Studying the onset of deconfinement with multi‐messenger astronomy of neutron stars

Blaschke, D.; Cierniak, Mateusz

doi:10.1002/asna.202113909

Cited by 42 publications

(56 citation statements)

References 44 publications

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“…From this condition, together with the chemical potential at the saturation density

μ false(n_{0} false) = {ξ μ}_{0}

, follows from Equation (2) for the limiting case

c_{s}^{2} = 1

the minimal value of

A

A_{\min} = \frac{n_{0} μ_{0}}{2 ξ} = 81 MeV {normalfm}^{- 3},

when for typical nuclear EoS

ξ = 0.98

. By combining this limit with the relation between the mass

M_{normalSP}

of the SP and

M_{\max}

, that has been found by Blaschke & Cierniak (2021), we can estimate the minimum value of the maximum mass (

M_{\max} = M_{normalSP}

) for a given choice of the speed of sound parameter. The extent of this estimate is visible in Figure 3, with the resulting prediction on

M_{\max}

and the range of radii to be expected at the mass of PSR J0740 + 6620 listed in Table 1.…”

Section: Location Of the Special Point And Its Propertiesmentioning

confidence: 63%

“…In this work, we have extended the investigations of the SP of hybrid star sequences and its properties which we started in Blaschke & Cierniak (2021) and Cierniak & Blaschke (2020) following up on the initial study (Yudin et al 2014). In particular, we demonstrated for the first time that the SP is also invariant when the phase transition construction within the class of two‐phase approaches is altered from the traditional Maxwell construction to the replacement interpolation method using a parabolic interpolation with the lower limit on the onset of the mixed phase at

n_{onset} \geq n_{0}

and demanding causality (

c_{s}^{2} \leq 1

) as well as mechanical stability (

dn / italicd μ \geq 0

everywhere) for the resulting hybrid EoS.…”

Section: Discussionmentioning

confidence: 98%

“…This situation allows for two new types of masquerade effect. Alford et al (2005), namely, when a hybrid EoS of the first kind (stiff hadronic ‐ soft quark matter) masquerades like a soft hadronic one (see, e.g., Blaschke et al 2020) and one of the second kind (soft hadronic ‐ stiff quark matter) which masquerades like a stiff hadronic one (see, e.g., Blaschke & Cierniak 2021). Such situations can now be systematically generated and investigated with the help of the SP that should be chosen to lie on that hadronic EoS which should appear as a masquerade of a suitably chosen hybrid EoS sequence belonging to that same SP.…”

Section: Discussionmentioning

confidence: 99%

“…In this manuscript, we will analyze the possibility of a phenomenological constant–speed–of–sound (CSS) model to consistently explain all of the current multimessenger observations. For that purpose, we will employ the “Special Point” interface, a heuristic tool discovered in Yudin et al (2014) and recently studied in Cierniak & Blaschke (2020) and Blaschke & Cierniak (2021). This tool makes use of a property that is unique to two–phase models, namely, the existence of a stationary point for hybrid star sequences in the mass–radius plot with respect to variations of the onset density of the second phase.…”

Section: Introductionmentioning

confidence: 99%

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Hybrid neutron stars in the mass‐radius diagram

Cierniak

Blaschke

2021

Astron Nachr

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We present a systematic investigation of the possible locations for the special point (SP), a unique feature of hybrid neutron stars in the mass-radius diagram. The study is performed within the two-phase approach where the high-density (quark matter) phase is described by the constant-sound-speed (CSS) equation of state (EoS) and the nuclear matter phase around saturation density is varied from very soft (APR) to stiff (DD2 with excluded nucleon volume). Different construction schemes for the deconfinement transition are applied: Maxwell construction, mixed phase construction, and parabolic interpolation. We demonstrate for the first time that the SP is invariant not only against changing the nuclear matter EoS, but also against variation of the construction schemes for the phase transition. Since the SP serves as a proxy for the maximum mass and accessible radii of massive hybrid stars, we draw conclusions for the limiting masses and radii of hybrid neutron stars.

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“…From this condition, together with the chemical potential at the saturation density

μ false(n_{0} false) = {ξ μ}_{0}

, follows from Equation (2) for the limiting case

c_{s}^{2} = 1

the minimal value of

A

A_{\min} = \frac{n_{0} μ_{0}}{2 ξ} = 81 MeV {normalfm}^{- 3},

when for typical nuclear EoS

ξ = 0.98

. By combining this limit with the relation between the mass

M_{normalSP}

of the SP and

M_{\max}

, that has been found by Blaschke & Cierniak (2021), we can estimate the minimum value of the maximum mass (

M_{\max} = M_{normalSP}

) for a given choice of the speed of sound parameter. The extent of this estimate is visible in Figure 3, with the resulting prediction on

M_{\max}

and the range of radii to be expected at the mass of PSR J0740 + 6620 listed in Table 1.…”

Section: Location Of the Special Point And Its Propertiesmentioning

confidence: 63%

n_{onset} \geq n_{0}

and demanding causality (

c_{s}^{2} \leq 1

) as well as mechanical stability (

dn / italicd μ \geq 0

everywhere) for the resulting hybrid EoS.…”

Section: Discussionmentioning

confidence: 98%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Hybrid neutron stars in the mass‐radius diagram

Cierniak

Blaschke

2021

Astron Nachr

Self Cite

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show abstract

“…To circumvent that obstacle, we make use of the recently discovered fact that in the range of densities relevant for NS applications the nlNJL model can be represented with high accuracy by a constant-speed-of-sound (CSS) EoS [43]. This EoS is given by [44,45]…”

Section: Constant Speed-of-sound Representationmentioning

confidence: 99%

Bayesian analysis of multimessenger M-R data with interpolated hybrid EoS

et al. 2021

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We introduce a family of equations of state (EoS) for hybrid neutron star (NS) matter that is obtained by a two-zone parabolic interpolation between a soft hadronic EoS at low densities and a set of stiff quark matter EoS at high densities within a finite region of chemical potentials $$\mu _H< \mu < \mu _Q$$ μ H < μ < μ Q . Fixing the hadronic EoS as the APR one and choosing the color-superconducting, nonlocal NJL model with two free parameters for the quark phase, we perform Bayesian analyses with this two-parameter family of hybrid EoS. Using three different sets of observational constraints that include the mass of PSR J0740+6620, the tidal deformability for GW170817, and the mass-radius relation for PSR J0030+0451 from NICER as obligatory (set 1), while set 2 uses the possible upper limit on the maximum mass from GW170817 as an additional constraint and set 3 instead of the possibility that the lighter object in the asymmetric binary merger GW190814 is a neutron star. We confirm that in any case, the quark matter phase has to be color superconducting with the dimensionless diquark coupling approximately fulfilling the Fierz relation $$\eta _D=0.75$$ η D = 0.75 and the most probable solutions exhibiting a proportionality between $$\eta _D$$ η D and $$\eta _V$$ η V , the coupling of the repulsive vector interaction that is required for a sufficiently large maximum mass. We used the Bayesian analysis to investigate with the method of fictitious measurements the consequences of anticipating different radii for the massive $$2~M_\odot $$ 2 M ⊙ PSR J0740+6220 for the most likely equation of state. With the actual outcome of the NICER radius measurement on PSR J0740+6220 we could conclude that for the most likely hybrid star EoS would not support a maximum mass as large as $$2.5~M_\odot $$ 2.5 M ⊙ so that the event GW190814 was a binary black hole merger.

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Symmetry energy of strange quark matter and tidal deformability of strange quark stars

Xia

Lù

et al. 2022

NUCL SCI TECH

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Studying the onset of deconfinement with multi‐messenger astronomy of neutron stars

Cited by 42 publications

References 44 publications

Hybrid neutron stars in the mass‐radius diagram

Hybrid neutron stars in the mass‐radius diagram

Bayesian analysis of multimessenger M-R data with interpolated hybrid EoS

Symmetry energy of strange quark matter and tidal deformability of strange quark stars

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