Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-22T16:21:30.901Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of newly formed dust in Population III supernova remnants and its impact on the elemental composition of Population II.5 stars

Published online by Cambridge University Press:  01 June 2008

Takaya Nozawa ,
Takashi Kozasa ,
Asao Habe ,
Eli Dwek ,
Hideyuki Umeda ,
Nozomu Tominaga ,
Keiichi Maeda  and
Ken'ichi Nomoto
Takaya Nozawa
Affiliation:
Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan email: [email protected] Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8568, Japan
Takashi Kozasa
Affiliation:
Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan email: [email protected]
Asao Habe
Affiliation:
Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan email: [email protected]
Eli Dwek
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Hideyuki Umeda
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Nozomu Tominaga
Affiliation:
Division of Optical and Infrared Astronomy, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Keiichi Maeda
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8568, Japan Max-Planck-Institut für Astrophysik, 85741 Garching, Germany
Ken'ichi Nomoto
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8568, Japan Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan Research Center for the Early Universe, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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 aini. For Type II SNRs expanding into the ambient medium with density of nH,0 = 1 cm−3, grains of aini < 0.05 μm are detained in the shocked hot gas and are completely destroyed, while grains of aini > 0.2 μm are injected into the surrounding medium without being significantly destroyed. Grains with aini = 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 10−6–10−4Z⊙, 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.

Keywords

dustextinctionsupernovae: generalhydrodynamicsshock wavesstars: abundancesstars: chemically peculiarmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 254 - 259
Copyright
Copyright © International Astronomical Union 2008

References

Bianchi, S. & Schneider, R. 2007, MNRAS, 378, 973CrossRefGoogle Scholar
Cazaux, S. & Spaans, M. 2004, ApJ, 611, 40CrossRefGoogle Scholar
Collet, R., Asplund, M., & Trampedach, R. 2006, ApJ, 644, L121CrossRefGoogle Scholar
Frebel, A., et al. , 2008, ApJ, accepted [arXiv:0805.3341]Google Scholar
Machida, M. N., et al. , 2005, ApJ, 622, 39CrossRefGoogle Scholar
Mackey, J., Bromm, V., & Hernquist, L. 2003, ApJ, 586, 1CrossRefGoogle Scholar
Norris, J. E., et al. , 2007, ApJ, 670, 774CrossRefGoogle Scholar
Nozawa, T., et al. , 2003, ApJ, 598, 785CrossRefGoogle Scholar
Nozawa, T., et al. , 2007, ApJ, 666, 955CrossRefGoogle Scholar
Omukai, K., et al. , 2005, ApJ, 626, 627CrossRefGoogle Scholar
Salvaterra, R., Ferrara, A., & Schneider, R. 2004, New A, 10, 113CrossRefGoogle Scholar
Schneider, R., Ferrara, A., & Salvaterra, R. 2004, MNRAS, 351, 1379CrossRefGoogle Scholar
Schneider, R., et al. , 2006, MNRAS, 369, 1437CrossRefGoogle Scholar
Todini, P. & Ferrara, A. 2001, MNRAS, 325, 726CrossRefGoogle Scholar
Tsuribe, T. & Omukai, K. 2006, ApJ, 642, L61CrossRefGoogle Scholar