On the mass distribution of neutron stars in HMXBs

In recent years, the number of pulsars with secure mass measurements has increased to a level that allows us to probe the underlying neutron star (NS) mass distribution in detail. We critically review the radio pulsar mass measurements. For the first time, we are able to analyze a sizable population of NSs with a flexible modeling approach that can effectively accommodate a skewed underlying distribution and asymmetric measurement errors. We find that NSs that have evolved through different evolutionary paths reflect distinctive signatures through dissimilar distribution peak and mass cutoff values. NSs in double neutron star and neutron star-white dwarf systems show consistent respective peaks at 1.33 M ⊙ and 1.55 M ⊙ suggesting significant mass accretion (∆m ≈ 0.22 M ⊙ ) has occurred during the spin-up phase. The width of the mass distribution implied by double NS systems is indicative of a tight initial mass function while the inferred mass range is significantly wider for NSs that have gone through recycling. We find a mass cutoff at ∼ 2.1 M ⊙ for NSs with white dwarf companions which establishes a firm lower bound for the maximum NS mass. This rules out the majority of strange quark and soft equation of state models as viable configurations for NS matter. The lack of truncation close to the maximum mass cutoff along with the skewed nature of the inferred mass distribution both enforce the suggestion that the 2.1 M ⊙ limit is set by evolutionary constraints rather than nuclear physics or general relativity, and the existence of rare super-massive NSs is possible.

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The Neutron Star Mass Distribution

Kızıltan

Kottas

Yoreo

et al. 2013

ApJ

383

351

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The effects of strong magnetic fields on neutron star structure: lowest order constrained variational calculations

Bordbar

Rezaei

2013

Res. Astron. Astrophys.

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We investigate the effects of strong magnetic fields upon the large-scale properties of neutron and protoneutron stars. In our calculations, the neutron star matter was approximated by pure neutron matter. Using the lowest order constrained variational approach at zero and finite temperatures, and employing AV18 potential, we present the effects of strong magnetic fields on the gravitational mass, radius, and gravitational redshift of neutron and protoneutron stars. It is found that the equation of state for a neutron star becomes stiffer with an increase of magnetic field and temperature. This leads to larger values of the maximum mass and radius for the neutron stars.

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Dense Matter in Compact Stars: Theoretical Developments and Observational Constraints

Page

Reddy

2006

Annu. Rev. Nucl. Part. Sci.

236

246

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On the mass distribution of neutron stars in HMXBs

Cited by 3 publications

References 17 publications

The Neutron Star Mass Distribution

The Neutron Star Mass Distribution

The effects of strong magnetic fields on neutron star structure: lowest order constrained variational calculations

Dense Matter in Compact Stars: Theoretical Developments and Observational Constraints

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