Detailed analysis of the special points on 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>M</mml:mi><mml:mo>−</mml:mo><mml:mi>R</mml:mi></mml:math>
 solutions of hybrid/twin stars

Sen, Debashree; Alam, Naosad; Chaudhuri, Gargi

doi:10.1103/physrevd.106.083008

Cited by 14 publications

(10 citation statements)

References 133 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The effect of DM particles may be viewed as an effective softening/stiffening of the EoS corresponding to the whole structure of DM admixed NSs. This effect in principle represents similar behaviours to BM EoSs at high density such as those happen in the hybrid stars or twin stars as a deconfinement phase transition at the core of NSs Christian & Schaffner-Bielich (2021); Sen et al (2022) or hyperon puzzle Del Popolo et al (2020a). It is worth noting that DM admixed NSs can provide alternative explanations for exotic compact objects which have been detected so far such as the secondary component in the GW190814 event Abbott et al (2020) with the total mass ∼ 2.6M Das et al (2021); Lee et al (2021); Di Giovanni et al (2021), this object can be described within our DM model by the presence of ∼ 20% bosonic SIDM with m χ = 50 MeV and λ = π subject to a visible radius of about 10 km Karkevandi et al (2021).…”

Section: Conclusion and Remarksmentioning

confidence: 54%

Bosonic Dark Matter in Light of the NICER Precise Mass-Radius Measurements

Shakeri¹,

Karkevandi²

2022

Preprint

View full text Add to dashboard Cite

We explore the presence of self-interacting bosonic dark matter (DM) whithin neutron stars (NSs) in light of the latest mass-radius measurements of the Neutron Star Interior Composition Explorer (NICER). The bosonic DM is distributed in NSs as a core for DM particles with high mass, low fraction and low self-coupling constant or as a halo for particles with low mass, high fraction and high self-coupling constant leading to formation of DM admixed NSs. We focus on the evolution of the visible and dark radius of the mixed object due to DM model parameters and fractions. It is shown that DM core formation reduces the visible radius and total mass pushing them below observational limits while halo formation is in favor of the latest mass-radius constraints. Applying joint constraints for radius of 1.4M NSs and the maximum mass from NICER and LIGO/Virgo observations, we scan over the parameter space of the bosonic DM model to obtain an allowed region. It turns out that the maximum mass limit provides a more stringent constraint compare to the radius one. Our investigation allows for the exclusion of a large portion of DM fractions for sub-GeV bosons and limited the amount of accumulated DM to be less than ∼ 4% for the entire mass range at the strong coupling regime λ = π. In this paper, we introduce main features of the pulse profile corresponding to the DM admixed NS and the effect of DM halo on the light bending is considered extensively as an independent probe for the DM model. We find that the depth of minimum fluxes in the pulse profiles crucially depend on the amount of DM distributed around NS and its compactness. The current/future astrophysics missions via precise measurements of compact object properties may test the possibility of the existence of DM within NSs and break the degeneracies between different scenarios to interpret exotic observations.

show abstract

Section: Conclusion and Remarksmentioning

confidence: 54%

Bosonic Dark Matter in Light of the NICER Precise Mass-Radius Measurements

Shakeri¹,

Karkevandi²

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…To give an example of SP non-invariance, in Ref. [17] a notable spread of SPs in the mass-radius diagram was obtained for six different hadronic EOS. The likely reason for this should be the usage of a densitydependent bag pressure functional in the bag model description of the quark matter phase.…”

Section: Invariance Of Spts Under Change Of the Hadronic Eosmentioning

confidence: 99%

Special point "trains" in the M-R diagram of hybrid stars

Blaschke

Ayriyan²,

Cierniak³

et al. 2022

EPJ Web Conf.

View full text Add to dashboard Cite

We present a systematic investigation of the possible locations for the special point (SP), a unique feature of hybrid neutron stars in the massradius diagram. The study is performed within the two-phase approach where the high-density (quark matter) phase is described by the covariant nonlocal Nambu–Jona-Lasinio (nlNJL) model equation of state (EOS) which is shown to be equivalent to a constant-sound-speed (CSS) EOS. For the nuclear matter phase around saturation density different relativistic density functional EOSs are used: DD2p00, its excluded-volume modification DD2p40 and the hypernuclear EOS DD2Y-T. In the present contribution we apply the Maxwell construction scheme for the deconfinement transition and demonstrate that a simultaneous variation of the vector and diquark coupling constants results in the occurrence of SP "trains" which are invariant against changing the nuclear matter EOS. We propose that the SP train corresponding to a variation of the diquark coupling at constant vector coupling is special since it serves as a lower bound for the line of maximum masses and accessible radii of massive hybrid stars.

show abstract

“…Of them, one is generally located on the regular neutron (hadronic) star branch or the first stable branch while the other is a HS lying on the second stable branch. The two branches are often disconnected from each other by an instable region [19,28,29,32,38,46]. However, the location of the twins depends on the transition density of the HSs.…”

Section: Introductionmentioning

confidence: 99%

“…The appearance of SPs on the mass-radius diagram of HSs is an effect of variation of certain parameters related to different quark models [27-29, 33, 38-40, 57, 59]. The existence of such SPs can thus be treated as universal property of HS models and they serve as a remarkable tool to interpret the multi-messenger data as signals for the possible existence of HSs [33,40,46].…”

Section: Introductionmentioning

confidence: 99%

“…Recently, we studied HS properties obtained with different hadronic models and the MIT bag model with density dependent bag pressure in a Gaussian distribution form [60,61] with special emphasis on the formation of third family of compact stars and the emergence of SPs [46]. We showed that the mass corresponding to SP (M SP ) and the maximum mass (M max ) of the HSs follow a nearly linear (fitted) relationship where the slope is independent of the value of bag pressure.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Speed of Sound in Hybrid Stars and the Role of Bag Pressure in the Emergence of Special Points on M-R Variation of Hybrid Stars

Pal¹,

Podder²,

Sen³

et al. 2023

Preprint

View full text Add to dashboard Cite

We compute the hybrid star (HS) properties with the help of Maxwell construction. For the purpose we choose a fixed hadronic model and four different forms of MIT bag model for the quark phase. We investigate thoroughly the effects of the different parameters of the bag model on the speed of sound in HS matter and the structural properties of HSs in the light of the various recent constraints on them from astrophysical observations. We also examine the importance of each parameter involved in these four forms of bag model in the context appearance of special points (SPs) in the mass-radius (M − R) variation of HSs. We find that among all these parameters the bag pressure play the most significant role in the emergence of the SPs in the M − R dependence of HSs.

show abstract

Detailed analysis of the special points on M−R solutions of hybrid/twin stars

Cited by 14 publications

References 133 publications

Bosonic Dark Matter in Light of the NICER Precise Mass-Radius Measurements

Bosonic Dark Matter in Light of the NICER Precise Mass-Radius Measurements

Special point "trains" in the M-R diagram of hybrid stars

Speed of Sound in Hybrid Stars and the Role of Bag Pressure in the Emergence of Special Points on M-R Variation of Hybrid Stars

Contact Info

Product

Resources

About