Stellar core collapse with hadron-quark phase transition

Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Shoichi Yamada

Research output: Contribution to journalArticle

8 Citations (Scopus)

Abstract

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⊙.

Original languageEnglish
Article numberA50
JournalAstronomy and Astrophysics
Volume558
DOIs
Publication statusPublished - Oct 14 2013

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stellar cores
bags
phase transition
quarks
equation of state
equations of state
shock wave
explosion
massive stars
ambiguity
supernovae
explosions
shock waves
intervals
stars
simulation
interactions

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Stellar core collapse with hadron-quark phase transition. / Nakazato, Ken'ichiro; Sumiyoshi, Kohsuke; Yamada, Shoichi.

In: Astronomy and Astrophysics, Vol. 558, A50, 14.10.2013.

Research output: Contribution to journalArticle

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N2 - 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⊙.

AB - 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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