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P. S. Negi

Publications and source records attributed to P. S. Negi.

14 recordsLinked to original sources
arXiv2021

The Schwarzschild Mass in General Relativity

The central (surface) energy-density, $E_0 (E_R)$, which appears in the expression of total static and spherical mass, $M$ (corresponding to the total radius $R$) is defined as the density measured only by one observer located at the centre (surface) in the Momentarily Co-moving Reference Frame (MCRF). Since the mass, $M$, depends only on the central (surface) density for most of the equations of state (EOSs) and/or exact analytic solutions of Einstein's field equations available in the literature, the central (surface) density measured in the preferred frame (that is, in the MCRF) appears to be not in agreement with the coordinate invariant form of the field equations that result for the source mass, $M$. In order to overcome the use of any preferred coordinate system (the MCRF) defined for the central (surface) density in the literature, we argue for the first time that the said density may be defined in the coordinate invariant form, that is, in the form of the average density ($3M/4πR^3)$ of the the configuration which turns out to be independent of the radial coordinate $`r'$ and depends only on the central (surface) density of the configuration. In this connection, we further argue that the central (surface) density of the structure should be {\em independent} of the density measured on the other boundary (surface/central) because there exists no a priori relation between the radial coordinate $`r'$ and the proper distance from the centre of the sphere to its surface \cite{Ref1}. In the light of this reasoning, the various EOSs and analytic solutions of Einstein's field equations in which the central and the surface density are {\em interdependent} can not fulfill the definition of central (surface) density measured only by one observer located in the MCRF at the centre (surface) of the configuration.

gr-qc↗
arXiv2019

Turbulent boundary layers around wing sections up to Rec = 1,000,000

Reynolds-number effects in the adverse-pressure-gradient (APG) turbulent boundary layer (TBL) developing on the suction side of a NACA4412 wing section are assessed in the present work. To this end, we analyze four cases at Reynolds numbers based on freestream velocity and chord length ranging from Rec = 100, 000 to 1,000,000, all of them with 5 degree angle of attack. The results of four well-resolved large-eddy simulations (LESs) are used to characterize the effect of Reynolds number on APG TBLs subjected to approximately the same pressure-gradient distribution (defined by the Clauser pressure-gradient parameter beta). Comparisons of the wing profiles with zero-pressure-gradient (ZPG) data at matched friction Reynolds numbers reveal that, for approximately the same beta distribution, the lower-Reynolds-number boundary layers are more sensitive to pressure-gradient effects. This is reflected in the values of the inner-scaled edge velocity Ue+ , the shape factor H, the components of the Reynolds-stress tensor in the outer region and the outer-region production of turbulent kinetic energy. This conclusion is supported by the larger wall-normal velocities and outer-scaled fluctuations observed in the lower-Rec cases.Thus, our results suggest that two complementing mechanisms contribute to the development of the outer region in TBLs and the formation of large-scale energetic structures: one mechanism associated with the increase in Reynolds number, and another one connected to the APG. Future extensions of the present work will be aimed at studying the differences in the outer-region energizing mechanisms due to APGs and increasing Reynolds number.

physics.flu-dyn↗
arXiv2010

Neutron star sequences and the starquake glitch model for the Crab and the Vela pulsars

We construct for the first time, the sequences of stable neutron star (NS) models capable of explaining simultaneously, the glitch healing parameters, $Q$, of both the pulsars, the Crab ($Q \geq 0.7$) and the Vela ($Q \leq 0.2$), on the basis of starquake mechanism of glitch generation, whereas the conventional NS models cannot give such consistent explanation. Furthermore, our models also yield an upper bound on NS masses similar to those obtained in the literature for a variety of modern equations of state (EOSs) compatible with causality and dynamical stability. The results obtained in this paper set an upper and lower bound on the energy of a gravitationally redshifted electron-positron annihilation line in the range of about 0.309 - 0.315 MeV from the Crab and in the range of about 0.425 - 0.439 MeV from the Vela pulsar.

astro-ph↗
arXiv2008

Status of a self-bound equations of state and analytic solutions in general relativity

