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1. TWIN stellar evolution code and various other system tools You probably do not need to know how these work just how the considerably simpler WTTS works WTTS is a Perl script and so should run on any platform which can run Perl which includes Linux Mac OS X Windows HP UX the only modern operating system I Gnuplot Ghostscript Imagemagick Un Zip etc Operating System Figure 1 Structure of the WTTS and TWIN setup WTTS sits between you and TWIN but also isolates you from the details of all the other tools it uses have used which has no Perl is my iPod Detailed and up to date instructions for instal lation can be found at the WTTS website http www astro uni bonn de izzard window html and below The stellar evolution code used by WT TS is Peter Eggleton s TWIN This is a separate executable and must be downloaded or built from source For each piece of software you are required to install you probably have to download it first so rather than point you to a specific web page which is liable to change I would recommend using your favourite search engine Google Yahoo etc Section 2 details how to include WTTS and TWIN The user manual is in section 3 This explains about the various windows and settings which are in WTTS If you use WTTS for work you intend to publish please cite us we have a paper coming out soon in New Astronomy 2 Installation I assume you are using a command line interface Te2. later date 3 1 4 The Options Most of the screen is taken up by the series of sub tabs denoting evolution options They are grouped logically e g initial conditions are all together Each option comes with a short help description Sometimes you can enter a number in a box sometimes you have a limited choice Remember the choice is limited for a reason Detailed descriptions of what the options do and how they affect your stellar evolution runs can be found in Peter s writeup file which is distributed with the TWIN code On the other hand the help given here might be enough for you 3 2 Evolve Tab This is where the bulk of the stellar evolution is done There are buttons to start and stop the evolutionary sequence The TWIN log file is also shown and updated automatically during the evolutionary run 3 2 1 Evolve Click on this to start the stellar evolution 3 2 2 Terminate Click on this to end the stellar evolution if it does not end itself 3 2 3 Clear Log Window This clears the log window of its contents 3 2 4 Update Log Window This updates the log window with the current output from TWIN 3 2 5 Follow Log This can be toggled when it is on the log is continuously updated and the cursor is sent to the bottom so you can always see the latest activity This is annoying if you want to read something that happened some time ago so you can also turn it off 3 2 6 Display You can follow the log of st
3. purposes Apart form the first line this file consists of blocks of stellar structure First Line 1 number of grid points number of lines of one block ofstellar structure 2 number of variables number of columns may be different fom the number of variables listed below 3 Convective overshoot parameter Blocks of stellar structure Each block starts with a header containing 1 Model number 2 Model Age yr The the columns with the actual stellar structure follow one line for each mesh point The first line is the interior of the star The first 21 variabble are described in the IO manual Check it for units and please add them to this wiki The columns 22 and further are missing in this manual 1 Mass coordinate in solar units 2 Radius Coordinate in solar units 3 Pressure dyn cm 4 Density g cm 5 Temperature K 6 Opacity cm g 7 Adiabatic Temperature Gradient 8 Radiative Adiabatic Temperature Gradient Wrong in IO manual 9 XH 10 XHe 14 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 ol 32 33 34 35 XC XN XO XNe XMg Total Luminosity in solar units Energy generation by contraction erg g s Energy generation by nuclear reactions erg g s Energy generation in neutrinos erg g s Entropy erg g K Internal Energy erg g Reaction rate RPP pp chain effective 2p gt 1 2 He4 Reaction
4. sets some default values In most cases nofork and startfile should be left undefined Usually this function will call fork to allow it to both run the evolution code and return control to the user If nofork is set to 1 then fork is not called and the function will not return until the evolution code has finished running The function checks the main program to see if it should start from an input model which is not part of the ZAMS library If so or if startfile is set to 1 then the evolution code is started from a user specified input model It is up to this function to update the status bar and log file window as the programmer of the API function sees fit See the TWIN API version for such details Returns TRUE in the parent fork the child does not return it exits with code 0 and returns 0 in the case where nofork is set 4 3 20 save _evcode_ options Usage save_evcode_options Saves the currently evolution code options to files usually in preparation for an evo lutionary run 4 3 21 set _evcode_ options _list Usage set_evcode_ options _list Set main options list with the layout for the options tab List items should be in this format BLOCK VAR in FILE where BLOCK is the common block in capitals VAR is the variable in capitals FILE is the filename it is stored in Structure i e sub tabs is introduced with Label label text or Section section label Note variables with no options are treated as non e
