Can phase transitions of superdense matter strengthen supernova explosions?

Takahara, Mariko; Sato, Katsuhiko

doi:10.1016/0370-2693(85)91346-2

Cited by 26 publications

(17 citation statements)

References 19 publications

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“…The rest will then be transformed either by a slow burning on a time scale of a few seconds to a few minutes [3] or by a detonation [2]. For bag constants above the stability interval,…”

Section: Discussionmentioning

confidence: 99%

“…According to some investigations [2], the transformation occurs during the supernova explosion. In this scenario, the released binding energy is what makes the supernova succeed in the first place, supplying the final "push" which seems to lack in most of the computer simulations of the events.…”

Section: Introductionmentioning

confidence: 99%

“…[7], but with an extra term in the expression for the surface energy of quark matter, and with the two phases treated in a more self-consistent way. Unlike most of the approaches mentioned above [1,2,3,4,5,7], we will be considering the formation of both strange stars (for absolutely stable strange matter) and hybrid stars, where strange matter is formed only in the central regions due to the high pressure. First, we will deal with some general aspects of nucleation (Sec.…”

Section: Introductionmentioning

confidence: 99%

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Nucleation of quark matter bubbles in neutron stars

1994

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The thermal nucleation of quark matter bubbles inside neutron stars is examined for various temperatures which the star may realistically encounter during its lifetime.It is found that for a bag constant less than a critical value, a very large part of the star will be converted into the quark phase within a fraction of a second. Depending on the equation of state for neutron star matter and strange quark matter, all or some of the outer parts of the star may subsequently be converted by a slower burning or a detonation.

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“…The rest will then be transformed either by a slow burning on a time scale of a few seconds to a few minutes [3] or by a detonation [2]. For bag constants above the stability interval,…”

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Nucleation of quark matter bubbles in neutron stars

1994

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“…1, we show the mass-radius relations of the four EOS, for various entropies per baryon S and in beta equilibrium without neutrinos. 1 One observes an interesting feature for the hybrid EOS: with increasing entropy, a second maximum develops, which eventually even becomes the global maximum. It is well known from cold compact stars that stars on the branch between the right maximum and the local minimum are unstable with respect to radial perturbations [24].…”

Section: Novel Third Family Of Compact Starsmentioning

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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“…During the collapse, some sort of phase transition such as a quark deconfinement, hyperon appearance, or meson condensation may occur and affect the dynamics (e.g., Takahara & Sato 1985). In this paper, we investigate the hadron-quark phase transition.…”

Section: Introductionmentioning

confidence: 99%

Stellar core collapse with hadron-quark phase transition

Nakazato

Sumiyoshi

Yamada

2013

A&A

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Context. Hadronic matter undergoes a deconfinement transition to quark matter at high temperature and/or high density. It would be realized in collapsing cores of massive stars. Aims. In the framework of the MIT bag model, the ambiguities of the interaction are encapsulated in the bag constant. Some progenitor stars that invoke the core collapses explode as supernovae, and other ones become black holes. The fates of core collapses are investigated for various cases. Methods. Equations of state including the hadron-quark phase transition are constructed for the cases of the bag constant B = 90, 150, and 250 MeV fm −3 . To describe the mixed phase, the Gibbs condition is used. Adopting the equations of state with different bag constants, the core collapse simulations are performed for the progenitor models with 15 and 40 M . Results. If the bag constant is small, for example B = 90 MeV fm −3 , the interval between the bounce and black hole formation is shortened drastically for the model with 40 M , and the second bounce revives the shock wave leading to explosion for the model with 15 M .

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Can phase transitions of superdense matter strengthen supernova explosions?

Cited by 26 publications

References 19 publications

Nucleation of quark matter bubbles in neutron stars

Nucleation of quark matter bubbles in neutron stars

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

Stellar core collapse with hadron-quark phase transition

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