERATURE_ K 1073 EXIT VOLATILE FRACTION_ IN O 2000 3000 2800
36. ed every day YYMMDD stands for YearMonthDay e g 070120 for January 20th 2007 to store the database files C Data CJ Terrain CJ Mesoscale Meteo C Area terrain dat ls Area symbols dat 1 Mesomodel LJ Area F C Area Mesomodel 4MITA C3 Area Sicily CJ Area Sicily Area dbs in 2 Area L Area YYMMDD C3 Area Sicily Area YYMMDD meso Ist Area YYMMDD Mesomodel Area mesogrid dat Ates Donec Area Y YMMDD dbs Area Y YMMDD calmet geo Area YYMMDD dbs lst C Year Area YYMMDD calmet inp Area YYMMDD calmet res C3 Year 2007 Area YYMMDD calmet lst Mesomodel Area YYMMDD HH grb 46 2 Folder Documents Contains APOLLO documentation including this manual 3 Folder Scripts Contains the scripts These files are obviously OS dependent 4 Folder Models Contains the source codes and the executables of the fallout models and the program MoDELPOSTP Models added by users should lay in this folder Models DI Fall3d par C Fall3d ser C Hazmap CI Tephra C ModelPostp Fall3d par exe Fall3d ser exe Hazmap exe Tephra exe ModelPostp exe 1 Sources C Sources Sources C Sources 1 Sources 5 Folder Programs Contains the source codes and the executables of the APOLLO pro grams and the library LIBAPOLLO Programs C Calmet C Dbs C SetGm DI SetSre 22 LibApollo F SetGrn exe SetSrc exe F LibApollo a Geolnp CJ Builddbs Sou
37. f the dataset full 3D prognostic wind field source term and topography The model can be therefore used to forecast either ash concentration in the atmosphere or ash loading on the ground APOLLO contains both serial and parallel versions of FALL3D The structure of the code combined with the fact that the interaction among particles is a second order effect facilitates the parallelization enormously T wo kinds of parallelization are considered one for particle classes and one for space vertical layers Firstly the processors available are distributed among groups or teams Each team works only on a certain particle class or on a set of particle classes the number of processors must be in consequence a multiple or a divisor of the number of classes If each particle class has more than one processor assigned i e if the number of processors is a multiple of the number of classes a second parallelization on the domain is possible In this case the tasks within a team are subdivided in vertical layers Note that it implies a data exchange among processors of the same team but the teams remain isolated among them The non conservative form of continuity equation written in a generalised coordinate system X Y Z is oC 496 _ OC px OC px OC px ax nf aX av 7 MY ow eor og ea where is the scaled average concentration U V W are the scaled wind speeds Kx Ky and are the diagonal scaled diff
38. file Path of the executable 7 arguments Tephra exe FileLog FileRunInp FileSrc FileGrn FileDbs FileLst FileRes e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileRunInp Path including name of the run input file see Section 3 5 that contains the TEPHRA block e FileSrc Name including path of the source file e FileGrn Name including path of the granulometry file e FileDbs Path including name of the Dbs file It is a binary file created by the BUILDDBS program e FileLst Path including name of the Lst file It is an output ASCII file with information about the TEPHRA run e FileRes Path including name of the Res file This is binary output file with the results of TEPHRA For file format see section 6 5 22 3 5 run input file A run input file see Table 3 is an ASCII file composed by a series of blocks and labels Labels are case sensitive and can be placed in any order within a block Comments and extra lines can be inserted anywhere This file controls the input parameters needed by the programs SETGRN SETSRC MODELPOSTP as well as by the different models HAZMAP FALL3D and TEPHRA Each model has its own block labelled like the model where the model inputs are specified A new block named MODELNAME should be added to this file whenever a new model is added to the APOLLO runs There must exist an input file fo
39. gical database to 12 build update Block TIME read by the programs GEOINP MESOINP CALMETINP and BUILDDBS This block contains labels that define the time range of the meteorological database in UTC time e YEAR Simulation year e MONTH Simulation month 1 12 e DAY Simulation day 1 31 e BEGIN METEO DATA HOURS AFTER 00 Time in h after 0000UTC for the current day at which meteorological data start e END_METEO_DATA_ HOURS_AFTER_00 Time in h after 0000UTC for the current day at which meteorological data ends The meteo time interval should include the simulation time interval defined by the records RUN START HOURS AFTER 00 and RUN END HOURS AFTER 00 of the run input file see section 3 5 e TIME STEP METEO DATA MIN Time step in min of the meteo data Block DATABASE GRID read by programs GEOINP CALMETINP and BUILDDBs This block contains labels that define the size and location of the database e UTM ZONE UTM zone code 1 60 e UTM HEMISPHERE UTM hemisphere Possibilities are N or S e X ORIGIN UTM x origin of the database bottom left corner UTM coordinates in m e Y ORIGIN UTM M y origin of the database bottom left corner UTM coordinates in m e CELL SIZE KM Horizontal database cell size in km e g 0 5 1 2 etc e NX Number of grid cells in the x direction W E direction e NY Number of grid cells in the y direction S N direction e
40. he database For example if a model assumes that the wind field is horizontally uniform it is sufficient to use a selected value from each vertical layer of the database for instance the average or a manually specified profile The gathering of data from a database is consequently a model dependent step and must be implemented ad hoc for each particular model After a run the last step of the procedure is to postprocess the outcomes of models in order to draw maps with pre defined physical quantities All models can share the same postprocess treatment so that if two or more different models output the same quantity e g ground deposit thickness their respective maps are directly comparable The user introduces inputs by means of short ASCII control files There are two kinds of input files meteorological database input files and run input files The formers control the parameters that define a meteorological database each database must have its own input file The latter control the parameters that define a run each run must have its own input file Input control files can be modified at any time for example to incorporate data acquired during an on going eruption e g measurements of granulometry or column height estimations of the mass flow rate etc If the control input files remain unmodified models run periodically with the same eruptive parameters but using updated meteorological predictions The latter scenario could be character
41. hen this option switched on the program reads the values of the wind field from a meteorological file computes the averaged wind direction and solves the plume governing equations for each time interval and particle class accounting for wind Note that it introduces a time dependence in the source term even when all the eruptive parameters mass flow rate class fraction etc are kept constant in time PROGRAM CALL normally included in a script file Path of the executable 7 arguments SetSrc exe FileLog FileRunInp FileSrc FileGrn FileDbs ModelName UseMesh e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileRunInp Path including name of the run input file see Section 3 5 that contains the SOURCE block e FileSrc Name including path of the source file This is the output from SETSRC that is used later by models e FileGrn Name including path of the granulometry file e FileDbs Path including name of the Dbs file It is a binary file created by the BuUILDDBS program Only used if the SOURCE_TYPE record in the run input file is PLUME e ModelName Name of the model must coincide with the corresponding model block in the run input file This is used to read the number of granulometric classes used by each model e UseMesh Flag to indicate if the results are projected onto the model mesh Possibilities are YES or NO 3 4 Fallout mode
42. il which the value of the source term remains unchanged istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 e subroutine APOLLO get source value PURPOSE Gets the values of the source points nsrc x nclass values SINTAX call APOLLO get source value fname timesec src endsec istat message Variable length Description fname INPUT char Path including name of the file timesec INPUT int Time s after 00UTC at which data is ex tracted src OUTPUT real nsrc nclass Source values endsec OUTPUT int Time in s after OOUTC until which the value of the source term remains unchanged istat OUTPUT Execution status 0 means no error message OUTPUT char Output message only if istat Z 0 5 4 Routines to read a granulometry file A granulometry file contains information about fraction and density of the granulometric classes It is assumed constant during the whole run See section 6 3 for details on file format e subroutine APOLLO_get_granulometry_nclass PURPOSE Gets the number of granulometric classes SINTAX call APOLLO get granulometry nclass fname istat message Variable fname nc istat message INPUT OUTPUT OUTPUT OUTPUT kind char int int char 36 length Description any 4 4 100 Path including name of the file Number of granulometric classes Execution status 0 means no error Output message only if istat 4 0
43. int fname timesec word x z value endsec istat message 33 Variable kind length Description fname INPUT char Path including name of the file timesec INPUT int 4 Time s after 00UTC at which data is ex tracted word INPUT char any Code of the property to read Possibilities are TOPOGRAPHY VELOCITY X VELOCITY Y VELOCITY Z TEMPERATURE CONVECTIVE VELOCITY SCALE MIXING HEIGHT MONIN OBUKHOV LENGTH INPUT Point x coordinate UTM in m INPUT Point y coordinate UTM in m INPUT Point z coordinate in m terrain following NOTE z 0 for TOPOGRAPHY CONVECTIVE VELOCITY SCALE MIXING HEIGHT and MONIN OBUKHOV LENGTH value OUTPUT real Value of the property defined in word endsec OUTPUT int Time in s after 00UTC until which the value of the variable remains unchanged istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 e subroutine APOLLO get dbs value plane PURPOSE Gets the values of a variable on a plane vertical layer at a given time instant The plane is assumed to have nz x ny points at the same horizontal location that those of the database If the plane z coordinate does not coincide with a layer of the database results are interpolated linearly The plane can be above the upper limit of the database A terrain following coordinate system is assumed SINTAX call APOLLO get dbs value plane fname timesec word z value end
44. istic of a pre eruptive crisis period during which the eruptive parameters e g mass flow rate granulometry etc must necessarily be guessed based on the experience from previ ous events Some advantages of the APOLLO procedure are 1 Modularity Each program of the procedure performs a specific task and runs indepen dently from the rest It gives large flexibility and facilitates future modifications or addition of new functionalities 2 Flexibility There is an absolute flexibility concerning the quantity of meteorological data bases and number of runs For instance different databases for different regions can coexist and be updated with different periodicity e g every 6 hours daily etc It allows for instance to automate forecasts for several volcanoes or volcanic areas simultaneously On the other hand there is no limit on the number of runs for a specific location several runs can use the same meteorological database Thus for example one could consider different runs starting at the same time instant e g to model an event supposed to start after 24 hours but considering different scenarios characterized by different mass flow rates or column heights different runs starting at different time instants e g to model a single scenario supposed to start after 24 48 or 72 hours or both 3 Automatization The scripts that control the flow of the procedure can be launched pe riodically without user intervention It