5. they are necessarily quite big 4 WTTS API As of version 0 13 WTTS has used a crude application programming interface API in the STARS perl module in an attempt to abstract the details of the stellar evolution code from WTTS so that at some point in the future WTTS can be used with any stellar evolution code This is still experimental but currently the API works with TWIN and the BINSTAR codes 4 1 API Implementation The API in the STARS pm module is the default TWIN function set In order to load a different set of functions then a different module should be loaded instead of STARS pm At present this must be done manually but there is no reason why it cannot be automated in the future However right now there is only the STARS pm module 4 2 TWIN specific stuff Because WTTS was designed to work with TWIN it uses the output files from TWIN to function properly I would suggest that the easiest way to adapt WTTS to a different stellar evolution code is to simply output the same information as TWIN does to similarly 13 named files from the different code These are the mdl1 mdl2 out1 out2 plt1 plt2 and mod files The following descriptions are taken from the STARS wiki at http www astro ru nl eglebbeek which will contain the most up to date documentation This is correct as of WTTS V0 14 and the current TWIN code 4 2 1 mdl files This file contains stellar stucture at different ages written for plotting
6. Window To The Stars A Guide November 17 2011 1 Introduction We present Window To The Stars WTTS a graphical user interface to the popular TWIN single binary stellar evolution code for novices students and professional astro physicists It removes the drudgery associated with the traditional approach to running the code while maintaining the power output quality and flexibility a modern stellar evolutionist requires It is currently being used for cutting edge research and interactive teaching This guide is for version 0 16 1 of WTTS 1 1 What is a stellar evolution code A stellar evolution code makes models of stars and evolves them in time 1 2 What is TWIN The stellar evolution code used by WTTS is a modified version of the TWIN stellar evolution code originally developed by Peter Eggleton It uses an adaptive non Lagrangian mesh which allows stars to be evolved with only 200 meshpoints in a few minutes on a normal desktop computer It is written in FORTRAN The code has three modes of operation one to calculate the evolution of single stars and two different ways for binaries TWIN and non TWIN In TWIN mode the two stars are solved for simultaneously by inverting a single matrix while in non TWIN mode the code evolves both stars individually and alternates between them at regular intervals 1 3 What is WTTS WTTS is a user interface that sits between you and the gory details of what is going on with the
7. ar 1 or star 2 use these buttons to select which one 3 3 HRD Tab The Hertzsprung Russell diagram HRD which shows log L Lo vs log Tag K is the primary diagnostic tool of stellar evolution It is displayed for each star individually or for both stars and updates as the evolution progresses The tracks can be labelled with a third variable such as central temperature or core mass and coloured according to the effective temperature 3 3 1 X Range and Y Range Here you can enter the ranges of the X L and Y Tgp axes from minimum to maximum Enter a to have WTTS automatically calculate a range for you 3 3 2 Stellar Colours Switch this on to label the colours in your HRD with the true stellar colours You can adjust the colour settings e g hue contrast in the Misc tab 3 3 3 Label with You can label the curve in the HRD with a third variable e g age or mass Use this to select which third variable 3 3 4 Label spacing The labels are automatically designed to not overlap but you can override the spacing with the menu given here 0 1 is the default and is usually good enough On the other hand if you zoom in you will need to make the number smaller 3 3 5 Line width The width of the line in the HRD 3 3 6 Star 1 Star 2 Stars 1 and 2 You can plot either star 1 or star 2 or both with this menu 3 4 Structure Tab In this tab structural variables such as age model number total mass core mass lumi nosity rad
8. cached variables and data and close file handles in the API module This should be called from clear_ global_ caches in WTTS 4 3 4 emergency _ exit Usage emergency _ exit In an emergency e g when you use too much memory try to shut down the evolution code This should try to stop the code in a nice way then kill it 4 3 5 evcode colour _log_ text Usage evcode_colour_log_text Gtk textbuffer buffer int n Given the text buffer which contains the log output colour it If n is given then only colour the last n lines If n is undefined then colour the whole text buffer this is very slow 17 4 3 6 evcode _ eval Usage evcode_eval string s Evaluates the string s in the context of the API module rather than in WTTS main program context 4 3 7 evcode_plugin menu Usage evcode_ plugin menu menubar menubar Given the widget menubar from WTTS adds evolution code specific plugins Returns the menubar widget modified Copy then STARS pm version and hack it 4 3 8 evcode_value_from_hash Usage evcode_value_from_hash string file string key Returns the element key of the hash called file so called because the hashes are named after the files they represent 4 3 9 evcode_variable_ settings Usage evcode_variable_settings This function is called to set default evolution code settings and set up arrays of variables used by the evolution code API Some of the variables it sets are in the main context some are n
