CONSEQUENCES OF QUARK HADRON PHASE TRANSITION IN DENSE STARS

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CONSEQUENCES OF QUARK HADRON PHASE TRANSITION IN
DENSE STARS

• ABHIJIT BHATTACHARYYA
• SCOTTISH CHURCH COLLEGE
• KOLKATA

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PLAN

• Introduction
• Modelling the phase transition
• Rotating stars
• Effect of rotation on the structural properties
  of star
• Effect of rotation on the neutrino emission
• Conclusion

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Compact Stars

• Formed in the aftermath of Supernovae
• Neutron stars Stable against neutron degeneracy
  pressure
• Core density 8-10 times that of normal nuclear
  matter
• Exotic phase transitions are possible

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Construction of EOS

• Hadronic Interaction

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Quark Phase

• Non-interacting Bag Model
• Mixed phase is constructed using Gibbs
  Construction

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Construction of EOS

• Gibbs Construction

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Rotating Star
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Braking Index
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Neutrino Emission
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Rate equations
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Total Neutrino
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Conclusion

• Quark-Hadron phase transition have been studied
  in rotating compact stars
• The model gives a twin star solution in the
  static limit
• The twin-star solution vanishes for stars
  rotating faster than a certain value of the
  angular velocity
• The total neutrino emission increases by a factor
  of 2
• The angular distribution of the neutrinos are
  very much different from the static stars

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Collaborators

• Sanjay K. Ghosh (Bose Institute)
• Sibaji Raha (Bose Institute)