45. l run that is to calculate these quantities after the model run 4 2 The program MODELPOSTP DESCRIPTION The program MODELPostTP alias for Model Postprocess is an optional utility that reads a model output binary file see section 6 5 calculates some relevant quan tities at selected z planes and time instants and produces elementary maps in GRD see sec tion 6 6 and PS formats The parameters needed by MODELPOSTP are defined in the block POSTPROCESS MODELS located at the end of the run input file PROGRAM CALL normally included in a script file Path of the executable 4 5 argu ments ModelPostp exe FileLog FileRunInp FileRes BASERES FileSym e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileRunInp Path including name of the run input file see Section 3 5 that contains the POSTPROCESS MODELS block e FileRes Path including name of the Res file This is binary output file with the results of models For file format see section 6 5 e BASERES Path where the MODELPOSTP output files are dump e FileSym Path including name of the symbols file This file is optional MODELPosTP can be called using either 4 or 5 arguments and is used to add symbols and legends to the PS files For file format see section 6 7 30 5 The library LIBAPOLLO LIBAPOLLO is a library written in FORTRAN 77 It contains a set of user callable routines
46. line value istat message fname INPUT char Path including name of the file block INPUT char Block header line INPUT char Line header nval INPUT int Number of values to read value OUTPUT int nval Values of the nval integers to read istat OUTPUT Execution status 0 means no error message OUTPUT char Output message only if istat 4 0 e subroutine APOLLO_get_input_rea4 PURPOSE Gets nval reals of length 4 from a line SINTAX call APOLLO get input rea4 fname block line value nval istat message Variable length Description fname INPUT char Path including name of the file block INPUT char Block header line INPUT char Line header nval INPUT int Number of values to read value OUTPUT Values of the nval reals to read istat OUTPUT Execution status 0 means no error message OUTPUT char Output message only if istat 4 0 e subroutine APOLLO_get_input_rea8 PURPOSE Gets nval reals of length 8 from a line SINTAX call APOLLO get input rea8 fname block line value nval istat message fname INPUT char Path including name of the file block INPUT char Block header line INPUT char Line header nval INPUT int Number of values to read value OUTPUT Values of the nval reals to read istat OUTPUT Execution status 0 means no error message OUTPUT char Output message only if istat 4 0 e subroutine APOLLO_get_input_cha PURPOSE Gets nval characters from a line SINTA
47. lity 2 Creation of a source file using the program SETSRC Alternatively the same file can be supplied by the user without running the SETSRC utility 3 Model run 4 Optionally model postprocess using the program MODELPOSTP 3 2 Generation of a granulometry file The program SETGRN DESCRIPTION The granulometric distribution for a model is stored in a granulometry file see section 6 3 for details The program SETGRN is an utility that reads the GRANULOMETRY block of a run input file see section 3 5 and generates a granulometry file assuming that the mass fraction of particles follows a Gaussian distribution in and that the density of particles varies linearly with Note that in general each model present in a run has to have its own granulometry file because the number of discrete granulometric classes may vary from model to model Note that other distributions different from Gaussian and having arbitrary density size relationships can be also considered In this case however the granulometry files can not be generated by SETGRN but must be supplied directly by the user PROGRAM CALL normally included in a script file Path of the executable 4 arguments SetGranum exe FileLog FileRunInp FileGrn ModelName e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileRunInp Path including name of the run input file see Section 3 5 that con
48. ls 3 4 1 HAZMAP model DESCRIPTION HAZMAP is FORTRAN90 code for the solution of the equation of diffusion transport and sedimentation of small particles in order to model the dispersion of ash generated by a convective column Under the approximations of a constant horizontally uniform wind field and negligible vertical advection and diffusion this equation reduces to 2 2 Tx rud ew ri PED 092252 1 ot dx Oy Oz Ox Oy where C is the concentration of the particle velocity class j having a settling velocity V u uz Uy is the wind velocity is the constant horizontal turbulent diffusion coefficient and S is the source term Since the above expression is linear in mass an instantaneous release of the total mass from the eruption column can be assumed if wind and diffusion parameters do not 17 change significantly with time and only the final deposit is needed This quasi steady approach is assumed to hold during each simulation time interval Considering these approximations the above equation has a semi analytical solution as described in Macedonio et al 2005 The computational domain is split into thin horizontal layers that fall to the ground together with the particles originally contained in a given initial vertical interval 2 z 1 at time t 0 An analytical solution is then found for each layer Since the whole treatment is done separately for each class of particles and no vertical diffusion and wind
