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Title: FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE

Abstract

We investigate the formation of dust grains in the ejecta of Type Ia supernovae (SNe Ia), adopting the carbon-deflagration W7 model. In the calculations of dust formation, we apply the nucleation and grain growth theory and consider the two extreme cases of the formation of CO and SiO molecules: complete formation and no formation. The results of the calculations show that for the sticking probability of {alpha}{sub j} = 1, C, silicate, Si, and FeS grains can condense at early times of {approx}100-300 days after the explosion, whereas Fe and SiC grains cannot form substantially. Due to the low gas density in SNe Ia with no H-envelope, the average radii of the newly formed grains are generally below 0.01 {mu}m, being much smaller than those in Type II-P SNe. This supports our previous conclusion that the radius of dust formed in the ejecta is smaller in SNe with less massive envelopes. The total dust mass ranges from 3 x 10{sup -4} M{sub sun} to 0.2 M{sub sun} for {alpha}{sub j} = 0.1-1, depending on whether or not CO and SiO molecules are formed. We also estimate the optical depths and thermal emission by the newly formed dust and compare themmore » to the relevant observations of SNe Ia. We find that the formation of C grains in SNe Ia must be suppressed to be consistent with observational constraints. This implies that energetic photons and electrons heavily depress the formation efficiency of C grains or that the outermost C-O layer of SNe Ia is almost fully burned. Finally, we calculate dust destruction in the SN remnants and find that dust grains formed in the ejecta of SNe Ia are almost completely destroyed in the shocked gas before being injected into the interstellar medium. This indicates that SNe Ia are unlikely to be the major sources of interstellar dust.« less

Authors:
; ; ;  [1];  [2];  [3]
  1. Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8583 (Japan)
  2. Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810 (Japan)
  3. Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033 (Japan)
Publication Date:
OSTI Identifier:
21578326
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 736; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/736/1/45; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABUNDANCE; CARBON MONOXIDE; DUSTS; GRAIN GROWTH; INTERSTELLAR SPACE; IRON; IRON SULFIDES; NUCLEATION; SILICON CARBIDES; SILICON OXIDES; SUPERNOVA REMNANTS; SUPERNOVAE; BINARY STARS; CARBIDES; CARBON COMPOUNDS; CARBON OXIDES; CHALCOGENIDES; COSMIC RADIO SOURCES; ELEMENTS; ERUPTIVE VARIABLE STARS; IRON COMPOUNDS; METALS; OXIDES; OXYGEN COMPOUNDS; SILICON COMPOUNDS; SPACE; STARS; SULFIDES; SULFUR COMPOUNDS; TRANSITION ELEMENT COMPOUNDS; TRANSITION ELEMENTS; VARIABLE STARS

Citation Formats

Nozawa, Takaya, Maeda, Keiichi, Tanaka, Masaomi, Nomoto, Ken'ichi, Kozasa, Takashi, and Umeda, Hideyuki, E-mail: takaya.nozawa@ipmu.jp. FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE. United States: N. p., 2011. Web. doi:10.1088/0004-637X/736/1/45.
Nozawa, Takaya, Maeda, Keiichi, Tanaka, Masaomi, Nomoto, Ken'ichi, Kozasa, Takashi, & Umeda, Hideyuki, E-mail: takaya.nozawa@ipmu.jp. FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE. United States. doi:10.1088/0004-637X/736/1/45.
Nozawa, Takaya, Maeda, Keiichi, Tanaka, Masaomi, Nomoto, Ken'ichi, Kozasa, Takashi, and Umeda, Hideyuki, E-mail: takaya.nozawa@ipmu.jp. Wed . "FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE". United States. doi:10.1088/0004-637X/736/1/45.
@article{osti_21578326,
title = {FORMATION OF DUST IN THE EJECTA OF TYPE Ia SUPERNOVAE},
author = {Nozawa, Takaya and Maeda, Keiichi and Tanaka, Masaomi and Nomoto, Ken'ichi and Kozasa, Takashi and Umeda, Hideyuki, E-mail: takaya.nozawa@ipmu.jp},
abstractNote = {We investigate the formation of dust grains in the ejecta of Type Ia supernovae (SNe Ia), adopting the carbon-deflagration W7 model. In the calculations of dust formation, we apply the nucleation and grain growth theory and consider the two extreme cases of the formation of CO and SiO molecules: complete formation and no formation. The results of the calculations show that for the sticking probability of {alpha}{sub j} = 1, C, silicate, Si, and FeS grains can condense at early times of {approx}100-300 days after the explosion, whereas Fe and SiC grains cannot form substantially. Due to the low gas density in SNe Ia with no H-envelope, the average radii of the newly formed grains are generally below 0.01 {mu}m, being much smaller than those in Type II-P SNe. This supports our previous conclusion that the radius of dust formed in the ejecta is smaller in SNe with less massive envelopes. The total dust mass ranges from 3 x 10{sup -4} M{sub sun} to 0.2 M{sub sun} for {alpha}{sub j} = 0.1-1, depending on whether or not CO and SiO molecules are formed. We also estimate the optical depths and thermal emission by the newly formed dust and compare them to the relevant observations of SNe Ia. We find that the formation of C grains in SNe Ia must be suppressed to be consistent with observational constraints. This implies that energetic photons and electrons heavily depress the formation efficiency of C grains or that the outermost C-O layer of SNe Ia is almost fully burned. Finally, we calculate dust destruction in the SN remnants and find that dust grains formed in the ejecta of SNe Ia are almost completely destroyed in the shocked gas before being injected into the interstellar medium. This indicates that SNe Ia are unlikely to be the major sources of interstellar dust.},
doi = {10.1088/0004-637X/736/1/45},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 736,
place = {United States},
year = {2011},
month = {7}
}