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

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

Standard

The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics. / Dwek, Eli; Sarangi, Arkaprabha; Arendt, Richard G.; Kallman, Timothy; Kazanas, Demos; Fox, Ori D.

In: Astrophysical Journal, Vol. 917, No. 2, 84, 20.08.2021.

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

Harvard

Dwek, E, Sarangi, A, Arendt, RG, Kallman, T, Kazanas, D & Fox, OD 2021, 'The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics', Astrophysical Journal, vol. 917, no. 2, 84. https://doi.org/10.3847/1538-4357/ac09ea

APA

Dwek, E., Sarangi, A., Arendt, R. G., Kallman, T., Kazanas, D., & Fox, O. D. (2021). The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics. Astrophysical Journal, 917(2), [84]. https://doi.org/10.3847/1538-4357/ac09ea

Vancouver

Dwek E, Sarangi A, Arendt RG, Kallman T, Kazanas D, Fox OD. The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics. Astrophysical Journal. 2021 Aug 20;917(2). 84. https://doi.org/10.3847/1538-4357/ac09ea

Author

Dwek, Eli ; Sarangi, Arkaprabha ; Arendt, Richard G. ; Kallman, Timothy ; Kazanas, Demos ; Fox, Ori D. / The Infrared Echo of SN2010jl and Its Implications for Shock Breakout Characteristics. In: Astrophysical Journal. 2021 ; Vol. 917, No. 2.

Bibtex

@article{0b35c97bc11b4a588745a48502a4100c,
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",
month = aug,
day = "20",
doi = "10.3847/1538-4357/ac09ea",
language = "English",
volume = "917",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing, Inc",
number = "2",

}

RIS

TY - JOUR

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

IS - 2

M1 - 84

ER -

ID: 276697879