49. nd file names defined in section 7 are assumed e Script APOLLO Build Dbs DbsName Controls the creation of a database named Db sName There must exist a different script file for each database to create update This script updates first the date in the database input file through a call to a secondary script named APOLLO Dbs touchdate and then controls the construction of the meteorological database this task is done by the script APOLLO Dbs engine e Script APOLLO Dbs touchdate Changes the date in the date in the database input file e Script APOLLO Dbs engine Does the calls to the programs GEOINP MESOINP CAL METINP CALMET BUILDDBS and PosTPDBs The user can control which programs have to run 15 3 Run generation 3 1 Overview A run is the simulation of a given scenario APOLLO allows to include several fallout models within the same run Since models may run using different number of granulometric classes that is with a same granulometric distribution but with different discretization and or using different spatial discretizations it is necessary to supply different source and granulometry files to each model A run is defined in the run input file see section 3 5 and executed trough a script file see section 3 6 For each model present in a run the flow includes 1 Creation of the granulometry file using the program SETGRN Alternatively the same file can be supplied by the user without running the SETGRN uti
50. nts in the x direction NY Number of points in the y direction NZ Number of vertical layers value OUTPUT int 4 Value of the property defined in word istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 subroutine APOLLO get dbs property rea8 PURPOSE Gets the value of an real type property from a database SINTAX call APOLLO_get_dbs_property_rea8 fname word value istat message Variable kind length Description fname INPUT char any Path including name of the file word INPUT char any Code of the property to read Possibilities are X ORIGIN x origin coordinate UTM in Y ORIGIN y origin coordinate UTM in m X SPACE x grid spacing in km Y SPACE y grid spacing in km Z LAYERS z layers coordinates in m value OUTPUT real 8 Value of the property defined in word Returns an scalar except if word Z LAYERS In this case returns nz values istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 subroutine APOLLO get dbs value point PURPOSE Gets the value of a variable on a point and at a given time instant The point coordinates must lay within the bounds of the database If the point does not coincide with a node of the database grid results are interpolated bilinearly A terrain following coordinate system is assumed SINTAX call APOLLO get dbs value po
51. on and relevant prognostic meteorological variables wind field air temperature velocity scales Monin Obukhov length and mixing height Discrete prognostic values for these variables at different time instants are stored at the nodes of a 3D grid This grid is regular equally spaced along the horizontal but can have an arbitrary vertical layering It allows to define meteorological data grids finer within the Atmospheric Boundary Layer ABL where gradients of meteorological variables are larger and coarser at higher atmospheric levels Models are not constrained to run on the same grid where meteorological data are stored Models and database inerface through the library LIBAPOLLO which contains routines that extract values from a database either at a single point or at a horizontal layer There are two ways to construct a database The simplest one requires a vertical profile of tem perature and wind speed normally obtained from a vertical sounding The second option more elaborated is based on the program CALMET Scire et al 2000 an open source meteorological processor developed and maintained by scientists of the US Atmospheric Studies Group ASG which includes a diagnostic wind field generator APOLLO takes advantage of this functional ity to obtain time dependent wind and temperature fields as well as other micrometeorological variables Assimilating terrain information and an initial guess wind field on a coarse mesh CALMET ver
52. pp Chester D L Degg M Duncan A M Guest J E 2001 The increasing exposure of cities to the effects of volcanic eruptions a global survey Environ Haz 2 89 103 Collins W Rasch P Boville B Hack J McCaa J Williamson D Kiehl J Briegleb B 2004 Description of the NCAR Community Atmosphere Model CAM 3 0 Technical Report NCAR TN 464 STR National Center for Atmospheric Research Boulder Colorado Costa A Macedonio G Folch A 2006 A three dimensional Eulerian model for transport and deposition of volcanic ashes Earth Planet Sci Lett 241 34 634 647 Connor C B B E Hill B Winfrey N M Franklin and P C LaFemina 2001 Estimation of volcanic hazards from tephra fallout Natural Hazards Review 2 33 42 Dellino P D Mele R Bonasia G Braia L La Volpe R Sulpizio 2005 The analysis of the influence of pumice shape on its terminal velocity Geophys Res Lett 32 L21306 Dutton J Fichtl G 1969 Approximate equations of motion for gases and liquids J Atmos Sci 26 241 254 Ganser G 1993 A rational approachto drag prediction spherical and nonspherical particles Powder Technology 77 143 152 Jacobson M 1999 Fundamentals of atmospheric modelling 1st Edition Cambridge University Press New York Macedonio G Costa A Longo A 2005 A computer model for volcanic ash fallout and assessment of subsequent hazard Computer and Geosciences 31 837 845
