Special relativistic simulations of magneto-driven jet from core-collapse supernovae

Tomoya Takiwaki, Kei Kotake, Shoichi Yamada, Katsuhiko Sato

    Research output: Chapter in Book/Report/Conference proceedingConference contribution

    Abstract

    We performed 2.5 dimensional numerical simulations of magnetized rotational core-collapse. From the observational fact, it is probable that gamma-ray bursts and core-collapse supernovae have same origin. And the very collimated jet is preferable to explain the light curve of their afterglow. How this collimated jet is produced due to the process of core-collapse of massive star? There are two main energy-sources for this explosion. One is neutrino pair annihilations and another is magneto-hydrodynamical process. In this time we concentrate the magneto-hydrodynamical process. We found a jet-like shock wave is launched in the direction of the pole. The strength of initial magnetic field determine the profile of jet. We found common structures of these jets. We continue the simulation that the jet-like shock wave produced at the center propagate to the surface of the star. Since the previous works are performed separately at each stage such as core-collapse and jet-propagation, many initial uncertainty remains in each stage. However we have performed the simulations from the magnetized core-collapse to the jet-propagation totally. This study gives us deeper knowledge on the relation between the profile of the jet and the progenitor.

    Original languageEnglish
    Title of host publication11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity
    Pages1971-1973
    Number of pages3
    Publication statusPublished - 2008
    Event11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006 - Berlin
    Duration: 2006 Jul 232006 Jul 29

    Other

    Other11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006
    CityBerlin
    Period06/7/2306/7/29

    Fingerprint

    supernovae
    simulation
    shock waves
    propagation
    energy sources
    profiles
    afterglows
    massive stars
    gamma ray bursts
    light curve
    explosions
    poles
    neutrinos
    stars
    magnetic fields

    ASJC Scopus subject areas

    • Nuclear and High Energy Physics

    Cite this

    Takiwaki, T., Kotake, K., Yamada, S., & Sato, K. (2008). Special relativistic simulations of magneto-driven jet from core-collapse supernovae. In 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity (pp. 1971-1973)

    Special relativistic simulations of magneto-driven jet from core-collapse supernovae. / Takiwaki, Tomoya; Kotake, Kei; Yamada, Shoichi; Sato, Katsuhiko.

    11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. 2008. p. 1971-1973.

    Research output: Chapter in Book/Report/Conference proceedingConference contribution

    Takiwaki, T, Kotake, K, Yamada, S & Sato, K 2008, Special relativistic simulations of magneto-driven jet from core-collapse supernovae. in 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. pp. 1971-1973, 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006, Berlin, 06/7/23.
    Takiwaki T, Kotake K, Yamada S, Sato K. Special relativistic simulations of magneto-driven jet from core-collapse supernovae. In 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. 2008. p. 1971-1973
    Takiwaki, Tomoya ; Kotake, Kei ; Yamada, Shoichi ; Sato, Katsuhiko. / Special relativistic simulations of magneto-driven jet from core-collapse supernovae. 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. 2008. pp. 1971-1973
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    abstract = "We performed 2.5 dimensional numerical simulations of magnetized rotational core-collapse. From the observational fact, it is probable that gamma-ray bursts and core-collapse supernovae have same origin. And the very collimated jet is preferable to explain the light curve of their afterglow. How this collimated jet is produced due to the process of core-collapse of massive star? There are two main energy-sources for this explosion. One is neutrino pair annihilations and another is magneto-hydrodynamical process. In this time we concentrate the magneto-hydrodynamical process. We found a jet-like shock wave is launched in the direction of the pole. The strength of initial magnetic field determine the profile of jet. We found common structures of these jets. We continue the simulation that the jet-like shock wave produced at the center propagate to the surface of the star. Since the previous works are performed separately at each stage such as core-collapse and jet-propagation, many initial uncertainty remains in each stage. However we have performed the simulations from the magnetized core-collapse to the jet-propagation totally. This study gives us deeper knowledge on the relation between the profile of the jet and the progenitor.",
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    AB - We performed 2.5 dimensional numerical simulations of magnetized rotational core-collapse. From the observational fact, it is probable that gamma-ray bursts and core-collapse supernovae have same origin. And the very collimated jet is preferable to explain the light curve of their afterglow. How this collimated jet is produced due to the process of core-collapse of massive star? There are two main energy-sources for this explosion. One is neutrino pair annihilations and another is magneto-hydrodynamical process. In this time we concentrate the magneto-hydrodynamical process. We found a jet-like shock wave is launched in the direction of the pole. The strength of initial magnetic field determine the profile of jet. We found common structures of these jets. We continue the simulation that the jet-like shock wave produced at the center propagate to the surface of the star. Since the previous works are performed separately at each stage such as core-collapse and jet-propagation, many initial uncertainty remains in each stage. However we have performed the simulations from the magnetized core-collapse to the jet-propagation totally. This study gives us deeper knowledge on the relation between the profile of the jet and the progenitor.

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