HUSCAP logo Hokkaido Univ. logo

Hokkaido University Collection of Scholarly and Academic Papers >
Graduate School of Science / Faculty of Science >
Peer-reviewed Journal Articles, etc >

Dust Evolution in Population III Supernova Remnants

Files in This Item:
20kozasa_AIPCP990.pdf284.14 kBPDFView/Open
Please use this identifier to cite or link to this item:http://hdl.handle.net/2115/42825

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)

Submitter: 小笹 隆司

Export metadata:

OAI-PMH ( junii2 , jpcoar )

MathJax is now OFF:


 

Feedback - Hokkaido University