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1. Publishing publish public Digital publishing J SAY a Jo m Science 2011 8 26 Dust from Itokawa s Itokawa Dust Particles A Direct Link Between S Type Asteroids and Ordinary Chondrites Tomoki Nakamura Takaaki Noguchi Ma2. _ E E textual contents B MEE digital library
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6. 1 xe 66 6 RETLOMKTERORROHEICELT Ba f E 286 BUCHER An FE Vol 19 No 5 2012 Facemark Recommendation based on Emotion Communication and Motion Type Estimation D 40 1 4 1 8 in Microblogs Yuka EMURAttt and YoHEI SEkitit Many users use facemarks everyday in recent computer mediated communication en vironments such as e mail chatting and Microblogs Although facemarks are useful to express the emotion or communication intentions beyond natural language com munication many users feel difficult to choose the right one from lots of candidates according to the situation We propose a method to recommend facemarks based on the estimation of emotions communication or motion types in texts written by users Emotion communication or motion types are defined with Twitter corpus and esti mation system is implemented with k NN Five assessors evaluated the relevance of recommended facemarks for their intention and found that 66 6 of
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13. WW ccreal in 1 1 0 20 40 60 80 100 2001 2003 2005 2007 2011 SCREAL 2011 http www screal jp e A al tokawa Dust Particles A Direct Link Between S Type Asteroids and Ordinary Chondrites Tomoki Nakamura Takaaki Noguchi Masahiko Tanaka Michael E Zolensky Makoto Kimura Akira Tsuchiyama Aiko Nakato Toshihiro Ogami Hatsumi Ishida Masayuki Uesugi Toru Yada Kei Shirai Akio Fujimura Ryuji Okazaki Scott A Sandford Yukihiro Ishibashi Masanao Abe Tatsuaki Okada Munetaka Ueno s Toshifumi Mukai akoto Yoshikawa Junichiro Kawaguchi The Hayabusa spacecraft successfully recovered dust particles from the surface of near Earth asteroid 25143 Itokawa Synchrotron radiation x ray diffraction and transmission and scanning electron microscope analyses indicate that the mineralogy and mineral chemistry of the Itokawa dust particles are identical to
14. Department of Earth and Planetary Science Faculty of Science Kyushu University Hakozaki Fukuoka 812 8581 Japan NASA Ames Research Center Moffett Field CA 94035 USA To whom correspondence should be addressed E mail tomoki m toboku ac jp On the Teflon spatula we identified 1534 rocky particles by means of a field emission scanning electron microscope The particles have diameters ranging from 3 to 40 hm but are mostly smaller than 10 ym 7 Most Itokawa particles are angular and are probably broken pieces of larger rocks Among the 1534 harvested rocky particles 1087 are monomineralic includ ing 580 olivine particles 126 low Ca pyroxenes 56 high Ca pyroxenes 186 feldspars 172 plagi oclase and 14 K feldspar 113 troilites 13 chro mites 10 Ca phosphates and 3 Fe Ni metal grains The remaining 447 particles are poly mineralic mixtures mainly silicates Several other particles are silica minerals and K bearing halite all of uncertain origin Of the 40 particles removed by tapping diameters ranging from 30 to 180 um that were analyzed by x ray computed microtomog raphy 7 and x ray diffraction 38 were sub jected to more detailed mineralogic analysis Backscattered electron images of selected par ticles are shown in Fig 1 A to D RA OD02 0030 Fig 1A and RA QD02 0024 Fig 1B have a platy morphology are polymineralic and have many mineral grains 1 to 10 hm in diam eter adhering to t
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16. 1126 science Fig 1 A to D Backscattered electron BSE images of RA QD02 0030 A RA QD02 0024 B RA QD02 0013 C and RA QD02 0027 D www sciencemag org SCIENCE VOL 333 26 AUGUST 2011 14 tela ADVANCED Y ACCOUNT Science Magazine e Science AAAS ORG FEEDBACK HELP LIBRARIANS JOIN SUBSCRIBE NEWS SCIENCE JOURNALS CAREERS BLOGS amp COMMUNITIES MULTIMEDIA COLLECTIONS Science The World s Leading Journal of Original Scientific Research Global News and Commentary Science Home Currentlssue Previous Issues ScienceExpress Science Products My Science About the Journal Home gt Science Magazine gt 26 August 2011 gt Nakamura et al 333 6046 1113 1116 Science 26 August 2011 lt Prev Table of Contents Next gt ADVERTISEMENT Article Views Vol 333 no 6046 pp 1113 1116 gt Abstract DOI 10 1126 science 1207758 Science i ul Tent REPORT Webinar sn i Itokawa Dust Particles A Direct Link Between S Type Asteroids and Register for gt Figures Only Ordinary Chondrites upcoming webinars gt Supporting Online Access Now i r 4 4 2 Material Tomoki Nakamura Takaaki Noguchi Masahiko Tanaka Michael E Zolensky Makoto Kimura Akira Tsuchiyama Aiko Nakato Toshihiro OgamF Hatsumi Ishida Masayuki Uesugi Toru Yada Kei Shirai Akio Fujimura Ryuji Okazaki Scott A Sandford Yukihiro Ishibashi Masanao Abe Tatsuaki Okada Artic
