Secondary component of gravitational-wave signal GW190814 as an anisotropic neutron star

Roupas, Zacharias

doi:10.1007/s10509-021-03919-5

Cited by 52 publications

(22 citation statements)

References 71 publications

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“…Using Equation (29) in Equation ( 22) we get the form of mass in terms of the central density which is written in Appendix F. The pattern of the derivative of mass with respect to the central density given by the equation presented in Appendix F 1 and it is plotted in Figure 5d which ensures the stability of our model.…”

Section: Stability In the Static Statementioning

confidence: 92%

“…Moreover, among the gravitational waves, there are three events/candidates involving the merger of one neutron star or light mass black hole with another compact object. If this event is described solely by GR, the lower mass component of the binary can either be a neutron star with an unexpectedly stiff (or exotic) EoS, a black hole with an unexpectedly small mass, or a neutron star with an unexpectedly rapid rotation [10][11][12][13][14][15][16][17][17][18][19][20][21][22][23][24][25][26][27][28][29][30]. On the other hand, an natural and non-exotic description of the lower mass component of the event GW190814 can be given by extended gravity [31][32][33].…”

Section: Introductionmentioning

confidence: 99%

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Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

2022

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In the frame of Gauss–Bonnet gravity and in the limit of D→4, based on the fact that spherically symmetric solution derived using any of regularization schemes will be the same form as the original theory, we derive a new interior spherically symmetric solution assuming specific forms of the metric potentials that have two constants. Using the junction condition we determine these two constants. By using the data of the star EXO 1785-248, whose mass is M=1.3±0.2M⊙ and radius l=8.849±0.4 km, we calculate the numerical values of these constants, in terms of the dimensionful coupling parameter of the Gauss–Bonnet term, and eventually, we get real values for these constants. In this regard, we show that the components of the energy–momentum tensor have a finite value at the center of the star as well as a smaller value to the surface of the star. Moreover, we show that the equations of the state behave in a non-linear way due to the impact of the Gauss–Bonnet term. Using the Tolman–Oppenheimer–Volkoff equation, the adiabatic index, and stability in the static state we show that the model under consideration is always stable. Finally, the solution of this study is matched with observational data of other pulsars showing satisfactory results.

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Section: Stability In the Static Statementioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

2022

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“…The secondary component is either the lightest black hole or the heaviest NS ever discovered. However, this is still a question of debate [201][202][203][204][205][206][207][208][209].…”

Section: Gravitational Waves 421 Observationmentioning

confidence: 99%

Nuclear Physics and Astrophysics Constraints on the High Density Matter Equation of State

Stone

2021

Universe

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(1) This review has been written in memory of Steven Moszkowski who unexpectedly passed away in December 2020. It has been inspired by our many years of discussions. Steven’s enthusiasm, drive and determination to understand atomic nuclei in simple terms of basic laws of physics was infectious. He sought the fundamental origin of nuclear forces in free space, and their saturation and modification in nuclear medium. His untimely departure left our job unfinished but his legacy lives on. (2) Focusing on the nuclear force acting in nuclear matter of astrophysical interest and its equation of state (EoS), we take several typical snapshots of evolution of the theory of nuclear forces. We start from original ideas in the 1930s moving through to its overwhelming diversity today. The development is supported by modern observational and terrestrial data and their inference in the multimessenger era, as well as by novel mathematical techniques and computer power. (3) We find that, despite the admirable effort both in theory and measurement, we are facing multiple models dependent on a large number of variable correlated parameters which cannot be constrained by data, which are not yet accurate, nor sensitive enough, to identify the theory closest to reality. The role of microphysics in the theories is severely limited or neglected, mostly deemed to be too difficult to tackle. (4) Taking the EoS of high-density matter as an example, we propose to develop models, based, as much as currently possible, on the microphysics of the nuclear force, with a minimal set of parameters, chosen under clear physical guidance. Still somewhat phenomenological, such models could pave the way to realistic predictions, not tracing the measurement, but leading it.

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“…Therefore, it is a big challenge to explain the nature of such compact object. There is a lot of debate to understand the mystery of the secondary component of the GW190814 event [2][3][4][5][6][7][8][9][10][11][12]. The analysis of GW190814 data implies the possible nature of such a compact object as a NS only when (i) the equation of state (EOS) is very stiff [8] or (ii) it is a rapidly rotating compact object below the mass shedding frequency [5,12].…”

Section: Introductionmentioning

confidence: 99%

Dark matter admixed neutron star as a possible compact component in the GW190814 merger event

Das,

Kumar,

Patra

2021

Preprint

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We put constraints on the secondary component of GW190814 by analyzing the observational data of the event. The relativistic mean-field models are used to calculate the mass-radius profile and tidal deformability of the compact object, considering it as a massive neutron star with the presence of dark matter particles inside it. With the increase of dark matter percentage, the maximum mass, radius, and tidal deformability of the neutron star decreases. We observe that the predicted properties are well consistent with GW190814 observational data, suggesting the possibility of a dark matter admixed neutron star if the underlying nuclear equation of state is sufficiently stiff.

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Secondary component of gravitational-wave signal GW190814 as an anisotropic neutron star

Cited by 52 publications

References 71 publications

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

Anisotropic Compact Stars in D → 4 Limit of Gauss–Bonnet Gravity

Nuclear Physics and Astrophysics Constraints on the High Density Matter Equation of State

Dark matter admixed neutron star as a possible compact component in the GW190814 merger event

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