53. r each run Block TIME_UTC read by SETSRC and models This block contains labels that define the time range of a run in UTC time The run time interval must lay within the time interval bounds of the meteorological database to which a run is linked e YEAR Simulation year e MONTH Simulation month 1 12 e DAY Simulation day 1 31 e RUN START HOURS AFTER 00 Run start hour after 0000U TC of current day e ERUPTION END HOURS AFTER 00 Eruption end hour after 0000U TC of current day If the SETSRC program is used to generate the source term this is the time instant at which source is switched off e RUN END HOURS AFTER 00 Run end hour after 0000UTC Note that in general a run can continue even when the source term is switched off i e when the eruption has ceased in order to give time for the remaining airborne particles to fall T his can be important in time dependent models such as FALL3D In contrast for steady or quasi steady models HAZMAP or TEPHRA this is unrelevant and RUN END HOURS AFTER 00 can coincide with ERUPTION END HOURS AFTER 00 Block SOURCE read by SETSRC This block contains labels that define the source char acteristics e X VENT UTM M x coordinate of the vent UTM coordinates in m e Y VENT UTM M y coordinate of the vent UTM coordinates in m e MASS FLOW RATE KGS Values of the mass flow rate in kg s One value for each time in terval The
54. rces 1 Sources Sources Geolnp exe r BuildDbs exe Lj Sources PostpDbs r Mesolnp exe PostpDbs exe L 1 Sources C Sources CalmetInp Sources Calmet Calmet62 exe LJ Sources 6 Folder Runs Contains the runs Each run has a folder with the run input file and the results for the different models By default periodic daily runs are not deleted Thus a folder RunName YYMMDD is created every day YYMMDD stands for YearMonthDay e g 070120 for January 20th 2007 to store the run results CJ RunName CJ RunName Etna01 RunName YYMMDD Etna01 060101 RunName YYMMDD log C3 Model C3 Model Fall3d RunNameYYMMDD model inp RunNameYYMMDD model src RunNameYYMMDD model res RunNameYYMMDD model lst LJ Postprocess 47 48 8 References Arastoopour H Wang Weil S 1982 Particle particle interaction force in a dilute gassolid system Chemical Engineering Science 37 1379 1386 Azad A Kitada T 1998 Characteristic of the air pollution in the city of Dhaka Bangladesh in winter Atmos Environ 32 1991 2005 Bursik M 2001 Effect of wind on the rise height of volcanic plumes Geophys Res Lett 18 3621 3624 Casadevall T J 1993 Volcanic Ash and Airports Discussion and Recommendations from the Workshop on Impacts of Volcanic Ash on Airport Facilities U S Geological Survey Open File Report 93 518 52
55. red grid FORMAT GRD files contain five header lines that provide information about the size and limits of the grid followed by a list of z values scalar variable The fields within ASCII grid files must be space delimited The listing of z values follows the header information in the file The z values are stored in row major order starting with the minimum y coordinate The first z value in the grid file corresponds to the lower left corner of the map This can also be thought of the southwest corner of the map or more specifically the grid node of minimum x and minimum y The second z value is the next adjacent grid node in the same row the same y coordinate but the next higher x coordinate When the maximum z value is reached in the row the list of z values continues with the next higher row until all the rows of z values have been included The general format of an ASCII grid file is DSAA nx ny xo xf yo yf zmin zmax z M Ly z 1 nx aya Z ny nx 43 where e nx Number of cells in the x direction e ny Number of cells in the y direction e xo x coordinate of the grid bottom left corner UTM coordinates in m e xf x coordinate of the grid top right corner UTM coordinates in m e yo y coordinate of the grid bottom left corner UTM coordinates in m e yf y coordinate of the grid top right corner UTM coordinates in m e zmin Minimum value of z in the domain e zmax Maximum value of z in the
56. ry named LIBAPOLLO that acts as an interface between programs models and input data files Data from files and databases generated by different programs included in the APOLLO procedure can be read directly through simple LibApollo routine calls using either FORTRAN or C C without having a detailed knowledge of the file database format The APOLLO procedure generates all the data needed by models including a terrain and a meteorological database the definition of the source term and the granulometric distribution A meteorological database for a particular area contains short term predictions typically up to few days for meteorological variables e g wind field temperature turbulence related variables etc defined at the nodes of a 3D structured grid The meteorological database s is are ab solutely independent from models and can be updated automatically typically every day as new meteorological prognostics are available A run can start automatically after the construction of a meteorological database or at any user defined time a run is mainly an scenario it may content several simulations from different fallout models Whenever a fallout model runs it simply reads the required meteorological and if necessary terrain data from the database as well as the files that define the source and the granulometric data Clearly the kind of data to read varies from model to model a model is not constrained to use the entire contents of t