17. those of thermally metamorphosed LL chondrites consistent with spectroscopic observations made from Earth and by the Hayabusa spacecraft Our results directly demonstrate that ordinary chondrites the most abundant meteorites found on Earth come from S type asteroids Mineral chemistry indicates that the majority of regolith surface particles suffered long term thermal annealing and subsequent impact shock suggesting that tokawa is an asteroid made of reassembled pieces of the interior portions of a once larger asteroid spacecraft amived at S IV y 1998 SF36 in September 2005 1 Remote sensing measurements from the space craft suggest that Itokawa consists of rocks sim ilar to LLS and LL6 ordinary chondrites 2 3 confirming ground based spectral characterization 4 On 20 and 26 November 2005 the spacecraft descended to touchdown and capture dust par ticles from MUSES C Regio This area cons of dust and gravel deposits dominated by grains up to 1 cm in diameter 5 Although the sam pler did not operate as planned an elastic sampling hom impacted onto the asteroid surface directing dust particles into the spacecraft s sample catcher device 5 The Hayabusa sample capsule suc cessfully landed in the Woomera Prohibited Area in South Australia on 13 June 2010 Dust par ticles collected at the second touchdown were recovered by two methods In one method we used a Teflon spatula to sweep particles from about 10 of the sur
18. 72 18 Y Nakamuta Y Motomura Meteorit Planet Sci 34 763 1999 19 V Slater Reynolds H Y McSween Jr Meteorit Planet Sci 40 745 2005 20 D H Lindsley Am Mineral 68 477 1983 21 J Fabri s Contrib Mineral Petrol 69 329 1979 References K Ozawa Geochim Cosmochim Acta 48 2597 1984 M Miyamoto N Fujii H Takeda Proc Lunar Planet Sci 12B 1145 1981 M Trieloff et al Nature 422 502 2003 H Y McSween et al in Asteroids lll W Bottke ef al Eds Univ of Arizona Press Tucson AZ 2002 pp 559 571 26 D St ffler K Keil E R D Scott Geochim Cosmochim Acta 55 3845 1991 27 H Miyamoto et al Science 316 1011 2007 28 P Lee Icarus 124 181 1996 29 D G Korycansky E Asphaug Icarus 171 110 2004 Acknowledgments We thank the Hayabusa project team for sample return KEK for synchrotron experiments H Nakano Y Yamazaki K Shimada Y Kakazu T Hashimoto M Konno Y Katsuya and Y Matsushita for technical support and J Grossman T Ikeda T Hokada K Ozawa Y Nakamuta and S Wakita for helpful discussions Supported by NASA grant 769583 07 03 M E Z and S A S Supporting Online Material www sciencemag org cgi content ful 333 6046 1113 DC1 Figs 1 to S8 Tables 1 to 5 References 30 40 2 May 2011 accepted 2 August 2011 10 1126 science 1207758 J on April 23 2013
19. More Information on Related Content Similar Articles In Science Magazine gt PubMed Search Google Scholar for Articles by Nakamura T gt Articles by Kawaguchi The Hayabusa spacecraft arrived at S IV type asteroid 25143 Itokawa formerly 1998 SF36 in September 2005 7 Remote sensing measurements from the spacecraft suggest that Itokawa consists of rocks similar to LL5 and LL6 ordinary chondrites 2 3 confirming ground based spectral characterization 4 On 20 and 26 November 2005 the spacecraft descended to touchdown and capture dust particles from MUSES C Regio This area consists of dust and gravel deposits dominated by grains up to 1 cm in diameter 5 Although the sampler did not operate as planned an elastic sampling horn impacted onto the asteroid surface directing dust particles into the spacecraft s sample catcher device 5 The Hayabusa sample capsule successfully landed in the Woomera Prohibited Area in South Australia on 13 June 2010 Dust particles collected at the second touchdown were recovered by two methods In one method we used a Teflon spatula to sweep particles from about 10 of the surface of a sample catcher In Related Resources In Science Magazi NEWS amp ANALYSIS h tt PLANETARY SCIENCH Richard A Kerr cience 26 A THIS WEEK IN SCIENCE Extraterrestrial Dust Collection The latest news from ScienceNOW career advice articles www sciencemag or 333 6046 1113 full
