Asymmetries in the expansion and emission from young supernova remnants

We present two-dimensional and three-dimensional numerical simulations of asymmetric young supernova remnants (SNRs) carried out with the hydrodynamical code Yguazú, aiming to quantitatively assess the role of different factors that may give origin to such asymmetries in their expansion. In particul...

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Detalles Bibliográficos
Publicado: 2011
Materias:
Hydrodynamics
ISM: supernova remnants
Methods: numerical
Shock waves
Supernovae: individual (Tycho)
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v727_n1_p_Vigh
http://hdl.handle.net/20.500.12110/paper_0004637X_v727_n1_p_Vigh
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v727_n1_p_Vigh
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spelling paper:paper_0004637X_v727_n1_p_Vigh2023-06-08T14:29:00Z Asymmetries in the expansion and emission from young supernova remnants Hydrodynamics ISM: supernova remnants Methods: numerical Shock waves Supernovae: individual (Tycho) We present two-dimensional and three-dimensional numerical simulations of asymmetric young supernova remnants (SNRs) carried out with the hydrodynamical code Yguazú, aiming to quantitatively assess the role of different factors that may give origin to such asymmetries in their expansion. In particular, we are interested in modeling the morphology of Tycho's SNR to address whether the companion star of a Type Ia supernova progenitor has played a role in the subsequent evolution of the remnant.With the results from the numerical simulations, we can not only study the morphology of the SNR but also compute the emission of the remnant in different spectral bands. In particular, we simulate X-ray maps, which can be directly compared to recent and previous observations of Tycho's SNR. Our results suggest that the most likely explanation for Tycho's morphology is that after the supernova (SN) explosion the shock front stripped the envelope of its companion. We represent this effect by adding a conical region with an enhanced density into the initial sphere immediately after the explosion. Assuming that Tycho's companion was a massive red giant star, we explore different values of the angle of aperture and mass excess of the conical region. A good agreement with observational data was found for the model with a mass excess of 0.3 M and an aperture of 90°. After the collision with the SN shock wave, the companion would become an He-rich star. This scenario would gain observational support if a star with these characteristics is found in the vicinity of the center of the SN explosion. © 2011 The American Astronomical Society. All rights reserved. 2011 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v727_n1_p_Vigh http://hdl.handle.net/20.500.12110/paper_0004637X_v727_n1_p_Vigh
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
Shock waves
Supernovae: individual (Tycho)
spellingShingle Hydrodynamics
ISM: supernova remnants
Methods: numerical
Shock waves
Supernovae: individual (Tycho)
Asymmetries in the expansion and emission from young supernova remnants
topic_facet Hydrodynamics
ISM: supernova remnants
Methods: numerical
Shock waves
Supernovae: individual (Tycho)
description We present two-dimensional and three-dimensional numerical simulations of asymmetric young supernova remnants (SNRs) carried out with the hydrodynamical code Yguazú, aiming to quantitatively assess the role of different factors that may give origin to such asymmetries in their expansion. In particular, we are interested in modeling the morphology of Tycho's SNR to address whether the companion star of a Type Ia supernova progenitor has played a role in the subsequent evolution of the remnant.With the results from the numerical simulations, we can not only study the morphology of the SNR but also compute the emission of the remnant in different spectral bands. In particular, we simulate X-ray maps, which can be directly compared to recent and previous observations of Tycho's SNR. Our results suggest that the most likely explanation for Tycho's morphology is that after the supernova (SN) explosion the shock front stripped the envelope of its companion. We represent this effect by adding a conical region with an enhanced density into the initial sphere immediately after the explosion. Assuming that Tycho's companion was a massive red giant star, we explore different values of the angle of aperture and mass excess of the conical region. A good agreement with observational data was found for the model with a mass excess of 0.3 M and an aperture of 90°. After the collision with the SN shock wave, the companion would become an He-rich star. This scenario would gain observational support if a star with these characteristics is found in the vicinity of the center of the SN explosion. © 2011 The American Astronomical Society. All rights reserved.
title Asymmetries in the expansion and emission from young supernova remnants
title_short Asymmetries in the expansion and emission from young supernova remnants
title_full Asymmetries in the expansion and emission from young supernova remnants
title_fullStr Asymmetries in the expansion and emission from young supernova remnants
title_full_unstemmed Asymmetries in the expansion and emission from young supernova remnants
title_sort asymmetries in the expansion and emission from young supernova remnants
publishDate 2011
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v727_n1_p_Vigh
http://hdl.handle.net/20.500.12110/paper_0004637X_v727_n1_p_Vigh
_version_ 1768541637542150144

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