2016/02/15 by Katsuki Aoki, Kei-ichi Maeda, Makoto Tanabe
Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Class (philosophy) #Classical mechanics #Cosmology and Gravitation Theories #General relativity #Gravitation #Mathematical physics #Neutron star #Physics #Pulsars and Gravitational Waves Research #Star (game theory) #Stars #Theoretical physics #Theory of relativity #astro-ph.CO #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.93.064054
published as Phys. Rev. D 93, 064054 (2016) · 21 pages, 18 figures. v2: minor improvements, references added
arxiv created 2016/02/15 · openalex publication_date 2016/03/22 · arxiv updated 2016/03/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.