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Evolution of newly formed dust in Population III supernova remnants and its impact on the elemental composition of Population II.5 stars
| Title: | Evolution of newly formed dust in Population III supernova remnants and its impact on the elemental composition of Population II.5 stars |
| Authors: | Nozawa, Takaya Browse this author →KAKEN DB | | Kozasa, Takashi Browse this author →KAKEN DB | | Habe, Asao Browse this author →KAKEN DB | | Dwek, Eli Browse this author | | Umeda, Hideyuki Browse this author →KAKEN DB | | Tominaga, Nozomu Browse this author | | Maeda, Keiichi Browse this author →KAKEN DB | | Nomoto, Ken'ichi Browse this author |
| Keywords: | dust | | extinction | | supernovae: general | | hydrodynamics | | shock waves | | stars: abundances | | stars: chemically peculiar | | methods: numerical |
| Issue Date: | 2008 |
| Publisher: | Cambridge University Press |
| Citation: | Low-Metallicity Star Formation : From the First Stars to Dwarf Galaxies. L.K. Hunt, S. Madden and R. Schneider, eds. |
| Journal Title: | Proceedings of the International Astronomical Union |
| Volume: | 4 |
| Issue: | S255 |
| Start Page: | 254 |
| End Page: | 259 |
| Publisher DOI: | 10.1017/S1743921308024903 |
| Abstract: | We investigate the evolution of dust formed in Population III supernovae (SNe) by considering its transport and processing by sputtering within the SN remnants (SNRs). We find that the fate of dust grains within SNRs heavily depends on their initial radii a_ini. For Type II SNRs expanding into the ambient medium with density of n_[H,0] = 1 cm^[-3], grains of a_ini < 0.05 μm are detained in the shocked hot gas and are completely destroyed, while grains of a_ini > 0.2 μm are injected into the surrounding medium without being significantly destroyed. Grains with a_ini = 0.05-0.2 μm are finally trapped in the dense shell behind the forward shock. We show that the grains piled up in the dense shell enrich the gas up to 10^[-6]-10^[-4] Z☉, high enough to form low-mass stars with 0.1-1 M☉. In addition, [Fe/H] in the dense shell ranges from -6 to -4.5, which is in good agreement with the ultra-metal-poor stars with [Fe/H] < -4. We suggest that newly formed dust in a Population III SN can have great impact on the stellar mass and elemental composition of Population II.5 stars formed in the shell of the SNR. |
| Conference Name: | IAU Symposium |
| Conference Sequence: | 255 |
| Conference Place: | Rapallo, Genova |
| Rights: | © 2008 International Astronomical Union |
| Type: | proceedings |
| URI: | http://hdl.handle.net/2115/42831 |
| Appears in Collections: | 理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)
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Submitter: 小笹 隆司
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