We have obtained a criterion for spherically symmetric and static structures under hydrostatic equilibrium in general relativity (GR), which states that for a given value of $σ\equiv (P_0/E_0) \equiv $ the ratio of central pressure to central energy-density], the compaction parameter $u \equiv (M/a)$, where $M$ is the total mass and $a$ is the radius of the configuration] or the surface redshift of any regular configuration cannot exceed that of the corresponding homogeneous density sphere, that is, $u \leq u_h$, where $u_h$ is the compaction parameter of the homogeneous density sphere. By examining various exact solutions and surface). On the other hand, configurations having a finite density on the surface (that is, the self-bound structures) do not fulfill this criterion. This criterion puts a severe restriction on the static structures based upon the general relativistic field equations and consequently on the upper limit of mass, surface and central redshift and other physical parameters of spherically symmetric and static configurations.

astro-ph↗
arXiv2008

Dynamical stability of strange quark stars

We show that the mass-radius $(M-R)$ relation corresponding to the MIT bag models of strange quark matter (SQM) and the models obtained by Day et al (1998) do not provide the necessary and sufficient condition for dynamical stability for the equilibrium configurations, since such configurations can not even fulfill the necessary condition of hydrostatic equilibrium provided by the exterior Schwarzschild solution. These findings will remain unaltered and can be extended to any other sequence of pure SQM. This study explicitly show that although the strange quark matter might exist in the state of zero pressure and temperature, but the models of pure strange quark `stars' can not exist in the state of hydrostatic equilibrium on the basis of General Relativity Theory. This study can affect the results which are claiming that various objects like - RX J1856.5-3754, SAX J1808.4-3658, 4U 1728-34, PSR 0943+10 etc. might be strange stars.

astro-ph↗
arXiv2008

Hydrostatic equilibrium of causally consistent and dynamically stable neutron star models

We show that the mass-radius $(M-R)$ relation corresponding to the stiffest equation of state (EOS) does not provide the necessary and sufficient condition of dynamical stability for the equilibrium configurations, since such configurations can not satisfy the `compatibility criterion'. In this connection, we construct sequences composed of core-envelope models such that, like the stiffest EOS, each member of these sequences satisfy the extreme case of causality condition, $v = c = 1$, at the centre. We, thereafter, show that the $M-R$ relation corresponding to the said core-envelope model sequences can provide the necessary and sufficient condition of dynamical stability only when the `compatibility criterion' for these sequences is `appropriately' satisfied. However, the fulfillment of `compatibility criterion' can remain satisfied even when the $M-R$ relation does not provide the necessary and sufficient condition of dynamical stability for the equilibrium configurations. In continuation to the results of previous study, these results explicitly show that the `compatibility criterion' {\em independently} provides, in general, the {\em necessary} and {\em sufficient} condition of hydrostatic equilibrium for any regular sequence. Beside its fundamental feature, this study can also explain simultaneously, both (the higher as well as lower) values of the glitch healing parameter observed for the Crab and the Vela-like pulsars respectively, on the basis of starquake model of glitch generation.

astro-ph↗
arXiv2007

The Stability of an Isentropic Model for a Gaseous Relativistic Star

We show that the isentropic subclass of Buchdahl's exact solution for a gaseous relativistic star is stable and gravitationally bound for all values of the compactness ratio $u [\equiv (M/R)$, where $M$ is the total mass and $R$ is the radius of the configuration in geometrized units] in the range, $0 < u \leq 0.20$, corresponding to the {\em regular} behaviour of the solution. This result is in agreement with the expectation and opposite to the earlier claim found in the literature.

gr-qc↗
arXiv2006

Necessary and sufficient condition for hydrostatic equilibrium in general relativity

