The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes
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Cites background from "The Masses and Spins of Neutron Sta..."
...In current GW observations, small values of χeff are preferred and χp is unconstrained, while spin measurements in X-ray binaries point to a range of spin magnitudes [246], including high spins....
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Cites background from "The Masses and Spins of Neutron Sta..."
...A majority of the masses of black holes reported herein are larger than those reported via electromagnetic observations [256–258]....
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...[256] M....
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507 citations
References
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"The Masses and Spins of Neutron Sta..." refers background in this paper
...The first of these, PSR J1614−2230 [112], is a pulsar-white dwarf system that had its Shapiro delay measured due to its fortunate nearly edge-on orientation....
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...The mass inferred for PSR J1614–2230 was M = 1.97 ± 0.04 M⊙ [112]....
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...The first of these, PSR J1614–2230 [112], is a pulsar-white dwarf system that had its Shapiro delay measured due to its fortunate nearly edge-on orientation....
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3,224 citations
"The Masses and Spins of Neutron Sta..." refers background or methods in this paper
...us on the core-collapse formation route after we lay out some basic physical scales. Basic scales.—The range of known neutron star masses is 1.25 M⊙ − 2.01 M⊙ (PSR J0737–3039B [43] and PSR J0348+0432 [44], respectively; here M⊙ = 1.989×1033 g is the mass of the Sun). Here, and throughout this review, we use “mass” to refer to the gravitational mass of the object (i.e., the mass that would be inferred ...
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...ndence that is partially degenerate with what one would find in an orbit with moderate eccentricity. The mass inferred for PSR J1614–2230 was M = 1.97 ± 0.04 M⊙ [112]. More recently, Antoniadis et al. [44] have found a mass of M = 2.01 ± 0.04 M⊙ for PSR J0348+0432. This is another pulsar-white dwarf system, but the method of mass estimation was different. In addition to the pulsar frequency modulation, ...
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...ear physics. Precise neutron star masses, which until recently were limited to the narrow 1.25 M⊙ − 1.44 M⊙ range thus far observed from double neutron star 55 systems, have now been extended to 2 M⊙ [112, 44]. This has immediate implications for the equation of state of cold supranuclear matter; in particular, it requires that this matter be relatively hard, whatever its precise composition. Truly strong ...
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2,962 citations
"The Masses and Spins of Neutron Sta..." refers methods in this paper
...A more rigorous approach to the determination of the maximummass uses the Tolman–Oppenheimer–Volkoff equation [92]...
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2,164 citations
Additional excerpts
...The circumferential radius of the ISCO is given by [53] rISCO = GM/c2 3 + Z2 ∓ [(3 − Z1)(3 + Z1 + 2Z2)] where Z1 ≡ 1 + (1 − â2)1/3 (1 + â)1/3 + (1 − â)1/3 Z2 ≡ (3â2 + Z2 1 ) 1/2....
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