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Spiral instability can drive thermonuclear explosions in binary white dwarf mergers
kashyap, Rahul; Fisher, Robert T.; García-Berro Montilla, Enrique; Aznar Siguan, Gabriela; Ji, Suoqing; Lorén Aguilar, Pablo
Universitat Politècnica de Catalunya. Departament de Física Aplicada; Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica; Universitat Politècnica de Catalunya. CTE-CRAE - Grup de Recerca en Ciències i Tecnologies de l'Espai
Thermonuclear, or Type Ia supernovae (SNe Ia), originate from the explosion of carbon-oxygen white dwarfs, and serve as standardizable cosmological candles. However, despite their importance, the nature of the progenitor systems that give rise to SNe Ia has not been hitherto elucidated. Observational evidence favors the double-degenerate channel in which merging white dwarf binaries lead to SNe Ia. Furthermore, significant discrepancies exist between observations and theory, and to date, there has been no self-consistent merger model that yields a SNe Ia. Here we show that a spiral mode instability in the accretion disk formed during a binary white dwarf merger leads to a detonation on a dynamical timescale. This mechanism sheds light on how white dwarf mergers may frequently yield SNe Ia.
Peer Reviewed
Àrees temàtiques de la UPC::Física::Astronomia i astrofísica
Hydrodyanamics
White dwarf stars
Supernovae
hydrodynamics
supernovae: general
white dwarfs
ECCENTRIC GRAVITATIONAL INSTABILITIES
IA SUPERNOVAE
COLLISIONS
DETONATIONS
SIMULATIONS
PROGENITORS
EVOLUTION
REMNANTS
DISKS
END
Estels nans
Supernoves
Attribution-NonCommercial-NoDerivs 3.0 Spain
http://creativecommons.org/licenses/by-nc-nd/3.0/es/
info:eu-repo/semantics/publishedVersion
Artículo
         

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