We present explicit examples to show that the `compatibility criterion' is capable of providing a {\em necessary} and {\em sufficient} condition for any regular configuration to be compatible with the state of hydrostatic equilibrium. This conclusion is drawn on the basis of the finding that the $M-R$ relation gives the necessary and sufficient condition for dynamical stability of equilibrium configurations only when the compatibility criterion for these configurations is appropriately satisfied. In this regard, we construct an appropriate sequence composed of core-envelope models on the basis of compatibility criterion, such that each member of this sequence satisfies the extreme case of causality condition $v = c = 1$ at the centre. The maximum stable value of $u \simeq 0.3389$ (which occurs for the model corresponding to the maximum value of mass in the mass-radius relation) and the corresponding central value of the local adiabatic index, $(Γ_1)_0 \simeq 2.5911$, of this model are found fully consistent with those of the corresponding {\em absolute} values, $u_{\rm max} \leq 0.3406$, and $(Γ_1)_0 \leq 2.5946$, which impose strong constraints on these parameters of such models. In addition to this example, we also study dynamical stability of pure adiabatic polytropic configurations on the basis of variational method for the choice of the `trial function', $ξ=re^{ν/4}$, as well as the mass-central density relation, since the compatibility criterion is appropriately satisfied for these models. The results of this example provide additional proof in favour of the statement regarding compatibility criterion mentioned above.

astro-ph↗
arXiv2005

A starquake model for Vela pulsar

Various neutron star (NS) models correspond to an unrealistic mass range $\leq 0.5M_\odot$ for the Vela pulsar, if the observational constraints of the glitch healing parameter in the starquake model ($Q = I_{\rm core}/I_{\rm total} \leq 0.2$), are imposed on these models. However, we show that these observational constraints yield a realistic mass range for NS models, corresponding to a core given by the stiffest equations of state (EOS) and the envelope is characterized by the well known EOS of adiabatic polytrope, if the continuity of the adiabatic speed of sound together with pressure, energy-density, and the two metric parameters is assured at the core-envelope boundary of the models and this boundary is worked out on the basis of the `compatibility criterion' for hydrostatic equilibrium. The models yield the surface redshift $z_R \simeq 0.6913$ and mass $M \simeq 2.153 M_\odot$ for the ``central'' weighted mean value, $Q = 0.12 \pm 0.07$, of the glitch healing parameter of the Vela pulsar. These values of mass and surface redshift can increase upto $M \simeq 2.196 M_\odot$ and $z_R \simeq 0.7568$ (which represents an ultra-compact object (UCO; $z_R \geq 0.73$)) respectively for the upper weighted mean value of $Q \simeq 0.19$. However, for the lower weighted mean value of $Q \simeq 0.05$, the mass and surface redshift can decrease upto the values of $M \simeq 2.052 M_\odot$ and $z_R \simeq 0.6066$ respectively. The observation of the lower bound on the energy of a $γ$-ray pulse at about 0.30 MeV from the Vela pulsar in 1984 is in excellent agreement with the results of this study, provided this energy could be interpreted as the energy of a gravitationally redshifted electron-positron annihilation radiation from the star's surface.

astro-ph↗
arXiv2004

Hydrostatic equilibrium of insular, static, spherically symmetric, perfect fluid solutions in general relativity

An analysis of insular solutions of Einstein's field equations for static, spherically symmetric, source mass, on the basis of exterior Schwarzschild solution is presented. Following the analysis, we demonstrate that the {\em regular} solutions governed by a self-bound (that is, the surface density does not vanish together with pressure) equation of state (EOS) or density variation can not exist in the state of hydrostatic equilibrium, because the source mass which belongs to them, does not represent the `actual mass' appears in the exterior Schwarzschild solution. The only configuration which could exist in this regard is governed by the homogeneous density distribution (that is, the interior Schwarzschild solution). Other structures which naturally fulfill the requirement of the source mass, set up by exterior Schwarzschild solution (and, therefore, can exist in hydrostatic equilibrium) are either governed by gravitationally-bound regular solutions (that is, the surface density also vanishes together with pressure), or self-bound singular solutions (that is, the pressure and density both become infinity at the centre).

