Revisiting the maximum mass of differentially rotating neutron stars in general relativity with realistic equations of state

Espino, Pedro; Paschalidis, Vasileios

doi:10.1103/physrevd.99.083017

Cited by 22 publications

(28 citation statements)

References 82 publications

(180 reference statements)

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“…In Figure 10 we show the maximum rest mass normalized to the rest-mass of the TOV limit as a function of A −1 . The behavior is similar to that seen for polytropes [74] and hadronic EOSs [70] and it is followed very closely by the gravitational mass: at relatively low values ofÂ −1 ( 0.25), corresponding to rotational profiles closer to uniform rotation, there are only modest increases in the rest mass, not exceeding 40 %. For higher values ofÂ −1 , the increase of M 0,Max compared to the TOV limit grows until it reaches a maximum and then begins to decrease again aŝ A −1 is increased further.…”

Section: Maximum Masssupporting

confidence: 72%

“…Hence, as in [70], we esti-mateÂ −1 crit with the maximum of the functionÂ −1 min (r p /r e ), whereÂ −1 min is the smallest degree of differential rotation for which an equilibrium model exists with the given maximum energy density. This method allows the calculation ofÂ −1 crit to within 1 % accuracy [70]. Figure 14 shows the critical degree of differential rotation as a function of the maximum energy density for all the hybrid EOSs we consider in this work.…”

Section: A Appendix: Solution Space Of Differentially Rotating Starsmentioning

confidence: 99%

“…The term "hypermassive" [69] is used to describe those stars that are more massive than the supramassive limit, and are supported by the additional centrifugal support provided by differential rotation. There also exist stars that can support more than two times the TOV limit mass (these were termed "ubermassive" in [70]), and which can arise only when differential rotation is present. Differential rotation plays an important role in temporarily stabilizing a binary neutron star merger remnant, and likely many merger remnants go trough a hypermassive phase (see, e.g., [60,71,72] for recent reviews on binary neutron star mergers).…”

Section: Introductionmentioning

confidence: 99%

“…Differential rotation plays an important role in temporarily stabilizing a binary neutron star merger remnant, and likely many merger remnants go trough a hypermassive phase (see, e.g., [60,71,72] for recent reviews on binary neutron star mergers). Differentially rotating stars have been shown to exhibit a rich and interesting solution space (see [73][74][75] for polytropes, [70] for hadronic EOSs, and [76,77] for strange quark stars). For instance, as the degree of differential rotation varies, the topology of the star can change from spheroidal to quasi-toroidal, where the maximum energy density does not occur at the geometric center of the star, but in a ring around the stellar center of mass.…”

Section: Introductionmentioning

confidence: 99%

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Maximum mass and universal relations of rotating relativistic hybrid hadron-quark stars

et al. 2019

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We construct equilibrium models of uniformly and differentially rotating hybrid hadron-quark stars using equations of state (EOSs) with a first-order phase transition that gives rise to a third family of compact objects. We find that the ratio of the maximum possible mass of uniformly rotating configurationsthe supramassive limit -to the Tolman-Oppenheimer-Volkoff (TOV) limit mass is not EOS-independent, and is between 1.15 and 1.31, in contrast with the value of 1.20 previously found for hadronic EOSs. Therefore, some of the constraints placed on the EOS from the observation of the gravitational wave event GW170817 do not apply to hadron-quark EOSs. However, the supramassive limit mass for the family of EOSs we treat is consistent with limits set by GW170817, strengthening the possibility of interpreting GW170817 with a hybrid hadron-quark EOSs. We also find that along constant angular momentum sequences of uniformly rotating stars, the third family maximum and minimum mass models satisfy approximate EOS-independent relations, and the supramassive limit of the third family is approximately 16.5 % larger than the third family TOV limit. For differentially rotating spheroidal stars, we find that a lower-limit on the maximum supportable rest mass is 123 % more than the TOV limit rest mass. Finally, we verify that the recently discovered universal relations relating angular momentum, rest mass and gravitational mass for turning-point models hold for hybrid hadron-quark EOSs when uniform rotation is considered, but have a clear dependence on the degree of differential rotation. PACS. 04.40.Dg Relativistic stars: structure, and stability arXiv:1905.00028v1 [astro-ph.HE] 30 Apr 2019 4 Note that this result is in tension with what was found in [85] where different equations of state were adopted. M ↓ M TOV ↓ = 1 + 0.33 J J ↓,Kep 2 − 0.10 J J ↓,Kep 4 . (19)The spread in this equation is at most 2 %. 10 Moreover, we find that the bottom turning points can be described with the same Equations (18), but with a spread of 3 %. The universality becomes tighter if we consider top and bottom turning points separately. For the bottom turning points, the best-fitting functions are M ↓ M TOV ↓ = 1 + 0.35 J M TOV ↓ 2 2 − 0.12 J M TOV ↓ 2 4 , (20a) M 0,↓ M TOV 0,↓ = 1 + 0.58 J M TOV 0,↓ 2 2 − 0.35 J M TOV 0,↓ 2 4

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Section: Maximum Masssupporting

confidence: 72%

Section: A Appendix: Solution Space Of Differentially Rotating Starsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Maximum mass and universal relations of rotating relativistic hybrid hadron-quark stars

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“…More realistic descriptions of the matter may play an important role in the evolution of quasi-toroidal models, but we do not expect it to change our basic conclusion that massive, quasitoroidal models of neutron stars built with the KEH differential rotation law are generically dynamically unstable. In particular, analogous models to those studied here described by the KEH rotation law have been shown to exist for realistic, hybrid hadron-quark, and strange quark matter equations of state [18,19,21]. The KEH law may not suitably describe the remnants of BNS mergers [69,86,87].…”

Section: Discussionmentioning

confidence: 92%

Dynamical stability of quasitoroidal differentially rotating neutron stars

et al. 2019

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We investigate the dynamical stability of relativistic, differentially rotating, quasi-toroidal models of neutron stars through hydrodynamical simulations in full general relativity. We find that all quasi-toroidal configurations studied in this work are dynamically unstable against the growth of non-axisymmetric modes. Both one-arm and bar mode instabilities grow during their evolution. We find that very high rest mass configurations collapse to form black holes. Our calculations suggest that configurations whose rest mass is less than the binary neutron star threshold mass for prompt collapse to black hole transition dynamically to spheroidal, differentially rotating stars that are dynamically stable, but secularly unstable. Our study shows that the existence of extreme quasi-toroidal neutron star equilibrium solutions does not imply that long-lived binary neutron star merger remnants can be much more massive than previously found. Finally, we find models that are initially supra-Kerr (J/M 2 > 1) and undergo catastrophic collapse on a dynamical timescale, in contrast to what was found in earlier works. However, cosmic censorship is respected in all of our cases. Our work explicitly demonstrates that exceeding the Kerr bound in rotating neutron star models does not imply dynamical stability.

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Axisymmetric Rotating Compact Stars

Zhou

2020

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Revisiting the maximum mass of differentially rotating neutron stars in general relativity with realistic equations of state

Cited by 22 publications

References 82 publications

Maximum mass and universal relations of rotating relativistic hybrid hadron-quark stars

Maximum mass and universal relations of rotating relativistic hybrid hadron-quark stars

Dynamical stability of quasitoroidal differentially rotating neutron stars

Axisymmetric Rotating Compact Stars

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