MG14 - Talk detail |
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Participant |
Suwa, Yudai | |||||||
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Institution |
Max Planck Institute for Astrophysics - Karl-Schwarzschild-Str. 1 - Garching - Bayern - Germany | |||||||
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Session |
BN3 |
Accepted |
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Talk |
Oral abstract |
Title |
Neutrino-driven explosions of ultra-stripped type Ic supernovae generating binary neutron stars | |||||
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Abstract |
Binary compact mergers are promising candidates of strong gravitational wave (GW) emitters. Close binary systems are in particular payed attention since their merger times are shorter than cosmic age and strong GW emission just prior to the merger might be detected within a couple of years by advanced GW detecters. These close binary systems are considered to have experienced strong binary interactions, e.g. common envelope phase and explosions of secondary stars after such binary interactions may be different from canonical supernovae (SNe). Possible candidates of such SNe are ultra-stripped SNe, which imply considerably small amount of ejecta mass that leads to fast-evolving light curves. In this study, the explosion characteristics of ultra-stripped SNe are investigated. We perform stellar evolutionary simulations of bare carbon-oxygen cores until the iron cores become unstable and collapse. We also perform axisymmetric hydrodynamic simulations with spectral neutrino transport initiated from these iron cores. All models exhibit successful explosions driven by neutrino heating. The diagnostic explosion energy, ejecta mass, Ni mass, and neutron star mass are typically ~10^50 erg, ~0.1 M_sun, ~0.01M_sun, and ~ 1.3M_sun, which are compatible with observations of ultra-stripped SNe, e.g. SN 2005ek. |
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Pdf file |
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Session |
NS5 |
Accepted |
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Time |
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Oral abstract |
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On 56Ni synthesis by the magnetar model for long gamma-ray bursts and hypernovae | |||||
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Abstract |
A rapidly rotating neutron star with strong magnetic fields, called a magnetar, is a possible candidate for the central engine of long gamma-ray bursts and hypernovae (HNe). We solve the evolution of a shock wave driven by the wind from a magnetar and we evaluate the temperature evolution, by which we estimate the amount of 56Ni that produces the bright emission of HNe. We obtain a constraint on the magnetar parameters (i.e. the poloidal magnetic field strength Bp and initial angular velocity Omega_i) for synthesizing enough 56Ni mass to explain HNe. |
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Pdf file |
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