Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream
The double detonation model is one of the prevalent explosion mechanisms of Type Ia supernovae (SNe Ia) wherein an outer helium shell detonation triggers a core detonation in the white dwarf (WD). The dynamically driven double degenerate double detonation (D ^6 ) is the double detonation of the more...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada034 |
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| author | Nethra Rajavel Dean M. Townsley Ken J. Shen |
| author_facet | Nethra Rajavel Dean M. Townsley Ken J. Shen |
| author_sort | Nethra Rajavel |
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| description | The double detonation model is one of the prevalent explosion mechanisms of Type Ia supernovae (SNe Ia) wherein an outer helium shell detonation triggers a core detonation in the white dwarf (WD). The dynamically driven double degenerate double detonation (D ^6 ) is the double detonation of the more massive WD in a binary WD system where the localized impact of the mass transfer stream from the companion sets off the initial helium shell detonation. To have high numerical resolution and control over the stream parameters, we have implemented a study of the local interaction of the stream with the WD surface in 2D. In cases with lower base density of the shell, the stream's impact can cause surface detonation soon after first impact. With higher base densities, after the stream hits the surface, hot material flows around the star and interacts with the incoming stream to produce a denser and narrower impact. Our results therefore show that (1) a directly impacting stream for both a relatively high resolution and for a range of stream parameters can produce a surface detonation, (2) thinner helium shells ignite more promptly via impact, doing so sooner, and (3) there are lower limits on ignition in both shell density and incoming stream speed with lower limits on density being well below those shown by other work to be required for normal appearing SN Ia. This supports stream ignition and therefore the D ^6 scenario, as a viable mechanism for normal SNe Ia. |
| format | Article |
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| institution | Kabale University |
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| spelling | doaj-art-425805cb645448cf8cf85c40393a83582025-01-17T07:07:21ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197915410.3847/1538-4357/ada034Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting StreamNethra Rajavel0https://orcid.org/0009-0003-0182-2954Dean M. Townsley1https://orcid.org/0000-0002-9538-5948Ken J. Shen2https://orcid.org/0000-0002-9632-6106Department of Physics & Astronomy, The University of Alabama , Tuscaloosa, AL, USADepartment of Physics & Astronomy, The University of Alabama , Tuscaloosa, AL, USADepartment of Astronomy and Theoretical Astrophysics Center, University of California , Berkeley, CA, USAThe double detonation model is one of the prevalent explosion mechanisms of Type Ia supernovae (SNe Ia) wherein an outer helium shell detonation triggers a core detonation in the white dwarf (WD). The dynamically driven double degenerate double detonation (D ^6 ) is the double detonation of the more massive WD in a binary WD system where the localized impact of the mass transfer stream from the companion sets off the initial helium shell detonation. To have high numerical resolution and control over the stream parameters, we have implemented a study of the local interaction of the stream with the WD surface in 2D. In cases with lower base density of the shell, the stream's impact can cause surface detonation soon after first impact. With higher base densities, after the stream hits the surface, hot material flows around the star and interacts with the incoming stream to produce a denser and narrower impact. Our results therefore show that (1) a directly impacting stream for both a relatively high resolution and for a range of stream parameters can produce a surface detonation, (2) thinner helium shells ignite more promptly via impact, doing so sooner, and (3) there are lower limits on ignition in both shell density and incoming stream speed with lower limits on density being well below those shown by other work to be required for normal appearing SN Ia. This supports stream ignition and therefore the D ^6 scenario, as a viable mechanism for normal SNe Ia.https://doi.org/10.3847/1538-4357/ada034Type Ia supernovaeWhite dwarf starsSupernova dynamics |
| spellingShingle | Nethra Rajavel Dean M. Townsley Ken J. Shen Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream The Astrophysical Journal Type Ia supernovae White dwarf stars Supernova dynamics |
| title | Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream |
| title_full | Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream |
| title_fullStr | Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream |
| title_full_unstemmed | Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream |
| title_short | Local 2D Simulations of the Ignition of a Helium Shell Detonation on a White Dwarf by an Impacting Stream |
| title_sort | local 2d simulations of the ignition of a helium shell detonation on a white dwarf by an impacting stream |
| topic | Type Ia supernovae White dwarf stars Supernova dynamics |
| url | https://doi.org/10.3847/1538-4357/ada034 |
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