DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Meikle, P.; Kotak, R.; Farrah, D.; Mattila, S.; Dyk, Schuyler D. Van; Andersen, Anja C.; Fesen, Rob; Filippenko, A. V.; Foley, R. J.; Fransson, Claes; Gerardy, Christopher L.; Hoêflich, P.; Lundqvist, Peter; Pozzo, Monica; Sollerman, J.; Wheeler, J. C.

doi:10.1088/0004-637x/732/2/109

Cited by 73 publications

(83 citation statements)

References 95 publications

(308 reference statements)

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“…10. Total modelled dust masses versus post-explosion time for the various SN cases considered in this study and dust masses derived from mid-IR data for a sample of Type II-P SNe-SN1987A (Wooden et al 1993;Ercolano et al 2007), SN1999em (Elmhamdi et al 2003), SN2003gd (Sugerman et al 2006;Meikle et al 2007), SN2003J (Szalai & Vinkó 2013), SN2004dj (Szalai et al 2011;Meikle et al 2011 well with the latest submm dust masses derived from Herschel and ALMA data for SN1987A and other SNRs. The trend of a gradual growth of dust grains over ∼3−5 years is in contrast with recent radiative transfer study of SN1987A by Wesson et al (2015), who conclude the major growth of dust grains has taken place between day 1200 and day 9200, and that the grains are very large (a ∼ 3−5 µm).…”

Section: Summary and Discussionsupporting

confidence: 64%

Condensation of dust in the ejecta of Type II-P supernovae

Sarangi

Cherchneff

2015

A&A

138

189

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Aims. We study the production of dust in Type II-P supernova ejecta by coupling the gas-phase chemistry to the dust nucleation and condensation phases. We consider two supernova progenitor masses with homogeneous and clumpy ejecta to assess the chemical type and quantity of dust that forms. Grain size distributions are derived for all dust components as a function of post-explosion time.Methods. The chemistry of the gas phase and the simultaneous formation of dust clusters are described by a chemical network that includes all possible processes that are efficient at high gas temperatures and densities. The formation of key bimolecular species (e.g., CO, SiO) and dust clusters of silicates, alumina, silica, metal carbides, metal sulphides, pure metals, and amorphous carbon is considered. A set of stiff, coupled, ordinary, differential equations is solved for the gas conditions pertaining to supernova explosions. These master equations are coupled to a dust condensation formalism based on Brownian coagulation. Results. We find that Type II-P supernovae produce dust grains of various chemical compositions and size distributions as a function of post-explosion time. The grain size distributions gain in complexity with time, are slewed towards large grains, and differ from the usual Mathis, Rumpl, & Nordsieck power-law distribution characterising interstellar dust. Gas density enhancements in the form of ejecta clumps strongly affect the chemical composition of dust and the grain size distributions. Some dust type, such as forsterite and pure metallic grains, are highly dependent on clumpiness. Specifically, a clumpy ejecta produces large grains over 0.1 µm, and the final dust mass for the 19 M progenitor reaches 0.14 M . Clumps also favour the formation of specific molecules, such as CO 2 , in the oxygen-rich zones. Conversely, the carbon and alumina dust masses are primarily controlled by the mass yields of alumina and carbon in the ejecta zones where the dust is produced. The supernova progenitor mass and the 56 Ni mass also affect dust production. Our results highlight that dust synthesis in Type II-P supernovae is not a single and simple process, as often assumed. Several dust components form in the ejecta over time and the total dust mass gradually builds up over a time span around three to five years post-outburst. This gradual growth provides a possible explanation for the discrepancy between the small amounts of dust formed at early post-explosion times and the high dust masses derived from recent observations of supernova remnants.