20. aft suggest that Itokawa consists of rocks sim ilar to LLS and LL6 ordinary chondrites 2 3 confirming ground based spectral characterization 4 On 20 and 26 November 2005 the spaceQ descended to touchdown a titles from MUSES C Regi of dust and gravel deposits up to 1 cm in diameter 5 he Hayabusa spacecraft arrived at S IV type asteroid 25143 Itokawa former ly 1998 SF36 in September 2005 7 Remote sensing measurements from the spa RTS greatly between particles fig 7 which is typ ical of moderately shocked astromaterial cor responding shock stages up to S4 6 26 MUSES C Regio probably formed by segre gation and accumulation of fine gravel into areas close to the gravitational center of Itokawa due to global scale electrostatic grain levitation vibration induced granular migration and deposition of slow moving ejecta launched from surface impacts 27 29 Therefore particles in MUSES C Regio originally derived from diverse regions of Itokawa Fortunately despite the small mass of the recovered a sp samples they record the critical steps in history of this asteroid Itokawa was classified n S type asteroid from terrestrial remote sen sing and it has been commonly suggested that S Wpe asteroids the most abundant asteroids ne inner asteroid belt are the parent bodies of or y chondrites Our petrologic data from M C Regio confirm that Itokawa is indeed
21. angrdinary chondrite LL4 to LL6 thereby finally e these asteroids and meteorites References and Notes 1 A Fujiwara et al Science 312 1330 2006 2 M Abe et al Science 312 1334 2006 QC ft T Okada et al Science 312 1338 2006 R Binzel A S Rivkin S J Bus M Sunshine T H Burbine Meteorit Planet Sci 36 1167 2001 H Yano et al Science 312 1350 2006 See supporting material on Science Online A Tsuchiyama et al Science 333 1125 2011 A Brearley R H Jones Rev Mineral 36 3 1 1998 A E Rubin Geochim Cosmochim Acta 54 1217 1990 J B Brady D J Cherniak In Diffusion in Minerals and Melts Y Zhang D J Cherniak Eds Mineralogical Society of America Chantilly VA 2010 pp 899 920 W R Van Schmus A Wood Geochim Cosmochim Acta 31 747 1967 E A Jobbins et al Mineral Mag 35 881 1966 T J McCoy E R D Scott R H Jones K Keil G J Taylor Geochim Cosmochim Acta 55 601 1991 G R Huss A E Rubin N Grossman in Meteorites and the Early Solar System II D S Lauretta H Y McSween Jr Eds University of Arizona Press Tucson AZ 2006 pp 567 586 15 T E Bunch K Keil K G Snetsinger Geochim Cosmochim Acta 31 1569 1967 16 M Kimura H Nakajima H Hiyagon M K Weisberg Geochim Cosmochim Acta 70 5634 2006 17 J V Smith J Geol 80 505 19
22. face of a sample catcher In the other method we gently tapped on the ex terior of the sample catcher causing particles to drop onto a pure silica gl lide 6 p ppan Department of Earth and Planetary Material Sciences Facul of Science Tohoku University Aoba Sendai Miyagi 980 8578 Japan College of Science Ibaraki University 2 1 1 Bunkyo Mito Ibaraki 310 8512 Japan Synchrotron X ray Station at SPring 8 National Institute for Materials Science Sayo Hyogo 679 5198 Japan ARES NASA Johnson Space Center Houston TX 77058 USA Department of Earth and Space Science Graduate School of Science Osaka University Toyonaka 560 0043 Japan JAXA ISAS 3 1 1 Yoshinodai Sagamihara Kanagawa 229 8510 Japan Department of Earth and Planetary Scence Faculty of Science Kyushu University Hakozaki Fukuoka 812 8581 Japan NASA Ames Research Center Moffett Field CA 94035 USA To whom correspondence should be addressed E mail tomoki m tehoku ac jp On the Teflon spatula we identified 1534 he Hayahi type asteroid 25143 Itokawa former rocky particles by means of a field emission anning electron microscope The particles have diameters ranging from 3 to 40 pm but are 1 mostly smaller than 10 um 7 Most Itokawa I particles are angular and are probably broken 1 pieces of larger rocks Among the 1534 harvested 1 rocky particles 1087 are monomineralic includ 1 ing 580 olivine particles 126 low Ca pyr
