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Evolution of Dust in Primordial Supernova Remnants and Its Influence on the Elemental Composition of Hyper-Metal-Poor Stars

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Title: Evolution of Dust in Primordial Supernova Remnants and Its Influence on the Elemental Composition of Hyper-Metal-Poor 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
early universe
supernovae: general
stars; abundances
Population III
PACS=95.30.Lz
PACS=95.30.Wi
PACS=97.10.Tk
PACS=97.20.Wt
PACS=97.60.Bw
PACS=98.38.Mz
Issue Date: 21-May-2008
Publisher: American Institute of Physics
Citation: Origin of Matter and Evolution of Galaxies : The 10th International Symposium on Origin of Matter and Evolution of Galaxies : From the Dawn of Universe to the Formation of Solar System. Edited by Takuma Suda, Takaya Nozawa, Akira Ohnishi, Kiyoshi Kato, Masayuki Y. Fujimoto, Toshitaka Kajino, Shigeru Kubono. ISBN: 978-0-7354-0537-0
Journal Title: AIP Conference Proceedings
Volume: 1016
Issue: 1
Start Page: 55
End Page: 60
Publisher DOI: 10.1063/1.2943632
Abstract: The calculations for the evolution of dust within Population III supernova remnants (SNRs) are presented, based on the models of dust formed in the unmixed ejecta of Type II SNe. We show that once dust grains collide with the reverse shock penetrating into the ejecta, their fates strongly depend on the initial radius a_ini. For SNRs expanding into the interstellar medium (ISM) with n_[H,0] = 1 cm^[−3], grains of a_ini<0.05 µm are trapped in the hot gas to be completely destroyed; grains of a_ini = 0.05–0.2 µm are piled up in the dense shell formed behind the forward shock; grains of a_ini>0.2 µm are injected into the ISM without being eroded significantly. The total mass of surviving dust is 0.01 to 0.8 M☉ for n_[H,0] = 10 to 0.1 cm^[−3]. We also investigate the influence of the piled-up dust on the elemental abundances of the second-generation stars formed in the dense shell of Population III SNRs. The comparison of the calculated elemental abundances with those observed in hyper-metal-poor (HMP) and ultra-metal-poor (UMP) stars indicates that the transport of dust separated from metal-rich gas can be an important process in determining the abundance patterns of Mg and Si in HMP and UMP stars.
Description: Origin of Matter and Evolution of Galaxies: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System. 4–7 December 2007. Sapporo, Japan.
Conference Name: International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System
Conference Sequence: 10
Conference Place: Sapporo
Rights: Copyright 2008 American Institute of Physics. This article may be downloaded for personal use only. Any other use requires prior permission of the author and the American Institute of Physics. The following article appeared in AIP Conf. Proc., 2008, Volume 1016, pp. 55-60, and may be found at https://dx.doi.org/10.1063/1.2943632
Type: proceedings
URI: http://hdl.handle.net/2115/42826
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)

Submitter: 小笹 隆司

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