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SUMMARY:THE INFLUENCE OF RELATIVISTIC EFFECTS ON THE PARAMETERS OF NEUTRON
  STAR MODELS
DTSTART;VALUE=DATE-TIME:20261029T070000Z
DTEND;VALUE=DATE-TIME:20261029T071500Z
DTSTAMP;VALUE=DATE-TIME:20261101T090901Z
UID:indico-contribution-6193@cern.ch
DESCRIPTION:Speakers: Alina Shmakova (Astrakhan State University named V. 
 N. Tatishchev)\nAbstract: The paper theoretically investigates the equilib
 rium structure of neutron stars consisting of degenerate relativistic neut
 ron gas\, based on the equation of radial mass distribution. The thermodyn
 amic properties of a relativistic Fermi gas are studied\, and a relationsh
 ip between the compressibility coefficient and the particle concentration 
 is established without taking nuclear forces into account. The mass distri
 bution equation is numerically solved for the pulsar PSR J0740+6620\, and 
 its radius\, as well as the radial distributions of density\, pressure\, a
 nd Fermi energy\, are determined. A comparison of relativistic and non‑r
 elativistic models was carried out\, showing that taking relativistic effe
 cts into account leads to a denser star with a smaller radius. Based on nu
 merical calculations\, the Oppenheimer–Volkoff limit was estimated.\n\nK
 eywords: neutron star\, degenerate relativistic neutron gas\, radial distr
 ibution of the star’s mass.\n\nNeutron stars are giant cores consisting 
 of degenerate neutron gas\, primarily bound by gravitational forces. The d
 ensity distribution of stellar matter is examined using the example of the
  pulsar PSR J0740+6620\, whose mass is (2.08  0.07) times the mass of t
 he Sun [1].\nThe radial mass distribution function m(r) of an adiabatic st
 ar in the absence of rotation obeys the equation [2]:\n		m^{″}-\\frac{2}
 {r}m^{\\prime }+\\frac{G}{4\\pi }\\kappa {\\left(\\frac{m^{\\prime }}{r^{2
 }}\\right)}^{2}m=0\, 			(1)\nwhere κ is the compressibility of the substa
 nce\, G is the gravitational constant. It satisfies the boundary condition
 s: m(0)=0 and m(R)=M \, where M is the mass of the star\, and R is its rad
 ius. The compressibility of a degenerate relativistic neutron gas is expre
 ssed as [3]:\n		\\kappa =\\frac{9}{\\pi }\\cdot \\frac{(ch)^{3}}{8E_{0}^{4
 }}\\cdot \\frac{(1+x^{2})^{1/2}}{x^{5}}\, где	x=\\frac{hc}{2E_{0}}{\\le
 ft(\\frac{3n}{\\pi }\\right)}^{1/3}. 	(2)\nHere\, n is the particle concen
 tration\; E0 is the rest energy of the neutron\; h is Planck’s constant\
 ; c is the speed of light. In the non‑relativistic approximation x\n\nht
 tps://indico.particle.mephi.ru/event/626/contributions/6193/
LOCATION: Conference Hall 2
URL:https://indico.particle.mephi.ru/event/626/contributions/6193/
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