23. facemarks for https www jstage jst go jp article jn College of Knowledge and Library Sciences School of Informatics University of Tsukuba H at 7 DAI Presently with Fukoku Information Systems 19 5 19 40 1 a rt C e ch a r ja ttt Faculty of Library Information and Media Science University of Tsukuba 16 55 The Association for Natural Language Processing i igh 20 BR AF oe PRINT ISSN 1340 7619 2013 04 24 616 BHES J STAGE gt gt Vol 19 2012 No 5 p 401 418 D WE ONUSTISTAGE nip 19 401 Do http dx doi org 10 5715 jnlp 19 401 Bee 1 2 3 STAGE 20130319
24. heir surfaces Their appearance is typical of most Itokawa particles Two par ticles show different morphologies RA QD02 0013 Fig 1C has a smoother soccer ball shape whereas RA QD02 0027 Fig 1D consists of a large troilite crystal and smaller silicates Parti cles that contain troilite or taenite as major com ponents like RA QD02 0027 are rare Mineralogical analysis of individual tapped particles indicates that they consist mainly of coarse typically 10 to 50 um in diameter 7 crystalline silicates the most abundant being olivine The next most abundant minerals are low and high Ca pyroxene and plagioclase fig S6A Low Ca py roxene is exclusively composed of orthopyroxene except for RA QD02 0060 which is dominated by low Ca clinopyroxene monoclinic structure was confirmed by x ray diffraction The degree of crystallinity of silicates differs betv and within particles particularly for plagioclase Some particles contain chromite chlorapatite memillite and troilite up to 25 um in size Small inclusions up to 10 ym of taenite kamacite troilite and Se hte RCRD RIT tee IE Downloaded from www sciencemag org on April 23 2013 http 1207758 1 Tomoki Nakamura Takaaki Noguchi Masahiko Tanaka et al Itokawa Dust Particles A Direct Link Between S Type Asteroids and Ordinary Chondrites Science Vol 333 No 6046 2011 p 1113 1116 dx doi org 10
25. le Tools Munetaka Ueno Toshifumi Mukai Makoto Yoshikawa Junichiro Kawaguchi gt Podcast Interview ADVERTISEMENT gt Save to My Folders Author Affiliations gt Download Citation To whom correspondence should be addressed E mail tomoki m tohoku ac jp Science Alert Me When Article is ABSTRACT MOBILE Cited Now Available for Postto CiteULike The Hayabusa spacecraft successfully recovered dust particles from the surface of near Earth asteroid Mc 25143 ltokawa Synchrotron radiation x ray diffraction and transmission and scanning electron microscope analyses indicate that the mineralogy and mineral chemistry of the ltokawa dust particles are identical to those of thermally metamorphosed LL chondrites consistent with spectroscopic observations made from gt Commercial Reprints Earth and by the Hayabusa spacecraft Our results directly demonstrate that ordinary chondrites the most and E Prints abundant meteorites found on Earth come from S type asteroids Mineral chemistry indicates that the majority of regolith surface particles suffered long term thermal annealing and subsequent impact shock suggesting that Itokawa is an asteroid made of reassembled pieces of the interior portions of a once larger Related Content asteroid In Science Magazine gt E mail This Page gt Rights amp Permissions gt View PubMed Citation Science News amp Analysis by Kerr gt Science This Week in Science gt
26. oxenes s 156 high Ca pyroxenes 186 feldspars 172 plagi oclase and 14 K feldspar 113 troilites 13 chro ites 10 Ca phosphates and 3 Fe Ni metal 1 I I 1 I I 1 I 1 I I 1 I I I re meia WY ae grains The remaining 447 particles are poly mineralic mixtures mainly silicates Several other particles are silica minerals and K bearing halite all of uncertain origin Of the 40 particles removed by tapping diameters ranging from 30 to 180 um that were analyzed by x ray computed microtomog raphy 7 and diffraction 38 were sub jected to more detailed mineralogic analysis Backscattered electron images of selected par ticles are shown in Fig 1 A to D RA QD02 0030 Fig LA and RA QD02 0024 Fig 1B have a platy morphology are polymineralic and have many mineral grains 1 to 10 hm in diam eter adhering to their surfaces Their appearance is typical of most Itokawa particles Two par ticles show different morphologies RA QD02 0013 Fig 1C has a smoother soccer ball shape whereas RA QD02 0027 Fig 1D consists of a large troilite crystal and smaller silicates Parti cles that contain troilite or taenite as major com ponents like RA QD02 0027 are rare Mineralogical analysis of individual tapped particles indicates that they consist mainly of coarse typically 10 to SO um in diameter 7 crystalline silicates the most abundant being olivine The next most abundant minerals are lo
