The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics

Eli Dwek; Arkaprabha Sarangi; Richard G. Arendt; Timothy Kallman; Demos Kazanas; Ori D. Fox

doi:10.3847/1538-4357/ac09ea

The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics

Eli Dwek^*, Arkaprabha Sarangi, Richard G. Arendt, Timothy Kallman, Demos Kazanas, Ori D. Fox

^*Corresponding author for this work

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Research output: Contribution to journal › Journal article › Research › peer-review

6 Citations (Scopus)

Abstract

SN 2010jl is a Type IIn core-collapse supernova whose radiative output is powered by the interaction of the supernova (SN) shock wave with its surrounding dense circumstellar medium (CSM). After day similar to 60, its light curve developed a near-infrared (NIR) excess emission from dust. This excess could be a thermal IR echo from preexisting CSM dust, or emission from newly formed dust either in the cooling post-shock region of the CSM, or in the cooling SN ejecta. Recent analysis has shown that dust formation in the CSM can commence only after day similar to 380, and has also ruled out newly formed ejecta dust as the source of the NIR emission. The early (

Original language	English
Article number	84
Journal	Astrophysical Journal
Volume	917
Issue number	2
Number of pages	16
ISSN	0004-637X
DOIs	https://doi.org/10.3847/1538-4357/ac09ea
Publication status	Published - 20 Aug 2021

Keywords

INTERSTELLAR SILICATE MINERALOGY
DUST GRAINS
SUPER-NOVA
SN 2010JL
EMISSION
STEPS
PROGENITOR
EVOLUTION
SN-1987A
GAS

Access to Document

10.3847/1538-4357/ac09ea

https://arxiv.org/pdf/2106.06531.pdf

Cite this

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title = "The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics",

abstract = "SN 2010jl is a Type IIn core-collapse supernova whose radiative output is powered by the interaction of the supernova (SN) shock wave with its surrounding dense circumstellar medium (CSM). After day similar to 60, its light curve developed a near-infrared (NIR) excess emission from dust. This excess could be a thermal IR echo from preexisting CSM dust, or emission from newly formed dust either in the cooling post-shock region of the CSM, or in the cooling SN ejecta. Recent analysis has shown that dust formation in the CSM can commence only after day similar to 380, and has also ruled out newly formed ejecta dust as the source of the NIR emission. The early (",

keywords = "INTERSTELLAR SILICATE MINERALOGY, DUST GRAINS, SUPER-NOVA, SN 2010JL, EMISSION, STEPS, PROGENITOR, EVOLUTION, SN-1987A, GAS",

author = "Eli Dwek and Arkaprabha Sarangi and Arendt, {Richard G.} and Timothy Kallman and Demos Kazanas and Fox, {Ori D.}",

year = "2021",

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language = "English",

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T1 - The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics

AU - Dwek, Eli

AU - Sarangi, Arkaprabha

AU - Arendt, Richard G.

AU - Kallman, Timothy

AU - Kazanas, Demos

AU - Fox, Ori D.

PY - 2021/8/20

Y1 - 2021/8/20

N2 - SN 2010jl is a Type IIn core-collapse supernova whose radiative output is powered by the interaction of the supernova (SN) shock wave with its surrounding dense circumstellar medium (CSM). After day similar to 60, its light curve developed a near-infrared (NIR) excess emission from dust. This excess could be a thermal IR echo from preexisting CSM dust, or emission from newly formed dust either in the cooling post-shock region of the CSM, or in the cooling SN ejecta. Recent analysis has shown that dust formation in the CSM can commence only after day similar to 380, and has also ruled out newly formed ejecta dust as the source of the NIR emission. The early (

AB - SN 2010jl is a Type IIn core-collapse supernova whose radiative output is powered by the interaction of the supernova (SN) shock wave with its surrounding dense circumstellar medium (CSM). After day similar to 60, its light curve developed a near-infrared (NIR) excess emission from dust. This excess could be a thermal IR echo from preexisting CSM dust, or emission from newly formed dust either in the cooling post-shock region of the CSM, or in the cooling SN ejecta. Recent analysis has shown that dust formation in the CSM can commence only after day similar to 380, and has also ruled out newly formed ejecta dust as the source of the NIR emission. The early (

KW - INTERSTELLAR SILICATE MINERALOGY

KW - DUST GRAINS

KW - SUPER-NOVA

KW - SN 2010JL

KW - EMISSION

KW - STEPS

KW - PROGENITOR

KW - EVOLUTION

KW - SN-1987A

KW - GAS

U2 - 10.3847/1538-4357/ac09ea

DO - 10.3847/1538-4357/ac09ea

M3 - Journal article

VL - 917

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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