J/A+A/635/A84 BSk26 functionals (Carreau+, 2020)
Crystallization of the inner crust of a neutron star and the influence of shell
effects.
Carreau T., Gulminelli F., Chamel N., Fantina A.F., Pearson J.M.
<Astron. Astrophys. 635, A84 (2020)>
=2020A&A...635A..84C 2020A&A...635A..84C (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics
Keywords: stars: neutron - dense matter - plasmas
Abstract:
In the cooling process of a non-accreting neutron star, the
composition and properties of the crust are thought to
be fixed at the finite temperature where nuclear reactions fall out of
equilibrium. A lower estimation for this temperature is given by the
crystallization temperature, which can be as high as ∼7x109K in the
inner crust, potentially leading to sizeable differences with respect
to the simplifying cold-catalyzed matter hypothesis.
We extend a recent work (Fatina et al., 2020, Cat. J/A+A/633/A149) on
the outer crust, to the study of the crystallization of the inner
crust and the associated composition in the one-component plasma
approximation.
The finite temperature variational equations for non-uniform matter in
both the liquid and the solid phases are solved using a compressible
liquid-drop approach with parameters optimized on four different
microscopic models which cover the present uncertainties in nuclear
modeling.
We consider separately the effect of the different nuclear ingredients
with their associated uncertainties, namely the nuclear equation of
state, the surface properties in the presence of a uniform gas of
dripped neutrons, and the proton shell effects arising from the ion
single-particle structure. Our results suggest that the highest source
of model dependence comes from the smooth part of the nuclear
functional.
We show that shell effects play an important role at the lowest
densities close to the outer crust, but the most important physical
ingredient to be settled for a quantitative prediction of the inner
crust properties is the surface tension at extreme isospin values.
Description:
BSk22-BSk26 functionals. The ETF energy per nucleon is calculated for
nuclei up to nuclear drip lines, from Z=8 up to Z=122. The surface and
curvature parameters of our CLDM are fit to the ETF energy per nucleon
in order to avoid the double counting of shell effects when adding
Strutinsky shell corrections on top of the CLD energy.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
bsk22.dat 19 9896 BSk22 ETF mass table
bsk24.dat 19 9896 BSk24 ETF mass table
bsk25.dat 19 9896 BSk25 ETF mass table
bsk26.dat 19 9896 BSk26 ETF mass table
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See also:
J/A+A/633/A149 : Crystallization of neutron star outer crust (Fantina+, 2020)
Byte-by-byte Description of file: bsk22.dat bsk24.dat bsk25.dat bsk26.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Z Atomic number
7- 9 I3 --- A Mass number
12- 19 F8.5 --- E ? ETF energy per nucleon
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Acknowledgements:
Thomas Carreau, carreau(at)lpccaen.in2p3.fr
(End) Patricia Vannier [CDS ] 10-Mar-2020