The scenario of two families of compact stars

Drago, A.; Lavagno, Andrea; Pagliara, Giuseppe; Pigato, Daniele

doi:10.1140/epja/i2016-16040-3

Cited by 101 publications

(79 citation statements)

References 90 publications

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“…[37], a negative value of ∂T=∂n B j S was identified for a crossover transition from hadronic to quark matter, and in Ref. [38], it was identified for a hadronic EOS including hyperons and Deltas.…”

Section: Unusual Thermal Properties Of the Eos Induced By The Phamentioning

confidence: 98%

Hot third family of compact stars and the possibility of core-collapse supernova explosions

et al. 2016

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A phase transition to quark matter can lead to interesting phenomenological consequences in corecollapse supernovae, e.g., triggering an explosion in spherically symmetric models. However, until now, this explosion mechanism was only shown to be working for equations of state that are in contradiction with recent pulsar mass measurements. Here, we identify that this explosion mechanism is related to the existence of a third family of compact stars. For the equations of state investigated, the third family is only pronounced in the hot, early stages of the protocompact star and absent or negligibly small at zero temperature and thus represents a novel kind of third family. This interesting behavior is a result of unusual thermal properties induced by the phase transition, e.g., characterized by a decrease of temperature with increasing density for isentropes, and can be related to a negative slope of the phase transition line in the temperature-pressure phase diagram.

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Section: Unusual Thermal Properties Of the Eos Induced By The Phamentioning

confidence: 98%

Hot third family of compact stars and the possibility of core-collapse supernova explosions

et al. 2016

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“…It is important to stress that in this scenario the two families of stars, hadronic stars and quark stars, do coexist and that the transition between the two branches is provided by the appearance, in a hadronic star, of hyperons: once a sizable fraction of strangeness is present through hyperons, the (metastable) stellar system can convert into a pure strange quark star. The appearance of hyperons, as obtained by many calculations, should take place around 2-3 times saturation density, which in turn implies that only hadronic stars more massive than about 1.5 − 1.6M ⊙ can convert, see [10,11].…”

Section: Maximum Mass and Radii Of Strange Quark Starsmentioning

confidence: 88%

“…If future measurements will confirm the existence of stars for which R 1.4 11km [8], then one can conclude that strange quark stars co-exist with hadronic stars, as proposed in Refs. [9][10][11] In this two families scenario compact and light stars are hadronic stars whereas large and massive stars are strange quark stars. Since the ∼ 2M ⊙ compact stars are, in this scenario, interpreted as strange quark stars that implies that the density of bound strange quark matter (i.e.…”

Section: Introductionmentioning

confidence: 99%

Conditions for the existence of stable strange quark matter

2017

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Abstract.We discuss the possible existence of absolutely stable strange quark matter within three different types of chiral models. We will show that confinement plays a crucial role in determining the conditions for the Bodmer-Witten hypothesis to hold true. We discuss also which are the phenomenological signatures, related to measurements of masses and radii of compact stars, which would prove the existence of strange quark stars.

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“…Thus, within this scenario one has two coexisting families of compact stars: pure HSs and QSs. 30,79 The QS branch is occasionally referred to as the "third family" of compact stars, considering white dwarfs as the first family and pure HSs as the second family. Note also that there is a range of values of stellar gravitational mass (see Figs.…”

Section: -30mentioning

confidence: 99%

“…79). The members of these two families could have similar values for their gravitational masses but different values for their radii.…”

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confidence: 99%

Quark deconfinement in neutron stars and astrophysical implications

Bombaci

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2017

The Fourteenth Marcel Grossmann Meeting

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We investigate the quark deconfinement phase transition in cold (T = 0) and hot β-stable hadronic matter. Assuming a first-order phase transition, we calculate and compare the nucleation rate and the nucleation time due to quantum and thermal nucleation mechanisms. We show that above a threshold value of the central pressure a pure hadronic star (HS) (i.e. a compact star with no fraction of deconfined quark matter (QM)) is metastable to the conversion to a quark star (QS) (i.e. a hybrid star or a strange star). This process liberates a huge amount of energy, of the order of 10 53 erg, which produces a powerful neutrino burst, likely accompanied by intense gravitational waves emission, and possibly by a second delayed (with respect to the supernova explosion forming the HS) explosion which could be the energy source of a powerful gamma-ray burst (GRB). This stellar conversion process populates the QS branch of compact stars, thus one has in the universe two coexisting families of compact stars: HSs and QSs. We introduce the concept of critical mass Mcr for cold HSs and proto-hadronic stars (PHSs), and the concept of limiting conversion temperature for PHSs. We show that PHSs with a mass M < Mcr could survive the early stages of their evolution without decaying to QSs. Finally, we discuss the possible evolutionary paths of PHSs.

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The scenario of two families of compact stars

Cited by 101 publications

References 90 publications

Hot third family of compact stars and the possibility of core-collapse supernova explosions

Hot third family of compact stars and the possibility of core-collapse supernova explosions

Conditions for the existence of stable strange quark matter

Quark deconfinement in neutron stars and astrophysical implications

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