Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0801.2015)
· References in the article
· Citations to the Article (17) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (8)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Early Formation of Dust in the Ejecta of Type Ib SN 2006jc and Temperature and Mass of the Dust
Authors:
Nozawa, Takaya; Kozasa, Takashi; Tominaga, Nozomu; Sakon, Itsuki; Tanaka, Masaomi; Suzuki, Tomoharu; Nomoto, Ken'ichi; Maeda, Keiichi; Umeda, Hideyuki; Limongi, Marco; Onaka, Takashi
Affiliation:
AA(Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan; .; Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8568, Japan.), AB(Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan; .), AC(Optical and Infrared Astronomy Division, National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.; Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.), AD(Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.), AE(Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.), AF(Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.), AG(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.), AH(Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8568, Japan.; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Strasse 1, 85741 Garching, Germany.), AI(Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.), AJ(Istituto Nazionale di Astrofisica-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monteporzio Catone, Italy.; Center for Stellar and Planetary Astrophysics, School of Mathematical Sciences, P.O. Box 28M, Monash University, Victoria 3800, Australia.), AK(Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.)
Publication:
The Astrophysical Journal, Volume 684, Issue 2, pp. 1343-1350. (ApJ Homepage)
Publication Date:
09/2008
Origin:
UCP
ApJ Keywords:
ISM: Dust, Extinction, Stars: Supernovae: General, supernovae: individual (SN 2006jc)
DOI:
10.1086/589961
Bibliographic Code:
2008ApJ...684.1343N

Abstract

SN 2006jc is a peculiar supernova (SN), in which the formation of dust has been confirmed at an early epoch of ~50 days after the explosion. We investigate the possibility of such an early formation of dust grains in the expanding ejecta of SN 2006jc, applying the Type Ib SN model that is developed to reproduce the observed light curve. We find that the rapid decrease of the gas temperature in SN 2006jc enables the condensation of C grains in the C-rich layer at 40-60 days after the explosion, which is followed by the condensation of silicate and oxide grains until ~200 days. The average radius of each grain species is confined to be less than 0.01 μm due to the low gas density at the condensation time. The calculated total dust mass reaches ~=1.5 Msolar, of which C dust shares 0.7 Msolar. On the other hand, based on the calculated dust temperature, we show that the dust species and mass evaluated to reproduce the spectral energy distribution observed by AKARI and MAGNUM at day 200 are different from those obtained by the dust formation calculations; the dust species contributing to the observed flux are hot C and FeS grains with masses of 5.6×10-4 and 2.0×10-3 Msolar, respectively, although we cannot defy the presence of a large amount of cold dust such as silicate and oxide grains up to 0.5 Msolar. One of the physical processes responsible for the difference between calculated and evaluated masses of C and FeS grains could be considered to be the destruction of small-sized clusters by energetic photons and electrons prevailing within the ejecta at the earlier epoch.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints