Quark matter nucleation in hot hadronic matter

We study the quark deconfinement phase transition in hot β-stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per baryon of the hadron–quark phase transition. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucle...

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Published inPhysics letters. B Vol. 680; no. 5; pp. 448 - 452
Main Authors Bombaci, I., Logoteta, D., Panda, P.K., Providência, C., Vidaña, I.
Format Journal Article
LanguageEnglish
Published Kidlington Elsevier B.V 12.10.2009
Elsevier
Subjects
Dense matter
Elementary particles
Exact sciences and technology
neutron
Nuclear physics
Physics
Stars
The physics of elementary particles and fields
Dense matter
26.60.+c
25.75.Nq
97.60.Jd
Stars
Elementary particles
Neutron stars
Nucleation
Quarks
Critical mass
Phase transitions
Baryons
Protostars
Hadrons
Quark matter
Stellar mass
First order
Quark star
Critical temperature
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Abstract We study the quark deconfinement phase transition in hot β-stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per baryon of the hadron–quark phase transition. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates the finite temperature quantum nucleation mechanism. We next discuss the consequences for the physics of proto-neutron stars. We introduce the concept of limiting conversion temperature and critical mass Mcr for proto-hadronic stars, and we show that proto-hadronic stars with a mass M<Mcr could survive the early stages of their evolution without decaying to a quark star.
AbstractList We study the quark deconfinement phase transition in hot β-stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per baryon of the hadron–quark phase transition. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates the finite temperature quantum nucleation mechanism. We next discuss the consequences for the physics of proto-neutron stars. We introduce the concept of limiting conversion temperature and critical mass Mcr for proto-hadronic stars, and we show that proto-hadronic stars with a mass M<Mcr could survive the early stages of their evolution without decaying to a quark star.
Author Bombaci, I.
Vidaña, I.
Logoteta, D.
Panda, P.K.
Providência, C.
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  fullname: Panda, P.K.
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  givenname: C.
  surname: Providência
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  surname: Vidaña
  fullname: Vidaña, I.
  organization: Centro de Física Computacional, Department of Physics, University of Coimbra, 3004-516 Coimbra, Portugal
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Issue 5
Keywords Dense matter
26.60.+c
25.75.Nq
97.60.Jd
Stars
Elementary particles
Neutron stars
Nucleation
Quarks
Critical mass
Phase transitions
Baryons
Protostars
Hadrons
Quark matter
Stellar mass
First order
Quark star
Critical temperature
Language English
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Snippet We study the quark deconfinement phase transition in hot β-stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per...
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SubjectTerms Dense matter
Elementary particles
Exact sciences and technology
neutron
Nuclear physics
Physics
Stars
The physics of elementary particles and fields
Title Quark matter nucleation in hot hadronic matter
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