9. d be as root Note these are quite basic procedures for anyone experienced with a UNIX operating system If in doubt get help or email us 2 3 5 Get Rob s Perl modules You need Rob s custom Perl modules as well These are similar to those from CPAN but Rob wrote them himself In a temporary directory e g src modules download the modules and build them If you are root wget http www astro uni bonn de izzard code wtts rob_misc_perl_module zip wget http www astro uni bonn de izzard code wtts STARS_perl_module zip mkdir rob cd rob unzip rob_misc_perl_module zip perl Makefile PL make as root make install cd mkdir STARS cd STARS unzip STARS_perl_module zip perl Makefile PL make as root make install Rob s Perl modules should now be installed You can install the modules without being root by putting a line in your shell options file e g bashrc export PERL5LIB HOME 1lib perl lib per15 site_perl 5 8 5 where the 5 8 5 is your version of Perl run perl v to find out Then before the perl Makefile PL steps above type PREFIX HOME 1ib perl and continue as before 2 3 6 Other required software For plotting WTTS uses Gnuplot but also uses ImageMagick for its convert utility and or Ghostscript and perhaps the sed utility preferably GNU sed These should be available in package form for your operating system or are available in source form for you to build On any decent distributio
10. de_ hashes Usage load_evcode_hashes Stellar evolution options are stored in hashes where the hash keys are the variable names and the hash values are the values of the variables This function loads these hashes from input files so is sometimes useful 4 3 16 load _evcode_options_from_zipfile Usage load_evcode_options_from_zipfile array zip_ output The array zip _ output is the output from the unzip command which simply unzips a given file as saved with save_evcode_options_to_ zipfile If file names in zip_ output are recognised to be important then they can be acted upon The usual way to do this is with a call such as load_evcode_options_from_zipfile split n o unzip d cachedir o file where file is the zipped filename 4 3 17 reset _evcode_ options Usage reset_evcode_ options Resets some evolutionary code options Gets called at the beginning and when the Reset Options button is pressed unlike evcode_ variable_ settings which is called only at the beginning 4 3 18 reset _evcode_ options _to_ defaults Usage reset_evcode_options_to_ defaults This function sets all options in the Options tab to their default values 4 3 19 run_evcode Usage run_evcode Boolean nofork Boolean startfile This function calls the evolution code How it does this will depend very strongly on the evolution code In TWIN context this function looks at the widgets in the main 19 program to determine parameters It then
11. ditable 4 3 22 save_evcode_options_to_zipfile Usage save_evcode_options_to_zipfile string filename Saves the currently evolution code options to a zip file the name of which is filename so you can load them at a later time 4 3 23 set_col_ labels Usage set_col_labels Sets the main plticols array These are the names of the variables in each column of the plti file Also sets up the main plticols hash 20 4 3 24 set _evcode_start_model Usage set_evcode_start_model int n filename f Sets the starting model for star n to the file f 4 3 25 set_evcode_var Usage set _evcode_var string data string blockname string varname string newval Sets the evolution code variable varname to newval by some circuitous route In the TWIN module the data variable stores the original data file and blockname is the name of the FORTRAN common block in which the data is stored The set_ evcode_ var function then searches the data for the blockname and varname and sets what it finds to newval This function is scheduled to be rewritten to remove the data and blockname as these are horribly programmed 4 3 26 stop_evcode Usage stop_ evcode Try to stop the evolutionary code in a nice way Should call a kill function main pidkill just in case it fails 4 3 27 variable help_ array Usage variable_help_array When called this function returns an array of strings of the format VARNAME Help text where VARNAME is the nam
12. ds 0 205 e ExtUtils PkgConfig 1 07 e File Tail 0 99 3 e Glib 1 102 e Gtk2 1 102 For Gtk2 perl and Glib perl you must have the Glib and Gtk2 libraries already installed on your system You can get these as packages e g RPM packages or by going to www gtk org 2 3 3 Packages If you want to try the package route which you probably should then you are on your own because it is different for each system If you are very lucky then you are using a system with a proper administrator and if you are really lucky indeed then he will read this and install everything for you With RPM packages e g on Redhat or Fedora Linux you should download the required packages log in as root with su and issue the command rpm install lt package name gt for each package 2 3 4 CPAN CPAN has a search facility search cpan org where you can simply search for the Perl modules listed above For example to get the Perl Gtk2 module type gtk2 into the search box This gives you the search results the first one is Gtk2 Click on the Gtk2 which brings you to a description of the module and a link to Download Click on that and save the file Gtk2 xxxx tar gz where xxxx is the module version which should not be too important to a temporary directory e g src then issue these commands tar xvzf Gtk2 xxxx tar gz cd Gtk2 the directory name may differ slightly perl Makefile PL make make install where the final command shoul
