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Equation Of State and back bending phenomenon in rotating neutron star s. M. Bejger E. Gourgoulhon P. Haensel L. Zdunik. 1 st Astro-PF Workshop – CAMK, 14 October 2004 Compact Stars: structure, dynamics, and gravitational waves. Plan. - PowerPoint PPT Presentation
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Equation Of State and back bending phenomenon in rotating neutron stars
1st Astro-PF Workshop – CAMK, 14 October 2004Compact Stars: structure, dynamics, and gravitational waves
M. BejgerE. GourgoulhonP. HaenselL. Zdunik
Plan
1. Historical remarksGlendenning 1997 Spyrou, Stergioulas 2002
2. Back bending phenomenon for Neutron Stars (with hyperons)new approach MB – Req dependence at fixed frequency
J(f) at fixed baryon mass3. Polytropic EOS and back bending
Phase transition to quark phase through mixed phase4. The role of instability
• rapidly rotating pulsar spins down (looses angular momentum J)• central density increases with time• the density of the transition to the mixed quark-hadron phase is reached• the radius of the star and the moment of inertia significantly decreases • the increase of central density of the star is more important than decrease of angular momentum J=I Ω dJ=I dΩ+Ω dI dΩ = dJ /I - Ω dI /I > 0• the epoch of SPIN-UP BY ANGULAR MOMENTUM LOSS
Spin up
Braking index -singularity
Energy loss equation
Consequences of back-bending
• the braking index has very large value• the isolated pulsar may be observed to be spinning up
Signature of the transition to the mixed phase with quarks
Re-invistigate the deconfinement phase-transition of spinning-down PSR
• fully relativistic, rapidly rotating models (vs. Slow-rotation approximation)• analytic expression for quark phase (vs interpolation of tabulated EOS)• high accuracy of the code and EOS – extremely important
For normal pulsar the quark core appears without back-bending behaviour
Braking index – no singular behaviour
Back-bending for NS with hyperons
• 2-D multidomain LORENE code based on spectral methods• softening of the EOS due to the appereance of hypeons
MB – Req at fixed frequency
Analysis of the BB problem in the baryon mass MB – equatorial radius Req plane:• MB is constant during the evolution of solitary pulsars• at fixed frequency – the frequency are directly connected to the back-bending definition• numerical reasons: frequency is basic input parameter in the numerical calculations of rotating star (with central density ρc)• no need to calculate the evolution of the star with fixed MB
• numerical procedure: input - (f, ρc) , output – (M,MB ,J,R)
Discussion based on MB (ρc) f=const or MB (R) f=const
Softening of the EOS due to the core with hyperons
Signature of BB – minimum of MB at fixed frequency
Back-bending and MB (x) f=const
x=Req x= ρc x= Pc
The softening of the EOS due to the hyperonization leads to the flattening of the MB (x) f=const curves.
Back bending - between two frequencies defined by the existence of the point x of vanishing first and second derivative(point of inflexion).
002
2
dx
Md
dx
dM BB
This condition does not depend on the choice of x.
The onset of back-bending
02
2
constfc
B
rot
M
02
2
constfeq
B
rotR
M
0
constfc
B
rot
M
0
constfeq
B
rot
R
M
Interesting points
• minimum frequency for BB• maximum frequency for deceleration after BB • acceleration from Keplerian configuration
Importance of angular momentum
Why to use angular momentum J instead of moment of inertia I ?
• J is well defined quantity in GR describing the instantaneous state of rotating star• the evolution of rotating star can be easily calculated under some assumptions about the change of J
12/ ndt
dTJT magnetic braking n=3
GW emission n=5
• the moment of inertia defined as J/Ω does not describe the response of the star to the change of J or Ω (rather dJ/dΩ)• J enters the stability condition of rotating stars with respect to axially symmetric perturbations
Instability
0
constMcB
J
0
constJc
BM
0
constJc
M
ANGULAR MOMENTUM
vs
MOMENT OF INERTIA
Angular momentum vs rotational frequency
Angular momentum vs rotational frequency
Importance of the accuracy
The innermost zone boundary not adjusted to the surface of hyperonthreshold except for f~920 Hz
2 domains inthe interior ofthe star
The boundary have to be adjusted to the point of the discontinuity of properties of EOS
Conclusions for NS with hyperons
• the presence of hyperons neutron-star cores can strongly affect the spin evolution of solitary NS (isolated pulsar)• epochs with back-bending for normal rotating NS were found for two of four EOS • for these models pulsar looses half of its initial angular momentum without changing much its rotation period
Mixed Phase – analytical EOS
<1 nuclear matter - polytrope
1< <2 mixed phase – polytrope
>2 quark matter – linear EOS
nnP
nnnP 01
)()()(
4/300 )1()(
3
1)(
P
nnP
Mixed Phase – analytical EOS
Mixed Phase – analytical EOS
Mixed Stable
Mixed Stable
Mixed Unstable
Mixed Unstable
Mixed Marginally Stable
Mixed Marginally Stable
Rotation and stability
If nonrotating stars are stable (ie. softening of the EOS does not result in unstable branch) then for any value of total angular momentum J (fixed) MB increases.
If MB (x) J=0 has local maximum and minimum (unstable region) than for any value of total angular momentum J (fixed) such region exists.
In most cases rotation neither stabilizes nor destabilizes configurations with phase transitions.
Onset of instability – test of the code
• Test of the code (GR effects)• Test of the thermodynamic consistency of the equation of state
dn
ndn
dn
dP )/(2
• Total angular momentum J• Gravitational mass M• Baryon mass MB
The extrema of two of these quantities at third fixed at the same point
Cusps in Figures fixedJBfixedMBfixedM MMMJMJB )(,)(,)(
dNdJdM
First law of thermodynamics
Mixed unstable M(J)
MB =const
Mixed unstable M(MB)
J =const