Dust formation and He II λ4686 emission in the dense shell of the peculiar type Ib supernova 2006jc

Nathan Smith, Ryan J. Foley, Alexei V. Filippenko

Research output: Contribution to journalArticle

111 Citations (Scopus)

Abstract

We present evidence for the formation of dust grains in an unusual Type Ib supernova (SN) based on late-time spectra of SN 2006jc. The progenitor suffered an outburst qualitatively similar to those of luminous blue variables (LBVs) just 2 yr prior to the SN, and we propose that the dust formation is a consequence of the SN blast wave overtaking that .LBV-like shell. The key evidence for dust formation is (1) the appearance of a red/near-infrared continuum emission source that can be fit by T ≈, 1600 K graphite grains, and (2) fading of the redshifted sides of intermediate-width He I emission lines, yielding progressively more asymmetric blueshifted lines as dust obscures receding material. This provides the strongest case yet for dust formation in any SN Ib/c. Both developments occurred between 51 and 75 days after peak brightness, while the few other SNe observed to form dust did so after a few hundred days. Geometric considerations indicate that dust formed in the dense swept-up shell between the forward and reverse shocks, and not in the freely expanding SN ejecta. The rapid cooling leading to dust formation may have been aided by extremely high shell densities of 1010 cm-3, indicated by Heiline ratios. The brief epoch of dust formation is accompanied by He n 24686 emission and enhanced X-ray emission, suggesting a common link. These clues imply that the unusual dust formation in this object was not attributable to properties of the SN itself, but instead-like most peculiarities of SN 2006jc-was a consequence of interaction with the dense environment created by an LBV-like eruption 2 yr before the SN.

Original languageEnglish (US)
Pages (from-to)568-579
Number of pages12
JournalAstrophysical Journal
Volume680
Issue number1
DOIs
StatePublished - Jun 10 2008
Externally publishedYes

Fingerprint

supernovae
dust
shell
blasts
fading
ejecta
outburst
graphite
volcanic eruptions
near infrared
brightness
volcanic eruption
shock
time measurement
continuums
cooling

Keywords

  • Dust, extinction
  • Stars: mass loss
  • Stars: Winds, outflows
  • Stars: Wolf-Rayet
  • Supernovae: Individual (SN 2006jc)

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Dust formation and He II λ4686 emission in the dense shell of the peculiar type Ib supernova 2006jc. / Smith, Nathan; Foley, Ryan J.; Filippenko, Alexei V.

In: Astrophysical Journal, Vol. 680, No. 1, 10.06.2008, p. 568-579.

Research output: Contribution to journalArticle

@article{1844079adb7040cd96c7edb6db8574f1,
title = "Dust formation and He II λ4686 emission in the dense shell of the peculiar type Ib supernova 2006jc",
abstract = "We present evidence for the formation of dust grains in an unusual Type Ib supernova (SN) based on late-time spectra of SN 2006jc. The progenitor suffered an outburst qualitatively similar to those of luminous blue variables (LBVs) just 2 yr prior to the SN, and we propose that the dust formation is a consequence of the SN blast wave overtaking that .LBV-like shell. The key evidence for dust formation is (1) the appearance of a red/near-infrared continuum emission source that can be fit by T ≈, 1600 K graphite grains, and (2) fading of the redshifted sides of intermediate-width He I emission lines, yielding progressively more asymmetric blueshifted lines as dust obscures receding material. This provides the strongest case yet for dust formation in any SN Ib/c. Both developments occurred between 51 and 75 days after peak brightness, while the few other SNe observed to form dust did so after a few hundred days. Geometric considerations indicate that dust formed in the dense swept-up shell between the forward and reverse shocks, and not in the freely expanding SN ejecta. The rapid cooling leading to dust formation may have been aided by extremely high shell densities of 1010 cm-3, indicated by Heiline ratios. The brief epoch of dust formation is accompanied by He n 24686 emission and enhanced X-ray emission, suggesting a common link. These clues imply that the unusual dust formation in this object was not attributable to properties of the SN itself, but instead-like most peculiarities of SN 2006jc-was a consequence of interaction with the dense environment created by an LBV-like eruption 2 yr before the SN.",
keywords = "Dust, extinction, Stars: mass loss, Stars: Winds, outflows, Stars: Wolf-Rayet, Supernovae: Individual (SN 2006jc)",
author = "Nathan Smith and Foley, {Ryan J.} and Filippenko, {Alexei V.}",
year = "2008",
month = "6",
day = "10",
doi = "10.1086/587860",
language = "English (US)",
volume = "680",
pages = "568--579",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - Dust formation and He II λ4686 emission in the dense shell of the peculiar type Ib supernova 2006jc

