Relativistic stars in bigravity theory

Katsuki Aoki, Keiichi Maeda, Makoto Tanabe

    Research output: Contribution to journalArticle

    6 Citations (Scopus)

    Abstract

    Assuming static and spherically symmetric spacetimes in the ghost-free bigravity theory, we find a relativistic star solution, which is very close to that in general relativity. The coupling constants are classified into two classes: Class [I] and Class [II]. Although the Vainshtein screening mechanism is found in the weak gravitational field for both classes, we find that there is no regular solution beyond the critical value of the compactness in Class [I]. This implies that the maximum mass of a neutron star in Class [I] becomes much smaller than that in general relativity (GR). On the other hand, for the solution in Class [II], the Vainshtein screening mechanism works well even in a relativistic star and the result in GR is recovered.

    Original languageEnglish
    Article number064054
    JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
    Volume93
    Issue number6
    DOIs
    Publication statusPublished - 2016 Mar 22

    Fingerprint

    stars
    relativity
    screening
    void ratio
    ghosts
    gravitational fields
    neutron stars

    ASJC Scopus subject areas

    • Nuclear and High Energy Physics

    Cite this

    Relativistic stars in bigravity theory. / Aoki, Katsuki; Maeda, Keiichi; Tanabe, Makoto.

    In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 93, No. 6, 064054, 22.03.2016.

    Research output: Contribution to journalArticle

    @article{a83d9b9f0bee44959fef12407453afc7,
    title = "Relativistic stars in bigravity theory",
    abstract = "Assuming static and spherically symmetric spacetimes in the ghost-free bigravity theory, we find a relativistic star solution, which is very close to that in general relativity. The coupling constants are classified into two classes: Class [I] and Class [II]. Although the Vainshtein screening mechanism is found in the weak gravitational field for both classes, we find that there is no regular solution beyond the critical value of the compactness in Class [I]. This implies that the maximum mass of a neutron star in Class [I] becomes much smaller than that in general relativity (GR). On the other hand, for the solution in Class [II], the Vainshtein screening mechanism works well even in a relativistic star and the result in GR is recovered.",
    author = "Katsuki Aoki and Keiichi Maeda and Makoto Tanabe",
    year = "2016",
    month = "3",
    day = "22",
    doi = "10.1103/PhysRevD.93.064054",
    language = "English",
    volume = "93",
    journal = "Physical review D: Particles and fields",
    issn = "0556-2821",
    publisher = "American Institute of Physics Publising LLC",
    number = "6",

    }

    TY - JOUR

    T1 - Relativistic stars in bigravity theory

    AU - Aoki, Katsuki

    AU - Maeda, Keiichi

    AU - Tanabe, Makoto

    PY - 2016/3/22

    Y1 - 2016/3/22

    N2 - Assuming static and spherically symmetric spacetimes in the ghost-free bigravity theory, we find a relativistic star solution, which is very close to that in general relativity. The coupling constants are classified into two classes: Class [I] and Class [II]. Although the Vainshtein screening mechanism is found in the weak gravitational field for both classes, we find that there is no regular solution beyond the critical value of the compactness in Class [I]. This implies that the maximum mass of a neutron star in Class [I] becomes much smaller than that in general relativity (GR). On the other hand, for the solution in Class [II], the Vainshtein screening mechanism works well even in a relativistic star and the result in GR is recovered.

    AB - Assuming static and spherically symmetric spacetimes in the ghost-free bigravity theory, we find a relativistic star solution, which is very close to that in general relativity. The coupling constants are classified into two classes: Class [I] and Class [II]. Although the Vainshtein screening mechanism is found in the weak gravitational field for both classes, we find that there is no regular solution beyond the critical value of the compactness in Class [I]. This implies that the maximum mass of a neutron star in Class [I] becomes much smaller than that in general relativity (GR). On the other hand, for the solution in Class [II], the Vainshtein screening mechanism works well even in a relativistic star and the result in GR is recovered.

    UR - http://www.scopus.com/inward/record.url?scp=84962638401&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84962638401&partnerID=8YFLogxK

    U2 - 10.1103/PhysRevD.93.064054

    DO - 10.1103/PhysRevD.93.064054

    M3 - Article

    VL - 93

    JO - Physical review D: Particles and fields

    JF - Physical review D: Particles and fields

    SN - 0556-2821

    IS - 6

    M1 - 064054

    ER -