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 >

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

Files in This Item:
13kozasa_PIAUs255.pdf246.39 kBPDFView/Open
Please use this identifier to cite or link to this item:http://hdl.handle.net/2115/42831

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)

Submitter: 小笹 隆司

Export metadata:

OAI-PMH ( junii2 , jpcoar )

MathJax is now OFF:


 

Feedback - Hokkaido University