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...

Descripción completa

Guardado en:

Detalles Bibliográficos
Autores principales:	Velázquez, Pablo Fabián, Reynoso, Estela Marta
Publicado:	2014
Materias:	Hydrodynamics ISM: supernova remnants Methods: numerical Radiation mechanisms: thermal X-rays: ISM
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v442_n1_p229_ToledoRoy http://hdl.handle.net/20.500.12110/paper_00358711_v442_n1_p229_ToledoRoy
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00358711_v442_n1_p229_ToledoRoy
record_format	dspace
spelling	paper:paper_00358711_v442_n1_p229_ToledoRoy2023-06-08T15:01:38Z A 3D numerical model for Kepler's supernova remnant Velázquez, Pablo Fabián Reynoso, Estela Marta 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. 2014 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v442_n1_p229_ToledoRoy http://hdl.handle.net/20.500.12110/paper_00358711_v442_n1_p229_ToledoRoy
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	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 Velázquez, Pablo Fabián Reynoso, Estela Marta 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.
author	Velázquez, Pablo Fabián Reynoso, Estela Marta
author_facet	Velázquez, Pablo Fabián Reynoso, Estela Marta
author_sort	Velázquez, Pablo Fabián
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
publishDate	2014
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v442_n1_p229_ToledoRoy http://hdl.handle.net/20.500.12110/paper_00358711_v442_n1_p229_ToledoRoy
work_keys_str_mv	AT velazquezpablofabian a3dnumericalmodelforkeplerssupernovaremnant AT reynosoestelamarta a3dnumericalmodelforkeplerssupernovaremnant AT velazquezpablofabian 3dnumericalmodelforkeplerssupernovaremnant AT reynosoestelamarta 3dnumericalmodelforkeplerssupernovaremnant
_version_	1768544169261793280

A 3D numerical model for Kepler's supernova remnant

Ejemplares similares