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Section: Summary and Discussionsupporting

confidence: 64%

Condensation of dust in the ejecta of Type II-P supernovae

Sarangi

Cherchneff

2015

A&A

138

189

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“…IR observations of young SNe (t 1-2 yr) in external galaxies usually find only 10 −5 -10 −3 M of dust (e.g., Wooden et al 1993;Ercolano et al 2007;Elmhamdi et al 2003;Meikle et al 2007Meikle et al , 2011Kotak et al 2009;Szalai et al 2011). On the other hand, observations of SNRs in our Galaxy and Large/Small Magellanic Clouds detect a larger amount of dust.…”

Section: Sn Dustmentioning

confidence: 80%

“…In fact, IR echo by the IS dust has been detected for several extragalactic SNe (Meikle et al 2007(Meikle et al , 2011Kotak et al 2009) and Cas A (Krause et al 2005;. The difference from the CS dust is that the density is set to be uniform and that the much larger outer radius is allowed.…”

Section: Light Echomentioning

confidence: 99%

A Search for Infrared Emission From Core-Collapse Supernovae at the Transitional Phase

Tanaka¹,

Nozawa²,

Sakon³

et al. 2012

ApJ

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Most of the observational studies of supernova (SN) explosions are limited to early phases (100 yr) in our Galaxy or very nearby galaxies. SNe at the epoch between these two, which we call the "transitional" phase, have not been explored in detail except for several extragalactic SNe including SN 1987A in the Large Magellanic Cloud. We present theoretical predictions for the infrared (IR) dust emissions by several mechanisms; emission from dust formed in the SN ejecta, light echo by circumstellar (CS) and interstellar (IS) dust, and emission from shocked CS dust. We search for IR emission from six core-collapse SNe at the transitional phase in the nearby galaxies NGC 1313, NGC 6946, and M101 by using the data taken with the AKARI satellite and Spitzer. Among six targets, we detect the emission from SN 1978K in NGC 1313. SN 1978K is associated with 1.3 × 10 −3 M of silicate dust. We show that, among several mechanisms, the shocked CS dust is the most probable emission source to explain the IR emission observed for SN 1978K. IR emission from the other five objects is not detected. Our current observations are sensitive to IR luminosity of >10 38 erg s −1 , and the non-detection of SN 1962M excludes the existence of the shocked CS dust for a high gas mass-loss rate of ∼10 −4 M yr −1 . Observations of SNe at the transitional phase with future IR satellites will fill the gap of IR observations of SNe with the age of 10-100 yr, and give a new opportunity to study the CS and IS environments of the progenitor, and possibly dust formation in SNe.

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“…Kotak et al 2009;Fox et al 2010;Otsuka et al 2010;Szalai et al 2011;Meikle et al 2011). Observations in X-ray and radio may also provide useful additional information about SN-CSM interactions.…”

Section: Discussionmentioning

confidence: 99%

Twelve type II-P supernovae seen with the eyes ofSpitzer

Szalai

Vinkó

2012

A&A

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Context. Core-collapse supernovae (CC SNe), especially those of type II-plateau (II-P), are thought to be important contributors to cosmic dust production. The most obvious indicator of newly-formed and/or pre-existing dust is the time-dependent mid-infrared (MIR) excess coming from the environment of SNe. In the past few years several CC SNe were monitored by the Spitzer Space Telescope in the nebular phase, hundreds of days after explosion. On the other hand, only a few of these objects have been analyzed and published to date. Aims. Our goal was to collect publicly available, previously unpublished measurements on type II-P (or peculiar IIP) SNe from the Spitzer database. The most important aspect was to find SNe observed with the Infrared Array Camera (IRAC) on at least two epochs. The temporal changes of the observed fluxes may be indicative of the underlying supernova, while spectral energy distribution (SED) fitting to the fluxes in different IRAC channels may reveal the physical parameters of the mid-IR radiation, which is presumably caused by warm dust. Methods. The IRS spectra were extracted and calibrated with SPICE, while photometric SEDs were assembled using IRAF and MOPEX. Calculated SEDs from observed fluxes were fit with simple dust models to obtain basic information on the dust presumed as the source of MIR radiation. Results. We found twelve SNe that satisfied the criterion above, observed at late-time epochs (typically after +300 days). In three cases we could not identify any point source at the SN position on late-time IRAC images. We found two SNe, 2005ad and 2005af, which likely have newly formed dust in their environment, while in the other seven cases the observed MIR flux may originate from pre-existing circumstellar or interstellar dust. Our results support the previous observational conclusions that warm new dust in the environment of SNe contributes only marginally to the cosmic dust content.

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DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Cited by 73 publications

References 95 publications

Condensation of dust in the ejecta of Type II-P supernovae

Condensation of dust in the ejecta of Type II-P supernovae

A Search for Infrared Emission From Core-Collapse Supernovae at the Transitional Phase

Twelve type II-P supernovae seen with the eyes ofSpitzer

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