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Simulated X-ray emission for a runaway model of Kepler's supernova remnant

Velazquez, Pablo F. ; Vigh, Carlos D. ; Reynoso, Estela M. ; Gomez, Daniel O. and Schneiter, E. Matias LU (2006) In Astrophysical Journal 649(2). p.779-787
Abstract
We present two-dimensional numerical simulations of a model for Kepler's supernova remnant (SNR) carried out with the YGUAZU-A code. Following previous studies, we have assumed that the peculiar shape of this young remnant arises as a consequence of the interaction of the SNR blast wave with the bow shock formed by the wind of its high velocity progenitor. Furthermore, from our numerical results we have obtained synthetic X-ray emission maps, which can be directly compared with recent and previous observations of this SNR. Our models show that a nice fit with respect to the X-ray morphology and luminosity is obtained for a SN progenitor with mass-loss rate of 5 x 10(-5) M-circle dot yr(-1), an ambient medium density of 10(-2) cm(-3), an... (More)
We present two-dimensional numerical simulations of a model for Kepler's supernova remnant (SNR) carried out with the YGUAZU-A code. Following previous studies, we have assumed that the peculiar shape of this young remnant arises as a consequence of the interaction of the SNR blast wave with the bow shock formed by the wind of its high velocity progenitor. Furthermore, from our numerical results we have obtained synthetic X-ray emission maps, which can be directly compared with recent and previous observations of this SNR. Our models show that a nice fit with respect to the X-ray morphology and luminosity is obtained for a SN progenitor with mass-loss rate of 5 x 10(-5) M-circle dot yr(-1), an ambient medium density of 10(-2) cm(-3), an initial explosion energy of 8 x 10(50) ergs, and a total ejected mass within 1.4-2.5 M-circle dot. In our simulations, parameters typical of a young population progenitor have not been considered. This model also predicts a similar to 0.3% yearly decrease in the total X-ray luminosity, which is consistent with observed values. The parameters employed in our runs correspond to a Type Ia supernova. Based on our simulations, we find that the expansion rate increases after the SNR blast wave overruns the bow shock, and we discuss whether this can explain the observed difference between the expansion rates measured from sequences of radio and X-ray images. (Less)
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author
; ; ; and
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
X-rays : ISM, supernova remnants, methods : numerical, ISM : individual (Kepler SNR), shock waves, hydrodynamics
in
Astrophysical Journal
volume
649
issue
2
pages
779 - 787
publisher
American Astronomical Society
external identifiers
  • wos:000240854200019
  • scopus:34547306118
ISSN
0004-637X
language
English
LU publication?
yes
id
1441cde8-be55-4325-990a-46fbd6de23e0 (old id 389783)
alternative location
http://www.journals.uchicago.edu/ApJ/journal/issues/ApJ/v649n2/64600/brief/64600.abstract.html
date added to LUP
2016-04-01 15:42:36
date last changed
2021-10-06 03:31:57
@article{1441cde8-be55-4325-990a-46fbd6de23e0,
  abstract     = {We present two-dimensional numerical simulations of a model for Kepler's supernova remnant (SNR) carried out with the YGUAZU-A code. Following previous studies, we have assumed that the peculiar shape of this young remnant arises as a consequence of the interaction of the SNR blast wave with the bow shock formed by the wind of its high velocity progenitor. Furthermore, from our numerical results we have obtained synthetic X-ray emission maps, which can be directly compared with recent and previous observations of this SNR. Our models show that a nice fit with respect to the X-ray morphology and luminosity is obtained for a SN progenitor with mass-loss rate of 5 x 10(-5) M-circle dot yr(-1), an ambient medium density of 10(-2) cm(-3), an initial explosion energy of 8 x 10(50) ergs, and a total ejected mass within 1.4-2.5 M-circle dot. In our simulations, parameters typical of a young population progenitor have not been considered. This model also predicts a similar to 0.3% yearly decrease in the total X-ray luminosity, which is consistent with observed values. The parameters employed in our runs correspond to a Type Ia supernova. Based on our simulations, we find that the expansion rate increases after the SNR blast wave overruns the bow shock, and we discuss whether this can explain the observed difference between the expansion rates measured from sequences of radio and X-ray images.},
  author       = {Velazquez, Pablo F. and Vigh, Carlos D. and Reynoso, Estela M. and Gomez, Daniel O. and Schneiter, E. Matias},
  issn         = {0004-637X},
  language     = {eng},
  number       = {2},
  pages        = {779--787},
  publisher    = {American Astronomical Society},
  series       = {Astrophysical Journal},
  title        = {Simulated X-ray emission for a runaway model of Kepler's supernova remnant},
  url          = {http://www.journals.uchicago.edu/ApJ/journal/issues/ApJ/v649n2/64600/brief/64600.abstract.html},
  volume       = {649},
  year         = {2006},
}