13. e of the variable and the Help text is whatever help text you would like to associate with the given variable 4 3 28 zams_ ms Usage zams_zs float z Returns a list of masses available in the ZAMS library for a given metallicity z which one of the list returned by zams_ zs 4 3 29 zams_zs Usage zams_zs Returns a list of metallicities available in the ZAMS library References 21
14. e traditional Kippenhahn plot shows convective regions as a function of mass coordi nate and time We expand on this idea by plotting a mapped 3D surface of any of the stellar evolutionary variables which includes convection as a function of any two others The map is in greyscale or colour with a selection of palettes In the case of mass coordinate used as an ordinate the core mass es convective boundaries and nuclear burning zones can be over plotted 3 6 1 Axis range resolution Each axis has its own range selector much like the other tabs and can be plotted as a linear log or 10 plot Choose a low resolution e g 10 to experiment with your plot as this will be faster 100 resolution should be used for publication quality plots 12 3 6 2 Palette Here you can choose from a series of colour palettes There is one greyscale palette suitable for black and white printing 3 6 3 Boundaries You can attempt to show the core mass surface boundaries convective boundaries and nuclear burning zones 3 6 4 Replot You must click on Replot to draw the graph Drawing is quite time consuming as the data must be extracted and then plotted and there is a lot of data involved 3 7 Miscellaneous Tab Other options can be changed here such as image size HRD colour contrast font type and size plot type postscript or PNG etc 3 8 Load Save Tab Here you can load or save a complete set of models The files are zipped because
15. in sequence ZAMS model or one of your own previously saved models If you are running WTTS for the first time then leave this setting at the default ZAMS library You can however chosen a metallicity Z and masses for the primary and secondary star If you are only planning on evolving a single star the secondary mass becomes irrelevant 3 1 2 Option Control If you press Reset from defaults then all the options will be reset to a default value which is usually suitable for basic single star evolution You can also Load and Save a whole set of options by clicking on Load and Save You can import a TWIN init dat file into your options by selecting Import gt init dat The plugins menu is for operations which are in some way special or automated At present version 0 13 there are two plugins e Import TWIN init dat This allows you to import an original TWIN init dat file into the current options set This can be useful for running say binaries using Peter s init dat files which come with the TWIN distribution e Remesher This plugin takes the selected starting model and changes the number of mesh points in it Note that the TWIN code has a maximum number of meshpoints usually 5000 which is set in the source file mesh f 3 1 3 Display Here you can choose either star 1 or star 2 This is the global control for the later plotting screens and enables you to display either star 1 or star 2 This will probably be removed at a
16. ius and abundances are plotted against one another The plot automatically updates throughout the evolution and many variables can be plotted at once with the option of logging the axes and choosing data ranges 3 4 1 Star menu Here you can choose whether to plot star 1 star 2 or both stars on your graph 10 3 4 2 x Variable Below this is the variable menu where you choose which variable to plot on the x axis 3 4 3 Y axis control With the three buttons Linear Y Axis Log Y Axis and 10 Y Axis you can plot either y logy y or 10 where y is the variable in question 3 4 4 X range and Y range Here you can choose the range of the x and y axes by selecting a minimum and maximum value As usual a means WTTS automatically scales the axis 3 4 5 y Variable This is the list of toggle buttons controlling the variables which should be plotted on the y axis 3 5 Internals Tab It is often desirable to examine the internal details of each stellar model individually or plot the results from a few models in one graph Plots are made of a selection of internal variables vs one other internal variable usually the mass coordinate for a selection of models It is possible to overlay the results of successive models or make an animated sequence There is also a sphere rendering mode which shows a spherical star with a slice removed so the internal details are visible There are twenty sub tabs in this tab so it is
