Neutron star corequakes and crustquakes

Heintzmann, H.; Hillebrandt, W.; Krotscheck, E.; Kundt, Wolfgang

doi:10.1016/0003-4916(73)90170-x

Cited by 42 publications

(57 citation statements)

References 10 publications

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“…Heintzmann and Hillebrandt [48] established that adiabatic index Γ should be greater 4 3 for a stable stellar configuration. We have evaluated the values of Γ from eq.…”

Section: Adiabatic Indexmentioning

confidence: 99%

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An Appraisal of Spatio—Temporal Occurrence of Fluvial Hazard: Case Study of Flood in the Districts of Jalpaiguri and Alipurduar (West Bengal, India)

Das¹

2022

Fluvial Systems in the Anthropocene

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In this article, we demonstrated a stellar model for compact star in presence of strange matter embedded in D ≥ 4 dimensional space-time defind by Finch-Skea metric. To study the relevant physical properties of the interior matter, we consider the equation of state (hencef orth EOS) as proposed in MIT bag model given by p = 1 3 (ρ − 4B), where B is termed as bag constant. The Mass-Radius relationships in four and higher dimensions are determined using the range of values of surface density through the relation ρs = 4B for which bulk strange matter may be a viable issue for compact objects. Here we choose the range of B such that stable strange matter may exist at zero external pressure relative to neutron. We note that a maximum value of the stellar radius is exist when B is fixed at a given allowed value for which metric functions considered here to be real. This is the maximum allowed radius (bmax) in this model which depends on surface density of a strange star. In four dimensions the compactness of a star is found to be greater than 0.33. In case of higher dimensions (D > 4), we observed different values of compactness. Causality conditions are satisfied interior to the star upto maximum allowed radius (bmax) for which metric function is real. The validity of energy conditions, surface red-shift and other parameters of the stellar configuration are studied and found new results. Stability of the system is also studied.

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“…Heintzmann and Hillebrandt [48] established that adiabatic index Γ should be greater 4 3 for a stable stellar configuration. We have evaluated the values of Γ from eq.…”

Section: Adiabatic Indexmentioning

confidence: 99%

“…The stability creterion of a compat star can be studied from the idea of adiabatic index (Γ) of the interior matter as described by Heintzmann and Hillebrandt [48] and is given below;…”

Section: Adiabatic Indexmentioning

confidence: 99%

An Appraisal of Spatio—Temporal Occurrence of Fluvial Hazard: Case Study of Flood in the Districts of Jalpaiguri and Alipurduar (West Bengal, India)

Das¹

2022

Fluvial Systems in the Anthropocene

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“…This is because the presence of anisotropy may result in a departure from the spherically symmetric distribution in order to escape gravitational collapse. The collapsing condition for perfect fluid distribution with non-relativistic distribution is γ < 4/3 [115,116]. However, when the matter distribution is anisotropic, this changes the form [117,118] to, The second and third terms of the r.h.s represent correction due to relativistic consideration and anisotropy respectively.…”

Section: Adiabatic Indexmentioning

confidence: 99%

Self-bound embedding Class I anisotropic stars by gravitational decoupling within vanishing complexity factor formalism

et al. 2023

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We present a spherically symmetric embedding Class I solution for compact star models using the gravitational decoupling approach. We have chosen a null complexity factor condition proposed by Herrera (Phys Rev D 97:044010, 2018) in the context of a self-gravitating system and derive the anisotropic solution through a systematic approach given by Contreras and Stuchlik (Eur Phys J C 82:706, 2022). In this regard, we use the Finch–Skea model along with the mimicking of mass constraint to find fluid pressure and the matter-energy density from the Einstein Field Equations (EFE). We tested the physical viability and impact of gravitational decoupling on the anisotropic solution through the graphical representation. Moreover, the energy exchange between the fluid distributions along with the mass-radius ratio of different compact objects has been also discussed.

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“…This approach has widely been used in literature. [ 79 ] Here, Γ is characterized as

\begin{equation} \Gamma =\frac{\mu +P_{r}}{P_{r}} {\left(\frac{dP_{r}}{d\mu }\right)}=\frac{\mu +P_{r}}{P_{r}} {\left(v_{sr}^{2}\right)}. \end{equation}

Figure demonstrates the graphical behavior of

\mid v_{s\bot }^{2}-v_{sr}^{2} \mid

and Γ for all candidates corresponding to the calculated values of charge as well as bag constant.…”

Section: Graphical Investigation Of Compact Stars Like Structuresmentioning

confidence: 99%

Study of Charged Compact Stars in Non‐minimally Coupled Gravity

Sharif

Naseer

2022

Fortschritte der Physik

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This paper studies the structural formation of various spherically symmetric anisotropic configured stars in ffalse(scriptR,scriptT,scriptQfalse)$f(\mathcal {R},\mathcal {T},\mathcal {Q})$ gravity under the influence of electromagnetic field, where scriptQ=RησTησ$\mathcal {Q}=\mathcal {R}_{\eta \sigma }\mathcal {T}^{\eta \sigma }$. We construct modified field equations by adopting the Krori‐Barua metric potentials (involving unknowns (A,B,C$A,B,C$)) and employ bag model equation of state to explore the physical characteristics of compact structures like Vela X‐I, 4U 1820‐30, SAX J 1808.4‐3658, Her X‐I and RXJ 1856‐37. The bag constant (frakturBfrakturc$\mathfrak {B_c}$) and other three unknowns are calculated by using experimental data of all considered stars. Further, we adopt a standard model scriptR+ϖRησTησ$\mathcal {R}+\varpi \mathcal {R}_{\eta \sigma }\mathcal {T}^{\eta \sigma }$ to interpret the graphical behavior of energy density, pressure in radial and tangential directions as well as anisotropy. We also investigate mass, compactness parameter, surface redshift and energy conditions for compact bodies by taking model parameter (ϖ) as ±5. The stability of the obtained solution is examined by means of two different criteria. We conclude that our proposed solution meets all the physical requirements and shows stable behavior everywhere for ϖ=5$\varpi =5$.

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Neutron star corequakes and crustquakes

Cited by 42 publications

References 10 publications

An Appraisal of Spatio—Temporal Occurrence of Fluvial Hazard: Case Study of Flood in the Districts of Jalpaiguri and Alipurduar (West Bengal, India)

An Appraisal of Spatio—Temporal Occurrence of Fluvial Hazard: Case Study of Flood in the Districts of Jalpaiguri and Alipurduar (West Bengal, India)

Self-bound embedding Class I anisotropic stars by gravitational decoupling within vanishing complexity factor formalism

Study of Charged Compact Stars in Non‐minimally Coupled Gravity

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