Relation between gravitational mass and baryonic mass for non-rotating and rapidly rotating neutron stars

doi:10.1007/s11467-019-0945-9

Front. Phys.

2020, Vol. 15

Issue (2) : 24603 https://doi.org/10.1007/s11467-019-0945-9

RESEARCH ARTICLE

Relation between gravitational mass and baryonic mass for non-rotating and rapidly rotating neutron stars

He Gao¹(

), Shun-Ke Ai^2,¹, Zhou-Jian Cao¹, Bing Zhang², Zhen-Yu Zhu^3,⁴, Ang Li³, Nai-Bo Zhang⁵, Andreas Bauswein⁶

¹. Department of Astronomy, Beijing Normal University, Beijing 100875, China
². Department of Physics and Astronomy, University of Nevada Las Vegas, NV 89154, USA
³. Department of Astronomy, Xiamen University, Xiamen 361005, China
⁴. Institute for Theoretical Physics, Max-von-Laue-Strasse 1, 60438 Frankfurt, Germany
⁵. Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, Weihai 264209, China
⁶. GSI Helmholtzzentrum für Schwerionenforschung, Planckstraβe 1, 64291 Darmstadt, Germany

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Abstract

With a selected sample of neutron star (NS) equations of state (EOSs) that are consistent with the current observations and have a range of maximum masses, we investigate the relations between NS gravitational mass M_g and baryonic mass M_b, and the relations between the maximum NS mass supported through uniform rotation (M_max) and that of nonrotating NSs (M_TOV). We find that for an EOS-independent quadratic, universal transformation formula ( $M b = M g + A × M g 2$ ), the best-fit A value is 0.080 for non-rotating NSs, 0.064 for maximally rotating NSs, and 0.073 when NSs with arbitrary rotation are considered. The residual error of the transformation is ~0.1M_⊙ for non-spin or maximum-spin, but is as large as ~0.2M_⊙ for all spins. For different EOSs, we find that the parameter A for non-rotating NSs is proportional to $R 1.4 − 1$ (where R_1.4 is NS radius for 1.4M_⊙ in units of km). For a particular EOS, if one adopts the best-fit parameters for different spin periods, the residual error of the transformation is smaller, which is of the order of 0.01 M_⊙ for the quadratic form and less than 0.01M⊙ for the cubic form ( $M b = M g + A 1 × M g 2 + A 2 × M g 3$ ). We also find a very tight and general correlation between the normalized mass gain due to spin $Δ m ≡ (M max ⁡ − M T O V) / M T O V$ and the spin period normalized to the Keplerian period $P$ , i.e., $log ⁡ 10 Δ m = (− 2.74 ± 0.05) log ⁡ 10 P + log ⁡ 10 (0.20 ± 0.01)$ , which is independent of EOS models. These empirical relations are helpful to study NS-NS mergers with a long-lived NS merger product using multi-messenger data. The application of our results to GW170817 is discussed.

Keywords gravitational waves

Corresponding Author(s): He Gao

Issue Date: 08 January 2020

Cite this article:

He Gao,Shun-Ke Ai,Zhou-Jian Cao, et al. Relation between gravitational mass and baryonic mass for non-rotating and rapidly rotating neutron stars[J]. Front. Phys. , 2020, 15(2): 24603.

URL:

https://academic.hep.com.cn/fop/EN/10.1007/s11467-019-0945-9
https://academic.hep.com.cn/fop/EN/Y2020/V15/I2/24603

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