17. log central The Structure tab showing surface and density central temperature and central den _ sity The Internals tab showing CNO abun The Kippenhahn diagram tab showing dances for one in every 500 models temperature as a function of mass coor dinate and age Figure 2 Example screenshots of the various tabbed windows showing the evolution of a 3Mo solar metallicity star a total of 2760 stellar models 3 1 Options Tab The first steps in creating a series of stellar evolution models are the choices of input parameters and physics We provide a selection of initial mass es from a library of zero age main sequence ZAMS stellar models with a range of metallicities typically 10 4 lt Z lt 0 03 It is also possible to load pre calculated models as the starting model see Internal below for details on saving models The physics and initial conditions for stellar evolution are then selected in a series of tabbed menus These provide the user with the original variable name an input box or menu and a description of what the parameter means with a suggested default parameter In this way every aspect of the stellar evolution run can be controlled We have added the ability to load or save a complete set of WITS options and also to import the original init dat files from the TWIN code distribution 3 1 1 Select Starting Model You must choose whether to start from a zero age ma
18. n the best way to use WTTS is to build the TWIN code and install the Perl modules yourself In this section we outline the general procedure which of course may need to be modified for your system 2 3 1 Build TWIN You should download the TWIN code distribution from our website currently http www astro uni bonn de izzard code wtts TWIN zip You must have a Fortran compiler We use ifort from Intel on Linux and g95 from GNU on Linux and MAC OS X So make a directory download TWIN zip to that directory and unzip the TWIN file e g mkdir wtts cd wtts wget http www astro uni bonn de izzard code wtts TWIN zip unzip TWIN zip Build it with make which assumes you have GNU make as your default make if this fails try gmake instead If you are not using ifort you should change the default Fortran compiler via the environment variable FORT E g to use g95 instead type export FORT g95 make Wait a little while until the build is finished 2 3 2 Get required standard Perl modules Here is where it gets tricky WTTS requires some quite standard Perl modules You can either get packages for these modules which are specific for your system e g RPMs for Redhat Fedora Linux e g www pbone net deb for Ubuntu Debian use apt or synaptic etc or perhaps Fink packages for OS X or install from downloaded source files from CPAN at www cpan org You need to install at least the following Perl modules e ExtUtils Depen
19. n solar units 9 log effective temperature K 10 log central temperature K 11 log maximum temperature K 12 log central density g cm 13 log density at maximum temperature g cm 14 Binding energy of envelope erg solar mass 15 Luminosity by Hydrogen burning in solar units 16 Luminosity by Helium burning in solar units 17 Luminosity by Carbon burning in solar units 18 Luminosity carried by neutrinos in solar units 16 19 Luminosity by release of excess thermal energy in solar units 20 Rotation period in days 21 k I M R basically the axis of gyration or moment of inertia T 22 Base of the convective envelope in units of the stellar radius 23 Thickness of the convective envelope in units of the stellar radius 4 3 Function List The following is a list of functions which are currently in the API V0 14 This is liable to change as the code is cleaned up added to and trimmed The names are also likely to change 4 3 1 analyse _evcode_ log for _termination_ reason Usage analyse_evcode_log_for_termination_reason Check the stellar evolution code s log file to determine why it failed and return a string containing an error message 4 3 2 check _for_evcode_ error Usage check_for_evcode_ error This checks for an error in the evolution code log file if one is detected sets the status bar and stops the evolution run 4 3 3 clear _evcode_ caches Usage clear_evcode_caches Clears up any
20. n these are installed by default What a definition of decent Use your favourite search engine to find these very useful tools You could try the following websites e www gnuplot info e www cs wisc edu ghost e www imagemagick org e www gnu org software sed 2 3 7 Running WTTS Now everything should be in place you can download and run Window To The Stars like this cd wtts wget http www astro uni bonn de izzard code wtts stars perlscript mv stars experimental perlscript wtts chmod 755 wtts wtts Of course you can change the name from wtts to whatever you like If there are any problems please feel free to email us see the website for our email address 3 Using Window To The Stars Window To The Stars is laid out in a logical progression of tabbed windows starting with the choice of physics through the stellar evolution to analysis of the results We shall describe each in turn and corresponding screenshots from the evolution of a 3Mo star can be found in Fig 2 In addition to the main tab window a status bar is visible at all times informing the user of the current status e g Evolving or Stopped and the physical state of the primary and secondary star All images can be saved as either PNG suitable for web based projects or Postscript for publications and talks Animations are saved as animated GIFs also compatible with web browsers The HRD tab labelled by
