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<p>In this study, a variable cosmological constant model is created for anisotropic star structures, which satisfies the remaining physical requirements, and validates the required energy conditions (Ecs), and TOV equations. First, the Finch-Skea spacetime solution is taken into account as a static spherically symmetric metric. Moreover, external Schwarzschild geometry is taken into account to correlate our internal stellar structure and determine the values of the constants used in the Finch-Skea spacetime solution. Finally, in this paper, multiple aspects are discussed, such as the radius, compactness, stresses, stability, density profile, and masses under the variable cosmological constant model in <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="10509_2025_4435_Article_IEq1.gif" Format="GIF" Height="19" Rendition="HTML" Resolution="72" Type="Linedraw" Width="58" /> </InlineMediaObject> <EquationSource Format="MATHML"><math> <mi>f</mi> <mo stretchy="false">(</mo> <mi>R</mi> <mo>,</mo> <mi>T</mi> <mo stretchy="false">)</mo> </math></EquationSource> <EquationSource Format="TEX">$f(R,T)$</EquationSource> </InlineEquation> gravity for various stars.</p>

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Impact of a variable cosmological constant on stellar matter configurations in Finch-Skea spacetime

  • 期刊论文

  • 发表日期：

    2025年5月14日

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  • M. Ilyas,
  • Maha,
  • Salma Nawaz,
  • Falak Sher,
  • Fawad Khan

摘要

In this study, a variable cosmological constant model is created for anisotropic star structures, which satisfies the remaining physical requirements, and validates the required energy conditions (Ecs), and TOV equations. First, the Finch-Skea spacetime solution is taken into account as a static spherically symmetric metric. Moreover, external Schwarzschild geometry is taken into account to correlate our internal stellar structure and determine the values of the constants used in the Finch-Skea spacetime solution. Finally, in this paper, multiple aspects are discussed, such as the radius, compactness, stresses, stability, density profile, and masses under the variable cosmological constant model in f ( R , T ) $f(R,T)$ gravity for various stars.