57. se limitations in order to advance towards a simultaneously efficient and accurate performance of models The goal of the APOLLO procedure is to facilitate the execution of fallout models by means of an automatic acquisition and manipulation of input data a subsequent automation of runs and a final shared postprocess analysis The idea is to increase performance eliminate involuntary human manipulation errors speed up computing times and anticipate the scientific response during emergencies Moreover another no trivial advantage is that models share inputs and postprocess treatment through the production of maps written in portable formats which allow for immediate comparison among outcomes from different models 1 3 Overview of the APOLLO procedure APOLLO acronym for Automatic Procedure to mOdeL voLcanic ash dispersiOn is a platform independent procedure designed to facilitate the execution and subsequent interpretation of volcanic ash transport and fallout models The APOLLO procedure is built on a series of open source programs that perform different tasks generate input data needed by models and do simple postprocessing Three open source fallout models HAZMAP FALL3D both serial and parallel versions and TEPHRA are included in this version of APOLLO However the user is not constrained to these models but can alternatively add other model s with mi nor modifications on the source codes To this purpose APOLLO contains a libra
58. se programs have to run each time meteorological data is updated 3 Run the BUILDDBS program to construct the meteorological database either from a CAL MET output or from a vertical profile in the latter case steps 1 and 2 are unnecessary 4 Optionally run also the program POSTPDBS that allows a simple visualization of meteo rological data Steps 2 to 4 can be performed automatically by means of the script APOLLO Build Dbs DbsName see section 2 4 Database input file FileDbsInp Grid of the Mesoscale mesoscale model model prognostics Terrain FileTerr FileMesoGrid BaseGrib FileMesoRes FileCalInp FileCalGeo Calmet v6 2 BuildDbs FilesGRD FileDbs FilesPS PostpDbs FileDbsLst Figure 1 Summary of the database construction update flow 2 2 Description of programs 2 2 1 The program GEOINP DESCRIPTION CALMET requires an input file with 2D geophysical data at ground level Data in this file include terrain elevation land use type surface parameters surface roughness albedo Bowen ratio soil heat flux and leaf area index and anthropogenic heat flux The program GEOINP alias for GEOphysical INPut generator extracts data from a terrain file interpolates the geophysical parameters needed by CALMET from the terrain file to the ground nodes of the database of the CALMET grid and finally writes these data in a CALMET readable format A terrain file see section 6 1 is a free
59. sec istat message 34 Variable length Description fname INPUT char Path including name of the file timesec INPUT int Time s after 00UTC at which data is ex tracted word INPUT char Code of the property to read Possibilities are TOPOGRAPHY VELOCITY X VELOCITY Y VELOCITY Z TEMPERATURE CONVECTIVE VELOCITY SCALE MIXING HEIGHT MONIN OBUKHOV LENGTH INPUT real Plane z coordinate in m terrain following NOTE z 0 for TOPOGRAPHY CONVECTIVE VELOCITY SCALE MIXING HEIGHT and MONIN OBUKHOV LENGTH value OUTPUT real nx ny Values at the nz x ny nodes of the plane endsec OUTPUT int Time s after 00UTC until which the value of the variable remains unchanged istat OUTPUT Execution status 0 means no error message OUTPUT char Output message only if istat Z 0 5 3 Routines to read a source file A source file contains information about the distribution of the mass flow rate source term for each granulometric class The number and position of sources may vary with time See section 6 4 for details on file format e subroutine APOLLO get source nsrc PURPOSE Gets the number of sources SINTAX call APOLLO get_source_nsrc fname timesec nsrc endsec istat message Variable kind length Description fname INPUT char Path including name of the file timesec INPUT int 4 Time in s after OOUTC at which data is ex tracted nsrc OUTPUT int Number of sources endsec OUTPUT int Time in s after 00UTC un
60. sion 6 2 computes a zero divergence wind field and other diagnostic variables on a finer grid using a terrain following coordinate system CALMET gives the option to use a gridded wind as furnished by a prognostic meteorological model as the initial guess wind field Note that prognostic meteorological models run on significantly larger horizontal grid spacing 100km for synoptic models and 10km for mesoscale models and different vertical layering than those of CALMET Consequently CALMET interpolates the guess field from the grid of the prognostic model to its own grid Fig 1 illustrates the flow to create update a meteorological database W hen using the CALMET option the steps include 1 Download the files that contain the mesoscale meteorological prognostics This step is not done by the APOLLO procedure The user is responsible for periodic daily download and storage of data normally a set of files written in GRIB or NetCDF formats that contain mesoscale prognostics every 3 or 6 hours The choice of a specific mesoscale model may depend upon several factors but the spatial coverage of the models and the facilities to get access to data are obviously two determinant factors 2 Run the CALMET processor In order to facilitate the execution of CALMET APOLLO contains a set of programs GEOINP MESOINP and CALMETINP see section 2 2 for description that act as interfaces gathering data and creating the CALMET input files All the
61. sis procedure gives a second intermediate field The scheme is designed so that observations are used to correct the step 1 wind field within a user specified radius of influence whereas it remains unchanged at regions where observations are unavailable Finally a new divergence minimisation procedure is applied iteratively to the step 2 field until the divergence of velocity reaches a lower bound The final outcome of CALMET consists of values at the grid points for a zero divergence wind field consistent with the observations or pseudo observations and for other micrometeorological variables like the Monin Obukhov length the friction velocity or the atmospheric boundary layer height The latter ones are quantities that may be later required by some fallout models to estimate the eddy diffusivity tensor It is important to note that the approximation of a zero divergence wind field assumed by CALMET is fully adequate at heights lower or close to one kilometer Dutton and Fichtl 1969 although it is commonly extended up to few kilometres In consequence the CALMET output field can be used confidently just for low to medium eruptive columns PROGRAM CALL normally included in a script file Path of the executable 2 arguments Calmet62 exe FileLog FileCalInp e FileLog Path including name of the log file It is an ASCII file that contains information about the program execution e FileCalInp Path including name of the CalInp file C