21. ot 4 3 10 extract __ model Usage extract_model string filename array pointer models Alternative model extraction routine This will be removed in future to make way for extract_ evcode_ model but it is currently used with TWIN to get models for a mod file which extract_ evcode_ model cannot do yet The mod file is given in filename and the pointer to an array models contains the numbers of the models for extraction An array containing the model data is returned 4 3 11 extract_evcode_model int nmod Usage extract_evcode_model int nmod Extracts model nmod and returns the data as a string In TWIN context this extracts model nmod from the mdl file by calling random_ extract_ model 4 3 12 get _available_ models Usage get available models Returns a list of model numbers which are available for us to play with In TWIN context this function calls get_ TWIN_ model_ list on the mdl files 18 4 3 13 has_evcode_ terminated Usage has_evcode_terminated Returns 0 if the evolution code is running 1 if it is not running and 2 if it is running and or has crashed In the TWIN version this first checks if the main running_ pid variable is set then checks if a kill 0 can be performed on the pid How the check is performed may depend on the specific evolution code 4 3 14 load _evcode_defaults Usage load_evcode_defaults Loads and sets the variable hashes with their default values Redundant 4 3 15 load_evco
22. possible to work on multiple images at the same time There is an option to always look at the latest model so internal details are followed during a model sequence run Each model can be saved and later used as a starting model for a new evolutionary run see the Options tab description 3 5 1 Y Axis You can choose to plot many different variables on the y axis just click on the buttons 3 5 2 Display As usual choose to plot either star 1 or star 2 3 5 3 Still Animate You can either plot a series of models as a still image in which case they will be overlaid or as an animation 11 3 5 4 Frame This gives the current frame number of the animation 3 5 5 Speed This changes the speed of the animation which is usually limited by your CPU This goes to 11 3 5 6 Ranges You can change the x and y axis ranges here 3 5 7 Col Gis Each of these buttons affects the model list see below C clears the list 1 selects every model 2 every 2nd model 5 every 5th etc pipe logical ORs the entire list so selected becomes deselected and vice versa 3 5 8 Model List Click on a model number to plot it You can select as many as you like If you select a model hold shift then select another the range will be selected If you select a model hold the control key then select another the range will be unselected 3 5 9 Image Tabs You can plot 20 different images each has its own tab 3 6 Kippenhahn Tab Th
23. rate RPC effective C12 2 p gt N14 Reaction rate RPNG effective N14 2p gt O16 Reaction rate RPN effective N14 2p gt C12 He4 Reaction rate RPO effective O16 2p gt N14 He4 Reaction rate RAN effective N14 3 2 He4 gt Ne20 Cpa Mean Molecular Weight in atomic mass units Mixing coefficient for thermohaline mixing or unused Mixing coefficient for convective mixing convective velocity mixing length Actual temperature gradientd log T dlog P homology invariant dlog p dlog P or unused homology invariant U_hom dlog R dlog P or unused homology invariant V_ hom dlog M dlog P or unused 15 4 2 2 mod files These are only used for saving models so you do not need to know the format You should however know the equivalent format for your stellar evolution code and have an appropriate extract_ model function 4 2 3 plt files This file contains global properties for the output of the evolution calculation Each calculated structure model occupies one line First Line The first line contains the number of columns in the output This may be less than what is listed here Subsequent lines 1 Model number 2 Age of the model yr 3 Mass in solar units 4 Helium Hydrogen exhausted core mass in solar units 5 Carbon Oxygen Helium exhausted core mass in solar units 6 Oxygen Neon Carbon exhausted core mass in solar units 7 log radius in solar units 8 log luminosity i
24. rminal on MAC OS X with a bash shell type bash to get into a bash shell and you are vaguely familiar with how to make your computer work via this interface I assume you have Perl installed which should be standard on a decent operating system otherwise you must get it Try www perl com and also zip and unzip 2 1 Automated Installer The automated installer should install most of WITS and TWIN but will not install standard packages such as Gnuplot Ghostscript etc on your machine You can get the installer from our website and try it with wget http www astro uni bonn de izzard code wtts installer perl installer Please contact us if this does not work It is difficult to write an installer for every operating system so it may well go wrong on your machine and it is only through your feedback that we can improve WTTS You should now be able to run WTTS with this command wtts 2 2 Pre built executables We have started to experiment with pre built executables which will in theory replace the need for the Perl script You can get a binary file from http www astro uni bonn de izzard window html but be warned that these will only work on some systems e g the systems we have access to You will need to download both WTTS and TWIN to the same directory then just run the WTTS executable You may need to make a subdirectory called code and move the TWIN executable into it 2 3 Build It Yourself In true Unix fashio
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