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Gamma ray heating and neutrino cooling rates due to weak interaction processes on sd-shell nuclei in stellar cores

FAYAZ, Muhammad - Personal Name
MAJID, Muhammad - Personal Name
NABI, Jameel-Un - Personal Name

Gamma ray heating and neutrino cooling rates,
due to weak interaction processes, on sd-shell nuclei in stel-
lar core are calculated using the proton neutron quasiparticle
random phase approximation theory. The recent extensive
experimental mass compilation of Wang et al. (Chin. Phys.
C 36:1603, 2012), other improved model input parameters
including nuclear quadrupole deformation (Raman et al. in
At. Data Nucl. Data Tables 78(1):1–128, 2001; Möller et al.
in At. Data Nucl. Data Tables 109:1–204, 2016) and phys-
ical constants are taken into account in the current calcu-
lation. The purpose of this work is two fold, one is to im-
prove the earlier calculation of weak rates performed by
Nabi and Klapdor-Kleingrothaus (At. Data Nucl. Data Ta-
bles 71:149, 1999a) using the same theory. We further com-
pare our results with previous calculations. The selected sd-
shell nuclei, considered in this work, are of special interest
for the evolution of O–Ne–Mg core in 8–10 M stars due to
competitive gamma ray heating rates and cooling by URCA
processes. The outcome of these competitions is to deter-
mine, whether the stars end up as a white dwarf (Nabi in
Phys. Rev. C 78(4):045801, 2008b), an electron-capture su-
pernova (Jones et al. in Astrophys. J. 772(2):150, 2013) or
Fe core-collapse supernova (Suzuki et al. in Astrophys. J.
817(2):163, 2016). The selected sd-shell nuclei for calcu-
lation of associated weak-interaction rates include 20,23 O,
20,23 F, 20,23,24 Ne, 20,23 – 25 Na, and 23 – 25 Mg. The cooling
and heating rates are calculated for density range (10 ≤
ρ (g cm −3 ) ≤ 10 11 ) and temperature range (0.01 × 10 9 ≤
T (K) ≤ 30 × 10 9 ). The calculated gamma heating rates are
B J.-U. Nabi
jameel@giki.edu.pk
1
Faculty of Engineering Sciences, GIK Institute of Engineering
Sciences and Technology, Topi 23640, Khyber Pakhtunkhwa,
Pakistan
orders of magnitude bigger than the shell model rates (ex-
cept for 25 Mg at low densities). At high temperatures the
gamma heating rates are in reasonable agreement. The cal-
culated cooling rates are up to an order of magnitude bigger
for odd-A nuclei.

EB00000004002K Available

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Stellar evolution
Gamma ray heating rates
Neutrino cooling rates
sd-Shell nuclei
pn-QRPA theory
Core-collapse

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Muhammad Fayaz 1 · Jameel-Un Nabi 1 · Muhammad Majid 1

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Gamma ray heating and neutrino cooling rates due to weak interaction processes on sd-shell nuclei in stellar cores

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Gamma ray heating and neutrino cooling rates due to weak interaction processes on sd-shell nuclei in stellar cores

FAYAZ, Muhammad - Personal NameMAJID, Muhammad - Personal NameNABI, Jameel-Un - Personal Name

Series Title

Call Number

Publisher

Collation

Language

ISBN/ISSN

Classification

Content Type

Media Type

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Edition

Subject(s)

Specific Detail Info

Statement of Responsibility

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FAYAZ, Muhammad - Personal Name
MAJID, Muhammad - Personal Name
NABI, Jameel-Un - Personal Name