Gravitational wave emission during the transition to strange stars

Nobutoshi Yasutake, Masa Aki Hashimoto, Kei Kotake, Shoichi Yamada

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

    Abstract

    We present a series of axisymmetric, magneto-hydrodynamical simulations for the rotational core collapse of a massive star accompanying the QCD phase transition. To elucidate the implications of a phase transition against a supernova, we investigate the waveforms of gravitational wave derived from the quadrupole formula that includes the contributions from the electromagnetic fields. We adopt a phenomenological equation of state above the nuclear matter density ρ 0 that includes two parameters to change the hardness of the matter before the transition. We assume that the first order phase transition is the conversion of bulk nuclear matter to a chirally symmetric quark-gluon phase described by the MIT bag model. In most models with the phase transition, the first peak amplitudes are higher by a few percents to nearly ten percents than those without the transition. However, it is found that under the condition of the very strong differential rotation, the height of the peak becomes lower by several percents if the phase transition is included. In the paper, we show the typical models of our calculations.

    Original languageEnglish
    Title of host publicationProceedings of Science
    Publication statusPublished - 2006
    Event9th International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos, NIC 2006 - Geneva, Switzerland
    Duration: 2006 Jun 252006 Jun 30

    Other

    Other9th International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos, NIC 2006
    CountrySwitzerland
    CityGeneva
    Period06/6/2506/6/30

    Fingerprint

    gravitational waves
    stars
    bags
    massive stars
    supernovae
    waveforms
    electromagnetic fields
    equations of state
    hardness
    quantum chromodynamics
    quadrupoles
    quarks
    simulation

    ASJC Scopus subject areas

    • General

    Cite this

    Yasutake, N., Hashimoto, M. A., Kotake, K., & Yamada, S. (2006). Gravitational wave emission during the transition to strange stars. In Proceedings of Science

    Gravitational wave emission during the transition to strange stars. / Yasutake, Nobutoshi; Hashimoto, Masa Aki; Kotake, Kei; Yamada, Shoichi.

    Proceedings of Science. 2006.

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

    Yasutake, N, Hashimoto, MA, Kotake, K & Yamada, S 2006, Gravitational wave emission during the transition to strange stars. in Proceedings of Science. 9th International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos, NIC 2006, Geneva, Switzerland, 06/6/25.
    Yasutake N, Hashimoto MA, Kotake K, Yamada S. Gravitational wave emission during the transition to strange stars. In Proceedings of Science. 2006
    Yasutake, Nobutoshi ; Hashimoto, Masa Aki ; Kotake, Kei ; Yamada, Shoichi. / Gravitational wave emission during the transition to strange stars. Proceedings of Science. 2006.
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    abstract = "We present a series of axisymmetric, magneto-hydrodynamical simulations for the rotational core collapse of a massive star accompanying the QCD phase transition. To elucidate the implications of a phase transition against a supernova, we investigate the waveforms of gravitational wave derived from the quadrupole formula that includes the contributions from the electromagnetic fields. We adopt a phenomenological equation of state above the nuclear matter density ρ 0 that includes two parameters to change the hardness of the matter before the transition. We assume that the first order phase transition is the conversion of bulk nuclear matter to a chirally symmetric quark-gluon phase described by the MIT bag model. In most models with the phase transition, the first peak amplitudes are higher by a few percents to nearly ten percents than those without the transition. However, it is found that under the condition of the very strong differential rotation, the height of the peak becomes lower by several percents if the phase transition is included. In the paper, we show the typical models of our calculations.",
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