| Title: | Dust Evolution in Population III Supernova Remnants |
| 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 |
| shock waves |
| supernova remnants |
| supernovae: general |
| 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: | 11-Mar-2008 |
| Publisher: | American Institute of Physics |
| Citation: | First Stars III : First Stars II Conference. Edited by Brian W. O'Shea, Alexander Heger, and Tom Abel. ISBN: 978-0-7354-0509-7 |
| Journal Title: | AIP Conference Proceedings |
| Volume: | 990 |
| Issue: | 1 |
| Start Page: | 426 |
| End Page: | 428 |
| Publisher DOI: | 10.1063/1.2905654 |
| Abstract: | We present the results of calculations for the evolution of dust within Population III supernova remnants (SNRs), focusing on the dust formed in the unmixed ejecta of Type II SNe. We show that once dust grains inside the He core encounter the reverse shock, they are subject to different fates depending on their initial sizes 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 and are completely destroyed; grains of a_ini = 0.05-0.2μm are trapped in the dense shell behind the forward shock with the final sizes of 0.001-0.1μm; grains of a_ini > 0.2μm are injected into the ISM without significant destruction. The total mass of surviving dust is 0.01 to 0.8 M☉ and is higher for the lower ISM gas density. We also investigate the elemental abundances of the second-generation stars that form in the dense shell of Population III SNRs, based on the elemental composition of dust piled up in the shell. The comparison of those results with the observations of hyper-metal poor (HMP) stars indicates that the transport of dust segregated from metal-rich gas within a SNR can be responsible for the abundance patterns of Mg and Si in HMP stars. |
| Description: | First Stars III: First Stars II Conference. Santa Fe, New Mexico, U.S.A. 15–20 July 2007. |
| Conference Name: | First Stars III: First Stars II Conference |
| Conference Place: | Santa Fe, New Mexico |
| 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 990, pp. 426-428, and may be found at https://dx.doi.org/10.1063/1.2905654 |
| Type: | proceedings |
| URI: | http://hdl.handle.net/2115/42825 |
| 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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