Other
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985phrvd..31.1864d&link_type=abstract
Physical Review D (Particles and Fields), Volume 31, Issue 8, 15 April 1985, pp.1864-1868
Other
1
Neutron Stars
Scientific paper
The energy density ɛ plays a dominant role in determining properties of relativistic structures. Hence, in addition to the usual adiabatic exponents Γ1, Γ2, and Γ3, three new adiabatic exponents Γ=(d lnP/d lnɛ)S, Γ'-1=(d lnT/d lnɛ)S, and Γ''=(d lnɛ/d lnρ)S are defined. From the relativistic thermodynamic relation for an isothermal neutron-star core, Teν/2=constant, and the isentropic relation, (dɛ/dρ)S=(P+ɛ)/ρ it has been shown that Γ''=Γ2=1+f, Γ3=V2+1, Γ1=(V2/f)(1+f), Γ=V2/f, and Γ'=1+V2/(1+f). From the knowledge of V2(≡dP/dɛ) and f (≡P/ɛ) for any equation of state, one can learn about the behavior of the Γ's. For a purely degenerate neutron gas, we have Γ1=Γ=(5/3) and Γ2=Γ3=Γ'=1 for low densities, and Γ=1, Γ'=(5/4), and Γ1=Γ2=Γ3=(4/3) for infinitely large densities. For almost all equations of state for nuclear matter Γ1 and Γ decrease with increasing density and Γ2, Γ3, and Γ' increase with increasing density. By imposing some conditions on the Γ's we get some known and some new equations of state, viz. Γ1=Γ2=Γ3 leads to the equation P=const×ɛ or P=const×ρT and Γ=Γ2=Γ' leads to the equation P=const×ɛT or dP/dɛ=(P/ɛ)(1+P/ɛ). Equations of state and adiabatic exponents corresponding to constant values of Γ1, Γ2, Γ3, Γ, and Γ' are discussed. Knowledge of Γ2, Γ3, and Γ' helps us in understanding, respectively, the behavior of P, ρ, and ɛ with T for the equations of state of neutron-star matter.
No associations
LandOfFree
Adiabatic exponents and equations of state for neutron-star matter does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Adiabatic exponents and equations of state for neutron-star matter, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Adiabatic exponents and equations of state for neutron-star matter will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1290358