AU - Smith, Nathan

AU - Foley, Ryan J.

AU - Filippenko, Alexei V.

PY - 2008/6/10

Y1 - 2008/6/10

N2 - We present evidence for the formation of dust grains in an unusual Type Ib supernova (SN) based on late-time spectra of SN 2006jc. The progenitor suffered an outburst qualitatively similar to those of luminous blue variables (LBVs) just 2 yr prior to the SN, and we propose that the dust formation is a consequence of the SN blast wave overtaking that .LBV-like shell. The key evidence for dust formation is (1) the appearance of a red/near-infrared continuum emission source that can be fit by T ≈, 1600 K graphite grains, and (2) fading of the redshifted sides of intermediate-width He I emission lines, yielding progressively more asymmetric blueshifted lines as dust obscures receding material. This provides the strongest case yet for dust formation in any SN Ib/c. Both developments occurred between 51 and 75 days after peak brightness, while the few other SNe observed to form dust did so after a few hundred days. Geometric considerations indicate that dust formed in the dense swept-up shell between the forward and reverse shocks, and not in the freely expanding SN ejecta. The rapid cooling leading to dust formation may have been aided by extremely high shell densities of 1010 cm-3, indicated by Heiline ratios. The brief epoch of dust formation is accompanied by He n 24686 emission and enhanced X-ray emission, suggesting a common link. These clues imply that the unusual dust formation in this object was not attributable to properties of the SN itself, but instead-like most peculiarities of SN 2006jc-was a consequence of interaction with the dense environment created by an LBV-like eruption 2 yr before the SN.

AB - We present evidence for the formation of dust grains in an unusual Type Ib supernova (SN) based on late-time spectra of SN 2006jc. The progenitor suffered an outburst qualitatively similar to those of luminous blue variables (LBVs) just 2 yr prior to the SN, and we propose that the dust formation is a consequence of the SN blast wave overtaking that .LBV-like shell. The key evidence for dust formation is (1) the appearance of a red/near-infrared continuum emission source that can be fit by T ≈, 1600 K graphite grains, and (2) fading of the redshifted sides of intermediate-width He I emission lines, yielding progressively more asymmetric blueshifted lines as dust obscures receding material. This provides the strongest case yet for dust formation in any SN Ib/c. Both developments occurred between 51 and 75 days after peak brightness, while the few other SNe observed to form dust did so after a few hundred days. Geometric considerations indicate that dust formed in the dense swept-up shell between the forward and reverse shocks, and not in the freely expanding SN ejecta. The rapid cooling leading to dust formation may have been aided by extremely high shell densities of 1010 cm-3, indicated by Heiline ratios. The brief epoch of dust formation is accompanied by He n 24686 emission and enhanced X-ray emission, suggesting a common link. These clues imply that the unusual dust formation in this object was not attributable to properties of the SN itself, but instead-like most peculiarities of SN 2006jc-was a consequence of interaction with the dense environment created by an LBV-like eruption 2 yr before the SN.

KW - Dust, extinction

KW - Stars: mass loss

KW - Stars: Winds, outflows

KW - Stars: Wolf-Rayet

KW - Supernovae: Individual (SN 2006jc)

UR - http://www.scopus.com/inward/record.url?scp=46249134181&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=46249134181&partnerID=8YFLogxK

U2 - 10.1086/587860

DO - 10.1086/587860

M3 - Article

VL - 680

SP - 568

EP - 579

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -