Speaker
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Abstract
With the advancement in astrophysical instrumentation, the sensitivity and amount of observations associated with the neutron star are improving continuously. This demands sophisticated theoretical models of its structure and composition. Among its various layers, the crust possesses a challenge due to its complexity and importance in various observed phenomena, such as pulsar glitches, quasi-periodic oscillations (QPOs), etc. [1]. In view of crust structure of a neutron star, the compressible liquid drop model (CLDM) has various advantages compared to others, such as lower computational requirement, effectiveness, boundary conditions, etc. [2]. The CLDM model incorporates the compressibility of nuclear matter, negative lattice Coulomb energy, and the suppression of surface tension by the neutron gas [3, 4]. In CLDM formalism, the finite-size effects are introduced via surface and Coulomb energy parametrization in an ad-hoc manner, limiting the results’ sensitivity. The surface energy plays the most significant role and is responsible for the possible deviations [5, 6]. In this work, we intend to investigate the role of surface energy parametrization in the CLDM formalism and its sensitivity toward various neutron star properties. It is seen that the crustal properties of neutron star are significantly affected by the surface energy parametrization. We use the effective relativistic mean field model (E-RMF) to describe the nuclear interaction. The role of the equation of state (EoS) described within E-RMF formalism is also investigated in context to the properties of neutron star crust, such as crust thickness and mass, nuclear pasta thickness and transition properties, etc. The crustal properties are found to be sensitive to the density-dependent symmetry energy and slope parameter.
References
[1] M. Gearheart et al., Mon. Not. R. Astron. Soc 418 (2011) 2343.
[2] T. Carreau et al., A&A 640 (2020) A77.
[3] V. Parmar et al., Phys. Rev. D 105 (2022) 043017.
[4] V. Parmar et al., Phys. Rev. D 106 (2022) 023031.
[5] D. Ravenhall et al., Nucl. Phys. A 407 (1983) 571.
[6] W. G. Newton et al., Astrophys. J. Suppl. Ser. 204 (2013) 9.
| Session | Astroparticle Physics and Cosmology |
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