Rana Nandi
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View article: Evidence of Phase Transition from Binary Neutron Star Merger
Evidence of Phase Transition from Binary Neutron Star Merger Open
Binary neutron-star mergers offer crucial insights into the matter properties of neutron stars. We present direct evidence of phase transition on the observational signatures from such events. Our study employs a range of equations of stat…
View article: Structural response of neutron stars to rapid rotation and its impact on the braking index
Structural response of neutron stars to rapid rotation and its impact on the braking index Open
Pulsars are rotating neutron stars that are observed to be slowing down, implying a loss of their rotational energy. There can be several different physical mechanisms involved in their spin-down process. The properties of fast-rotating pu…
View article: MURCA driven bulk viscosity in neutrino trapped baryonic matter
MURCA driven bulk viscosity in neutrino trapped baryonic matter Open
We examine bulk viscosity, taking into account trapped neutrinos in baryonic matter, in the context of binary neutron star mergers. Following the merging event, the binary star can yield a remnant compact object with densities up to 5 nucl…
View article: Inferring Neutron Star Properties via r-mode Gravitational Wave Signals
Inferring Neutron Star Properties via r-mode Gravitational Wave Signals Open
We present two frameworks to infer some of the properties of neutron stars from their electromagnetic radiation and the emission of continuous gravitational waves due to r-mode oscillations. In the first framework, assuming a distance meas…
View article: MURCA driven Bulk viscosity in neutrino trapped baryonic matter
MURCA driven Bulk viscosity in neutrino trapped baryonic matter Open
We examine bulk viscosity, taking into account trapped neutrinos in baryonic matter, in the context of binary neutron star mergers. Following the merging event, the binary star can yield a remnant compact object with densities up to $5$ nu…
View article: Low Density Neutron Star Matter with Quantum Molecular Dynamics: The Role of Isovector Interactions
Low Density Neutron Star Matter with Quantum Molecular Dynamics: The Role of Isovector Interactions Open
The effect of isospin-dependent nuclear forces on the inner crust of neutron stars is modeled within the framework of Quantum Molecular Dynamics (QMD). To successfully control the density dependence of the symmetry energy of neutron-star m…
View article: Semi-empirical relation to understand matter properties at neutron star interiors
Semi-empirical relation to understand matter properties at neutron star interiors Open
The occurrence of quark matter at the center of neutron stars is still in debate. This study defines some semi-empirical parameters that try to quantify the presence and the amount of quark matter at star interiors. We find that one needs …
View article: Low Density Neutron Star Matter with Quantum Molecular Dynamics: The Role of Vector Interactions
Low Density Neutron Star Matter with Quantum Molecular Dynamics: The Role of Vector Interactions Open
The effect of isospin-dependent nuclear forces on the inner crust of neutron stars is modeled within the framework of Quantum Molecular Dynamics (QMD). To successfully control the density dependence of the symmetry energy of neutron-star m…
View article: Effect of the Landau quantization of electrons on the inner crusts of hot neutron stars
Effect of the Landau quantization of electrons on the inner crusts of hot neutron stars Open
In the present work we study the effects of strongly quantizing magnetic fields and finite temperature on the properties of inner crusts of hot neutron stars. The inner crust of a neutron star contains neutron-rich nuclei arranged in a lat…
View article: Semi Universal relation to understand matter properties at neutron star interiors
Semi Universal relation to understand matter properties at neutron star interiors Open
The occurrence of quark matter at the center of neutron stars is still in debate. This study defines some semi-empirical parameters that quantify the occurrence and the amount of quark matter at star interiors. These parameters show semi-u…
View article: Towards mitigation of apparent tension between nuclear physics and astrophysical observations by improved modeling of neutron star matter
Towards mitigation of apparent tension between nuclear physics and astrophysical observations by improved modeling of neutron star matter Open
Observations of neutron stars (NSs) by the LIGO-Virgo and NICER collaborations have provided reasonably precise measurements of their various macroscopic properties. In this paper, we employ a Bayesian framework to combine them and place i…
View article: GW190814: on the properties of the secondary component of the binary
GW190814: on the properties of the secondary component of the binary Open