62. t the date in the run input file through a call to a secondary script named APOLLO Run touchdate and then control the run of each model this task is done by other scripts one for model named APOLLO ModelName engine The user can control which models have to run e Script APOLLO Run touchdate This script located in the folder Scripts Runs changes the date in the run input file e Scripts APOLLO ModelName engine These scripts located in the folder Scripts Models run a certain model e g APOLLO Hazmap engine runs calling first the pro gram SETGRN to generate the model granulometry then the program SETSRC to generate the source term then the model and finally the program MODELPOSTP to postprocess results 29 4 Postprocess of models 4 1 Overview Fallout models output either 2D results at ground surface normally deposit load and or deposit thickness or 3D results concentration on air In many cases it is interesting to evaluate also other derived variables that may have interest from the point of view of hazard assessment or crisis management For example the air borne ash burden serves to compare simulations with satellital images or the maximum value of concentration along the vertical can give insights on flight safety if the volcanic cloud moves towards the vicinity of an airport or intersects an aerial corridor From a practical point of view it is better to split the postprocess computations from the mode
63. t two lines can be identical if they belong to different blocks Comments can be placed anywhere The routines that read an input file search first for a specific block header and then for a specific line header within the block The rest of the file contents is simply ignored e subroutine APOLLO_get_input_npar PURPOSE Gets the number of parameters numbers included in a line SINTAX call APOLLO get_input_npar fname block line istat message Variable kind length Description fname INPUT char Path including name of the file block INPUT char any Block header line INPUT char any Line header npar OUTPUT int 4 Number of parameters found in the line istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 e subroutine APOLLO get input nword PURPOSE Gets the number of words included in a line SINTAX call APOLLO get input nword fname block line nword istat message Variable kind length Description fname INPUT char any Path including name of the file block INPUT char Block header line INPUT char any Line header nword OUTPUT int 4 Number of words found in the line header not included istat OUTPUT 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 4 0 31 e subroutine APOLLO_get_input_int4 PURPOSE Reads nval integers of length 4 from a line SINTAX call APOLLO get_input_int4 fname block
64. tains the GRANULOMETRY block e FileGrn Name including path of the granulometry file This is the output from SETGRN that is used later by models e ModelName Name of the model must coincide with the corresponding model block in the run input file This is used to read the number of granulometric classes used by each model 3 3 Generation of a source file The program SETSRC DESCRIPTION The distribution of sources is defined in a source file see section 6 4 for details The program SETSRC is an utility that reads the SOURCE block from the control input file see section 3 5 and generates a source file The source term is constant for a given time 16 interval but there is no limit on the number and duration of the time intervals It allows in practise to discretize any kind of time dependency time dependent mass flow rate column height etc The program admits three possibilities point source mass is released in a single source point Suzuki distribution Suzuki 1983 Pfeiffer et al 2005 and buoyant plume model Bursik 2001 The last option is more elaborated and involves the solution of the 1D radial averaged plume governing equations that describe the convective region of an eruptive column These equations are intimately coupled with the wind field which for small to medium size plumes may induce a substantial plume bent over and subsequent variations of plume height and mass release location For this reason w
65. that act as an interface between programs and files used by the APOLLO procedure When invoked within a program these routines allow to read and extract information from different files The programs included in the APOLLO procedure make use of LIBAPOLLO routines for file read operations The use of this library is strongly recommended although not mandatory if the user wishes to add a new model to the procedure The reason is twofold First because it simplifies enormously the codes Second and more important because any future change in the format of a file will imply modifications only in the library but not in the programs models which will remain unchanged The LIBAPOLLO contains several families of routines devoted to different purposes NOTE The routines of the library can be called either form FORTRAN or C using the same sintaxis To call routines from C simply include the header CtoF h include CtoF h located in the folder Programs LibApollo CtoF 5 1 Routines to read an input control file An input control file either for a meteorological database or for a specific run is an ASCII file composed by blocks of lines labels Each block starts with a header that informs about the general contents of the lines below In turn each line of a block starts with a header word that can be followed by a number of words and or parameters a parameter is a number either integer or real Line headers within a block can not be repeated bu
