Analytical model of millisecond pulsar PSR J0514-4002A
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Analytical model of millisecond pulsar PSR J0514-4002A Sajahan Molla1,a , Bidisha Ghosh2,b , Mehedi Kalam2,c 1 Department of Physics, New Alipore College, L Block, New Alipore, Kolkata 700053, India 2 Department of Physics, Aliah University, IIA/27, Action Area II, Newtown, Kolkata 700156, India
Received: 23 August 2020 / Accepted: 6 October 2020 © Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2020
Abstract We construct a relativistic model for the newly discovered millisecond pulsar PSR J0514-4002A located in the globular cluster NGC 1851 (Ridolfi et al. in MNRAS 490:3860, 2019) by using Tolman VII spacetime. We have obtained central density (ρ0 ), central pressure ( p0 ), probable radius, compactness (u) and surface redshift (Z s ) of the above-mentioned newly discovered millisecond pulsar, which is very much consistent with reported data. Equation of state of the millisecond pulsar has come out as stiff in nature which is physically acceptable. Not even that our proposed model can analyze most of the millisecond pulsars having masses up to 1.51M . 1 Introduction The low-mass X-ray binaries (LMXBs) are binary systems in which a neutron star or a black hole accretes matter from a low-mass companion star. These systems (LMXBs) provide a laboratory to test the behavior of matter under extreme physical conditions that are unavailable on Earth. The reprocessed X-ray emission in the outer accretion disk, which is formed around the compact object, dominates the optical flux, thereby overflowing any intrinsic spectral feature of the donor star [1]. The millisecond pulsars (MSPs) are thought to be the offspring of low-mass X-ray binaries (LMXBs) in which mass transfer from a low-mass companion star to the neutron star carries angular momentum and spins it up to a very fast rotation [2]. When the rate of mass transfer decreases in the later evolutionary stages, these binaries host a radio millisecond pulsar [3,4]. At the end of their spin-up phase, they are reactivated as rotation-powered (radio and γ -ray loud) pulsars. In the year 1993, rotation-powered MSPs were identified as pulsed X-ray sources [5]. The millisecond pulsars (MSPs) are apparently long aged and emit optical, X-ray and γ -ray fluxes significantly below from the awaited canonical pulsars with similar periods. The first MSP B1937+214, by the definition of fast accretion spun-up pulsar, was discovered using the Arecibo telescope in 1982 [3]. A number of recently discovered millisecond pulsars (MSPs), which lie in binary systems with evolved companion (neutron star), tend to be lighter than the companion due to reduced mass transfer [6]. The study of millisecond pulsars (MSPs) takes much attention to the astrophysicists in the
a e-mail: [email protected] b e-mail: [email protected] c e-mail: [email protected] (corresponding author)
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present decades [7–14]. This study is very important in the physical as well a
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