A 3D numerical model for Kepler's supernova remnant
We present new 3D numerical simulations for Kepler's supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a Type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due...
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todo:paper_00358711_v442_n1_p229_ToledoRoy2023-10-03T14:47:10Z A 3D numerical model for Kepler's supernova remnant Toledo-Roy, J.C. Esquivel, A. Velázquez, P.F. Reynoso, E.M. Hydrodynamics ISM: supernova remnants Methods: numerical Radiation mechanisms: thermal X-rays: ISM We present new 3D numerical simulations for Kepler's supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a Type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the Type Ia supernova explosion is modelled using a power-law density profile, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler's supernova remnant are well reproduced by considering an AGB mass-loss rate of 10-5 M⊙ yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm-3 and an explosion energy of 7 × 1050 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6 × 1050 erg, which is within a factor of 2 of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ∼2.4 per cent yr-1 that is consistent with the observations. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Fil:Velázquez, P.F. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Reynoso, E.M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00358711_v442_n1_p229_ToledoRoy |
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Universidad de Buenos Aires |
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I-28 |
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R-134 |
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Hydrodynamics ISM: supernova remnants Methods: numerical Radiation mechanisms: thermal X-rays: ISM |
| spellingShingle |
Hydrodynamics ISM: supernova remnants Methods: numerical Radiation mechanisms: thermal X-rays: ISM Toledo-Roy, J.C. Esquivel, A. Velázquez, P.F. Reynoso, E.M. A 3D numerical model for Kepler's supernova remnant |
| topic_facet |
Hydrodynamics ISM: supernova remnants Methods: numerical Radiation mechanisms: thermal X-rays: ISM |
| description |
We present new 3D numerical simulations for Kepler's supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a Type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the Type Ia supernova explosion is modelled using a power-law density profile, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler's supernova remnant are well reproduced by considering an AGB mass-loss rate of 10-5 M⊙ yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm-3 and an explosion energy of 7 × 1050 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6 × 1050 erg, which is within a factor of 2 of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ∼2.4 per cent yr-1 that is consistent with the observations. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. |
| format |
JOUR |
| author |
Toledo-Roy, J.C. Esquivel, A. Velázquez, P.F. Reynoso, E.M. |
| author_facet |
Toledo-Roy, J.C. Esquivel, A. Velázquez, P.F. Reynoso, E.M. |
| author_sort |
Toledo-Roy, J.C. |
| title |
A 3D numerical model for Kepler's supernova remnant |
| title_short |
A 3D numerical model for Kepler's supernova remnant |
| title_full |
A 3D numerical model for Kepler's supernova remnant |
| title_fullStr |
A 3D numerical model for Kepler's supernova remnant |
| title_full_unstemmed |
A 3D numerical model for Kepler's supernova remnant |
| title_sort |
3d numerical model for kepler's supernova remnant |
| url |
http://hdl.handle.net/20.500.12110/paper_00358711_v442_n1_p229_ToledoRoy |
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AT toledoroyjc a3dnumericalmodelforkeplerssupernovaremnant AT esquivela a3dnumericalmodelforkeplerssupernovaremnant AT velazquezpf a3dnumericalmodelforkeplerssupernovaremnant AT reynosoem a3dnumericalmodelforkeplerssupernovaremnant AT toledoroyjc 3dnumericalmodelforkeplerssupernovaremnant AT esquivela 3dnumericalmodelforkeplerssupernovaremnant AT velazquezpf 3dnumericalmodelforkeplerssupernovaremnant AT reynosoem 3dnumericalmodelforkeplerssupernovaremnant |
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1782029987005595648 |