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Title: GAMMA-RAY EMISSION OF ACCELERATED PARTICLES ESCAPING A SUPERNOVA REMNANT IN A MOLECULAR CLOUD

Abstract

We present a model of gamma-ray emission from core-collapse supernovae (SNe) originating from the explosions of massive young stars. The fast forward shock of the supernova remnant (SNR) can accelerate particles by diffusive shock acceleration (DSA) in a cavern blown by a strong, pre-SN stellar wind. As a fundamental part of nonlinear DSA, some fraction of the accelerated particles escape the shock and interact with a surrounding massive dense shell producing hard photon emission. To calculate this emission, we have developed a new Monte Carlo technique for propagating the cosmic rays (CRs) produced by the forward shock of the SNR, into the dense, external material. This technique is incorporated in a hydrodynamic model of an evolving SNR which includes the nonlinear feedback of CRs on the SNR evolution, the production of escaping CRs along with those that remain trapped within the remnant, and the broadband emission of radiation from trapped and escaping CRs. While our combined CR-hydro-escape model is quite general and applies to both core collapse and thermonuclear SNe, the parameters we choose for our discussion here are more typical of SNRs from very massive stars whose emission spectra differ somewhat from those produced by lower mass progenitors directlymore » interacting with a molecular cloud.« less

Authors:
 [1]
  1. Physics Department, North Carolina State University, Box 8202, Raleigh, NC 27695 (United States)
Publication Date:
OSTI Identifier:
21574721
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 731; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/731/2/87; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATION; CLOUDS; COSMIC RADIATION; GAMMA RADIATION; HYDRODYNAMIC MODEL; MONTE CARLO METHOD; PARTICLES; PHOTON EMISSION; SHOCK WAVES; STELLAR WINDS; SUPERNOVA REMNANTS; SUPERNOVAE; BINARY STARS; CALCULATION METHODS; COSMIC RADIO SOURCES; ELECTROMAGNETIC RADIATION; EMISSION; ERUPTIVE VARIABLE STARS; IONIZING RADIATIONS; MATHEMATICAL MODELS; PARTICLE MODELS; RADIATIONS; STARS; STATISTICAL MODELS; STELLAR ACTIVITY; THERMODYNAMIC MODEL; VARIABLE STARS

Citation Formats

Ellison, Donald C, and Bykov, Andrei M., E-mail: don_ellison@ncsu.edu, E-mail: byk@astro.ioffe.ru. GAMMA-RAY EMISSION OF ACCELERATED PARTICLES ESCAPING A SUPERNOVA REMNANT IN A MOLECULAR CLOUD. United States: N. p., 2011. Web. doi:10.1088/0004-637X/731/2/87.
Ellison, Donald C, & Bykov, Andrei M., E-mail: don_ellison@ncsu.edu, E-mail: byk@astro.ioffe.ru. GAMMA-RAY EMISSION OF ACCELERATED PARTICLES ESCAPING A SUPERNOVA REMNANT IN A MOLECULAR CLOUD. United States. https://doi.org/10.1088/0004-637X/731/2/87
Ellison, Donald C, and Bykov, Andrei M., E-mail: don_ellison@ncsu.edu, E-mail: byk@astro.ioffe.ru. 2011. "GAMMA-RAY EMISSION OF ACCELERATED PARTICLES ESCAPING A SUPERNOVA REMNANT IN A MOLECULAR CLOUD". United States. https://doi.org/10.1088/0004-637X/731/2/87.
@article{osti_21574721,
title = {GAMMA-RAY EMISSION OF ACCELERATED PARTICLES ESCAPING A SUPERNOVA REMNANT IN A MOLECULAR CLOUD},
author = {Ellison, Donald C and Bykov, Andrei M., E-mail: don_ellison@ncsu.edu, E-mail: byk@astro.ioffe.ru},
abstractNote = {We present a model of gamma-ray emission from core-collapse supernovae (SNe) originating from the explosions of massive young stars. The fast forward shock of the supernova remnant (SNR) can accelerate particles by diffusive shock acceleration (DSA) in a cavern blown by a strong, pre-SN stellar wind. As a fundamental part of nonlinear DSA, some fraction of the accelerated particles escape the shock and interact with a surrounding massive dense shell producing hard photon emission. To calculate this emission, we have developed a new Monte Carlo technique for propagating the cosmic rays (CRs) produced by the forward shock of the SNR, into the dense, external material. This technique is incorporated in a hydrodynamic model of an evolving SNR which includes the nonlinear feedback of CRs on the SNR evolution, the production of escaping CRs along with those that remain trapped within the remnant, and the broadband emission of radiation from trapped and escaping CRs. While our combined CR-hydro-escape model is quite general and applies to both core collapse and thermonuclear SNe, the parameters we choose for our discussion here are more typical of SNRs from very massive stars whose emission spectra differ somewhat from those produced by lower mass progenitors directly interacting with a molecular cloud.},
doi = {10.1088/0004-637X/731/2/87},
url = {https://www.osti.gov/biblio/21574721}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 731,
place = {United States},
year = {Wed Apr 20 00:00:00 EDT 2011},
month = {Wed Apr 20 00:00:00 EDT 2011}
}