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Xia Zhou

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Title: Xia Zhou


1
The deconfinement phase transition in the
interior of neutron stars
Huazhong Normal University
  • Xia Zhou Xiao-ping Zheng

May 21, 2009 CSQCD?
2
  • Phase transition and energy release
  • The thermal evolution of neutron stars
  • Summary

3
Phase 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 ?
4
Phase 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
5
Phase 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

6
Phase transition and energy release
The baryon number density dependence of releasing
energy per converted baryon for different bag
constants
7
Phase 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
8
Phase transition and energy release
Latent heat chemical balance
The absorbed energy per baryon during phase
transition
M. Stejner et.al ApJ, 6941019, 2009
9
Phase 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)

11
Cooling curves of rotating hybrid star with
deconfinement heating
12
Surface 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
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