We show that the odds of the mass-gap (secondary) object in GW190814 being a neutron star (NS) improve if one allows for a stiff high-density equation of state (EoS) or a large spin. Since its mass is $\in (2.50,2.67) \, \mathrm{M}_{\odot …
View article: Maximum mass of hybrid star formed via shock-induced phase transition in cold neutron stars
Maximum mass of hybrid star formed via shock-induced phase transition in cold neutron stars Open
This paper studies the maximum mass limit of the hybrid star formed after the shock-induced phase transition of a cold neutron star. By employing hadronic and quark equation of state that satisfies the current mass bound, we use combustion…
View article: Observed glitches in 8 young pulsars
Observed glitches in 8 young pulsars Open
The abrupt change in the pulse period of a pulsar is called a pulsar glitch. In this paper, we present eleven pulsar glitches detected using the Ooty Radio Telescope (ORT) and the upgraded Giant Metrewave Radio Telescope (uGMRT) in high ca…
View article: Role of crustal physics in the tidal deformation of a neutron star
Role of crustal physics in the tidal deformation of a neutron star Open
In the late inspiral phase, gravitational waves from binary neutron star mergers carry the imprint of the equation of state due to the tidally deformed structure of the components. If the stars contain solid crusts, then their shear modulu…
View article: Constraining the relativistic mean-field model equations of state with gravitational wave observations
Constraining the relativistic mean-field model equations of state with gravitational wave observations Open
The first detection of gravitational waves from the binary neutron star merger event GW170817 has started to provide important new constraints on the nuclear equation of state at high density. The tidal deformability bound of GW170817 comb…
View article: Glitch Behavior of Pulsars and Contribution from Neutron Star Crust
Glitch Behavior of Pulsars and Contribution from Neutron Star Crust Open
Pulsars are highly magnetized rotating neutron stars (NSs) with a very stable rotation speed. Irrespective of their stable rotation rate, many pulsars have been observed to feature a sudden jump in the spin frequency, known as a pulsar gli…
View article: Constraining the equation of state with gravitational wave observation
Constraining the equation of state with gravitational wave observation Open
The first detection of gravitational waves from binary neutron star merger event GW170817 has started to provide important new constraints on the nuclear equation of state at high density. The tidal deformability bound of GW170817 combined…
View article: Effect of the Coulomb interaction on the liquid-gas phase transition of nuclear matter
Effect of the Coulomb interaction on the liquid-gas phase transition of nuclear matter Open
We investigate the role of the Coulomb interaction on the liquid-gas phase transition of nuclear matter with three different values of proton fraction ($Y_p$=0.5,0.3 and 0.1), relevant for heavy-ion physics as well as various astrophysical…
View article: Studies of the neutron star crust
Studies of the neutron star crust Open
The physics of the neutron star crust is highly relevant for many observable phenomena like the temperature evolution of accreting neutron stars or the evolution of supernovae. In order to investigate the structure and dynamics of the crus…
View article: Simulations of the Neutron Star Crust
Simulations of the Neutron Star Crust Open
The properties of the neutron star crust are crucially important for many physical processes occurring in the star. For instance, the crustal transport coefficients define the temperature evolution of accreting stars after bursts, which ca…
View article: Low-density nuclear matter with quantum molecular dynamics: The role of the symmetry energy
Low-density nuclear matter with quantum molecular dynamics: The role of the symmetry energy Open
We study the effect of isospin-dependent nuclear forces on the pasta phase in the inner crust of neutron stars. To this end we model the crust within the framework of quantum molecular dynamics (QMD). For maximizing the numerical performan…
View article: Role of nuclear physics in oscillations of magnetars
Role of nuclear physics in oscillations of magnetars Open
Strong magnetic fields have important effects on the crustal properties of\nmagnetars. Here we study the magneto-elastic oscillations of magnetars taking\ninto consideration the effect of strong magnetic fields on the crustal\ncomposition …
View article: Nonequilibrium phase transition in compact stars through a violent shock
Nonequilibrium phase transition in compact stars through a violent shock Open
In this letter we study the dynamics of a first order phase transition from\nnucleonic to quark matter in neutron stars. Using standard equations of state\nfor these two phases we find the density range where such a transition is\npossible…