astro-ph↗
arXiv2004

Rotation curves of spiral galaxies: A general-relativistic model

Spiral galaxies are considered as static, spherically symmetric Dark Matter Configurations (DMC)in which non-zero rest-mass particles (NZRPs) move along appropriate trajectories. Using general relativity (GR), we show that a mass of dark matter about 127 - 212 $\times 10^{11} M_{\odot}$ is required inside the sphere of size $a \sim 10 $ kpc for agreement with the observed typical orbital velocity ranging from 150 to 250 km sec$^{-1}$. In our model, it is possible to obtain flat, slightly rising, and even declining rotation curves. The model self-evidently explains the reason why most of the spirals show almost flat or slightly rising rotation curves and very few show declining curves. The NZRPs follow trajectories, and are finally trapped in circles of minimum radii $\sim 0.03a - 0.005a$ with rotation velocities reaching $\sim 6544-8445$ km sec $^{-1}$. The velocity values are consistent with observations of central regions of various galaxies. This scenario may also lead to conditions suitable for evolution of relativistic supermassive stars and supermassive black holes at the centres of various galaxies. Based on this study, we obtain the density parameter $Ω\sim 0.127 - 0.212 $, leading to an open model of the Universe with an age of $\sim 16.8 - 17.6 $ Gyr, which is significantly higher than the presently estimated age of globular clusters $\sim 13 - 15 $ Gyr.

astro-ph↗
arXiv2004

Causal configurations of homogeneous energy density in general relativity

If the causality condition [the speed of sound always remains less than that of light in vacuum, i. e., $v \leq c = 1$] is imposed on the spheres of homogeneous energy density, the `ratio of the specific heats', $γ\leq 2.59457$, constraints the compaction parameter, $u [\equiv (M/a)$, mass to size ratio in geometrized units] of the dynamically stable configurations $ \leq 0.34056 $ [corresponding to a surface redshift $(z_a) \leq 0.771$]. Apparently, The maximum value of $u$ obtained in this manner belongs to an absolute upper bound, and gives: (i) The maximum value for static neutron star masses as $5.4 M_\odot$, if we substitute the density at the surface of the configuration equal to the average nuclear density, $E = 2 \times 10^{14}$ g cm$^{-3}$ [e.g. {\it Nature}, {\bf 259}, 377 (1976)]. (ii) However, if the density of the static configuration is constrained to the value $1.072 \times 10^{14}$ g cm$^{-3}$, by imposing the empirical result that the minimum rotation period of the fastest rotating pulsar known to date, PSR 1937 + 21, is 1.558 ms, the maximum mass value for static neutron stars exceed upto $7.4 M_\odot$. These masses have important implications for the massive compact objects like Cyg X-1, Cyg XR-1, and LMC-X3 etc., which may not, necessarily, represent black holes. (iii) The minimum rotation periods for a static $1.442 M_\odot$ neutron star to be 0.3041 ms. (iv) A suitable stable model of ultra-compact objects [$u > (1/3)$] which has important astrophysical significance.

astro-ph↗
arXiv2004

Exact Solutions of Einstein's Field Equations

We examine various well known exact solutions available in the literature to investigate the recent criterion obtained in ref. [20] which should be fulfilled by any static and spherically symmetric solution in the state of hydrostatic equilibrium. It is seen that this criterion is fulfilled only by (i) the regular solutions having a vanishing surface density together with the pressure, and (ii) the singular solutions corresponding to a non-vanishing density at the surface of the configuration . On the other hand, the regular solutions corresponding to a non-vanishing surface density do not fulfill this criterion. Based upon this investigation, we point out that the exterior Schwarzschild solution itself provides necessary conditions for the types of the density distributions to be considered inside the mass, in order to obtain exact solutions or equations of state compatible with the structure of general relativity. The regular solutions with finite centre and non-zero surface densities which do not fulfill the criterion [20], in fact, can not meet the requirement of the `actual mass' set up by exterior Schwarzschild solution. The only regular solution which could be possible in this regard is represented by uniform (homogeneous) density distribution. The criterion [20] provides a necessary and sufficient condition for any static and spherical configuration (including core-envelope models) to be compatible with the structure of general relativity. Thus, it may find application to construct the appropriate core-envelope models of stellar objects like neutron stars and may be used to test various equations of state for dense nuclear matter and the models of relativistic stellar structures like star clusters.

gr-qc↗