Title: Xia Zhou
1The deconfinement phase transition in the
interior of neutron stars
Huazhong Normal University
May 21, 2009 CSQCD?
2- Phase transition and energy release
- The thermal evolution of neutron stars
- Summary
3Phase transition and energy release
The total energy and baryon number densities for
the mixed phase
With the volume fraction, energy per baryon
The derivative of e with respect to ?
4Phase transition and energy release
Energy release per baryon with respect to total
baryon number
The energy release per baryon during phase
transition
From S to F, the total release energy can be
expressed as
5Phase transition and energy release
- Construct the hybrid stars
- Hadronic phase relativistic mean field theory
(RMF) - Quark phase MIT bag model
- Mixed phase baryon number conservation and
global charge neutrality
6Phase transition and energy release
The baryon number density dependence of releasing
energy per converted baryon for different bag
constants
7Phase transition and energy release
The baryon number density dependence of releasing
energy per converted baryon for soft, moderate
and stiff hadronic matter equation of state
8Phase transition and energy release
Latent heat chemical balance
The absorbed energy per baryon during phase
transition
M. Stejner et.al ApJ, 6941019, 2009
9Phase transition and energy release
Heating luminosity of latent heat
it is less important and does not signi?cantly
change the thermal evolution ( M. Stejner et.al
ApJ, 6941019, 2009)
Heating luminosity of deconfinement heating
10- Hybrid stars neutron star with quark phase or
mixed phase interiors. The mixed phase of
hadronic and quark matter construct with Gibbs
conditions - The cooling equation
- Heating effect released dissipation energy
during varying pressure first-order phase
transition (deconfinement heating)
11Cooling curves of rotating hybrid star with
deconfinement heating
12Surface temperature due to rotochemical heating
and deconfinement heating in quasi-equilibrium
state as a function of stellar radius
O. Kargaltsev et.al ApJ, 602327,2004
13- The deconfinement dissipation would significantly
influence the thermal evolution of neutron stars - For the older pulsars with high thermal
radiation, the deconfinement dissipation heating
mechanism is more effect under the hybrid stars
model - We need more observational data