Asset Details
Do you wish to reserve the book?
Impact of symmetry energy on sound speed and spinodal decomposition in dense neutron-rich matter
Hey, we have placed the reservation for you!
By the way, why not check out events that you can attend while you pick your title.
Oops! Something went wrong.
Looks like we were not able to place the reservation. Kindly try again later.
Are you sure you want to remove the book from the shelf?
Impact of symmetry energy on sound speed and spinodal decomposition in dense neutron-rich matter
Do you wish to request the book?
Impact of symmetry energy on sound speed and spinodal decomposition in dense neutron-rich matter
Please be aware that the book you have requested cannot be checked out. If you would like to checkout this book, you can reserve another copy
We have requested the book for you!
Your request is successful and it will be processed during the Library working hours. Please check the status of your request in My Requests.
Oops! Something went wrong.
Looks like we were not able to place your request. Kindly try again later.
Journal Article
Impact of symmetry energy on sound speed and spinodal decomposition in dense neutron-rich matter
2023
Overview
Using a meta model for nuclear Equation of State (EOS) with its parameters constrained by astrophysical observations and terrestrial nuclear experiments, we examine effects of nuclear EOS especially its symmetry energy
E
sym
(
ρ
)
term on the speed of sound squared
C
s
2
(
ρ
)
and the critical density
ρ
t
where
C
s
2
(
ρ
t
)
vanishes (indicating the onset of spinodal decomposition) in both dense neutron-rich nucleonic matter relevant for relativistic heavy-ion collisions and the cold
n
+
p
+
e
+
μ
matter in neutron stars at
β
-equilibrium. Unlike in nucleonic matter with fixed values of the isospin asymmetry
δ
, in neutron stars with a density dependent isospin profile
δ
(
ρ
)
determined consistently by the
β
-equilibrium and charge neutrality conditions, the
C
s
2
(
ρ
)
almost always show a peak and then vanishes at
ρ
t
. The latter strongly depends on the high-density behavior of
E
sym
(
ρ
)
if the skewness parameter
J
0
characterizing the stiffness of high-density symmetric nuclear matter (SNM) EOS is not too far above its currently known most probable value of about
-
190
MeV inferred from recent Bayesian analyses of neutron star observables. Moreover, in the case of having a super-soft
E
sym
(
ρ
)
that is decreasing with increasing density above about twice the saturation density of nuclear matter, the
ρ
t
is significantly lower than the density where the
E
sym
(
ρ
)
vanishes (indicating the onset of isospin-separation instability and pure neutron matter formation) in neutron star cores.
Publisher
Springer Berlin Heidelberg,Springer Nature B.V,Springer Nature