27. round based spectral characterization 4 On 20 and 26 November 2005 the spacecraft descended to touchdown and capture dust par ticles from MUSES C Regio This area consists of dust and gravel deposits dominated by grains up to 1 cm in diameter 5 Although the sam pler did not operate as planned an elastic sampling horn impacted onto the asteroid surface directing dust particles into the spacecraft s sample catcher device 5 The Hayabusa sample capsule suc cessfully landed in the Woomera Prohibited Area in South Australia on 13 June 2010 Dust par ticles collected at the second touchdown were recovered by two methods In one method we used a Teflon spatula to sweep particles from about 10 of the surface of a sample catcher In the other method we gently tapped on the ex terior of the sample catcher causing particles to drop onto a pure silica glass slide 6 Department of Earth and Planetary Material Sciences Faculty of Science Tohoku University Aoba Sendai Miyagi 980 8578 Japan College of Science Ibaraki University 2 1 1 Bunkyo Mito Ibaraki 310 8512 Japan Synchrotron X ray Station at SPring 8 National institute for Materials Science Sayo Hyogo 679 5198 Japan ARES NASA Johnson Space Center Houston TX 77058 USA Department of Earth and Space Science Graduate School af Science Osaka University Toyonaka 560 0043 Japan JAXA ISAS 3 1 1 Yoshinodai Sagamihara Kanagawa 229 8510 Japan
28. sahiko Tanaka Michael E Zolensky Makoto Kimura Akira Tsuchiyama Aiko Nakato Toshihiro Ogami Hatsumi Ishida Masayuki Uesugi Toru Yada Kei Shirai Akio Fujimura Ryuji Okazaki Scott A Sandford Yukihiro Ishibashi Masanao Abe s Tatsuaki Okada Munetaka Ueno Toshifumi Mukai Makoto Yoshikawa Junichiro Kawaguchi The Hayabusa spacecraft successfully recovered dust particles from the surface of near Earth asteroid 25143 Itokawa Synchrotron radiation x ray diffraction and transmission and scanning electron microscope analyses indicate that the mineralogy and mineral chemistry of the Itokawa dust particles are identical to those of thermally metamorphosed LL chondrites consistent with spectroscopic observations made from Earth and by the Hayabusa spacecraft Our results directly demonstrate that ordinary chondrites the most abundant meteorites found on Earth come from S type asteroids Mineral chemistry indicates that the majority of regolith surface particles suffered long term thermal annealing and subsequent impact shock suggesting that Itokawa is an asteroid made of reassembled pieces of the interior portions of a once larger asteroid he Hayabusa spacecraft amved at S IV type asteroid 25143 Itokawa former ly 1998 SF36 in September 2005 7 Remote sensing measurements from the space craft suggest that Itokawa consists of rocks sim ilar to LLS and LL6 ordinary chondrites 2 3 confirming g
29. w and high Ca pyroxene and plagioclase fig S6A Low Ca py roxene is exclusively composed of orthopyroxene except for RA QD02 0060 which is dominated by low Ca clinopyroxene monoclinic structure was confirmed by x ray diffraction The degree of crystallinity of silicates differs between and within particles particularly for plagioclase Some particles contain chromite chlorapatite memillite and troilite up to 25 um in size Small inclusions up to 10 pm of taenite kamacite troilite and www sciencemag org SCIENCE _ VOL 333 26 AUGUST 2011 Downloaded from www sciencemag org on April 23 2013 aii CO Se Se Fete 1X 2X Of the 40 particles removed by tapping diameters ranging from 30 to 180 um that ifs were analyzed by x ray computed microtomog raphy 7 and x ray diffraction 38 were sub jected to more detailed mineralogic analysis Backscattered electron images of selected par ticles are shown in Fig 1 A to D 0030 Fig 1A and RA QD02 00 have a platy morphology are poly have many mineral grains to 10 eter adhering to their surfaces The is typical of most Itokawa particl ticles show different morphologies 0013 Fig 1C has a smoother soco whereas RA QD02 0027 Fig 1D large troilite crystal and smaller si cles that contain troilite or taenite al 0002 0013 0 and RA QD02 0027 0 cr
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