66. the x direction e ny Number of cells in the y direction e xo x coordinate of the grid bottom left corner UTM coordinates in m e yo y coordinate of the grid bottom left corner UTM coordinates in m e dx Grid spacing in m along the z direction e dy Grid spacing in m along the y direction e zlayer Coordinates of the grid vertical layers terrain following in m 42 e topg Topography e idime Spatial dimensions of results It can be 2 or 3 for results on a plane or in the space respectively e icode Code for results Possibilities if idime 2 are icode lt 0 Deposit load for granulometric class ABS icode icode 0 Total deposit load icode 1 Deposit thickness whereas possibilities if idime 3 are icode lt 0 Concentration for granulometric class ABS icode icode 1 Total concentration on air e itime Time of results Given in seconds after OOUTC for the current day e lenhi Length of the headerl e lenh2 Length of the header2 e headeri Free header for comments In the models HAZMAP FALL3D and TEPHRA contains the description of the results e header2 Free header for comments In the models HAZMAP FALL3D and TEPHRA contains the date and time in format Y Y Y Y MM DD HH SSSS e results These are nz x ny real 8 values if idime 2 and nz x ny x nz real 8 values if idime 3 6 6 The GRD file format DESCRIPTION ASCII grid files GRD contain results in a 2D structu
67. til which the value of the source term remains unchanged istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat Z 0 e subroutine APOLLO get source nclass PURPOSE Gets the number of classes SINTAX call APOLLO get source nclass fname timesec nclass endsec istat message 35 Variable kind length Description fname INPUT char Path including name of the file timesec INPUT int 4 Time s after 00UTC at which data is ex tracted nclass OUTPUT Number of classes endsec OUTPUT int Time in s after 00UTC until which the value of the source term remains unchanged istat OUTPUT int 4 Execution status 0 means no error message OUTPUT char 100 Output message only if istat 0 e subroutine APOLLO get source coordinates PURPOSE Gets the coordinates of the sources nsrc values on a terrain following coor dinate system SINTAX call APOLLO get source coordinates fname timesec y z endsec istat mes sage Variable length Description fname INPUT char any Path including name of the file timesec INPUT int 4 Time in s after OOUTC at which data is ex tracted OUTPUT real nsrc 8 x coordinates of the source points It returns nsrc values OUTPUT real nsrc 8 y coordinates of the source points It returns nsrc values OUTPUT real nsrc 8 z coordinates of the source points It returns nsrc values endsec OUTPUT int Time in s after 00UTC unt
68. ur to five ash producing eruptions per year Casadevall 1993 These data stress the potential socio economic impacts of volcanoes in general of ash fallout in particular and highlight the relevance of an adequate hazard assessment and risk mitigation policies On the other hand reliable short term forecasts represent a valuable aid for scientists and civil authorities to mitigate the effects of fallout on the surrounding areas during an episode of crisis In such a context it is essential to have accurate models for volcanic fallout An increasing number of models to predict ash transport and or the characteristics of the resulting fallout deposits have been developed during the last decades Simplest models are obviously less accurate but have lower computational requirements and hence are especially suitable to tackle inverse problems and or to produce immediate gross predictions In contrast complex models are more accurate but in general require more inputs not always available set up times pre and postprocess data treatment i e possible involuntary manipulation errors computational requirements and user expertise All these factors may preclude the efficiency of such models during an episode of pre eruptive crisis or even worst during the course of an eruption because may delay the production and delivery of short term forecasts to the decision making authorities An important challenge for the modelling community is to overcome the
69. usion coefficients the scaled atmospheric density and 5 is 19 the source term in the generalized coordinate system Considering as a frame of reference a simple terrain following coordinate system where the horizontal coordinates remain unchanged with respect to the Cartesian z X y Y z Z the scaling factors are those reported in Table 2 Equation 9 is solved for each particle velocity class independently i e assuming no interaction between particles belonging to different classes during the transport process For a detailed description see Costa et al 2005 In order to solve equation 9 it is necessary to evaluate the vertical and horizontal diffusion co efficients Inside the atmospheric surface layer the Monin Obukhov similarity theory estimates the vertical turbulent diffusivity K in terms of the friction velocity u and the Monin Obukhov length L KZ Gh where is the von Karman constant 0 4 z is the distance from the ground is the atmospheric stability function e g Jacobson 1999 Above the surface layer the original form of the Monin Obukhov similarity theory is no longer valid In order to extend this theory to the entire boundary layer z h lt 1 an evaluation of the Atmospheric Boundary Layer ABL height h is required For this purpose FALL3D uses a simple parameterisation valid on the entire ABL Ulke 2000 10 1 KA Z 1 1 4202 h L 20 stable h Lh 11

User's guide for the APOLLO procedure (version 1.0)

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