Anisotropic Stars: Exact Solutions

By Krsna Dev, M. Gleiser. 2000

255 citations recorded by the source corpus.

We study the effects of anisotropic pressure on the properties of spherically symmetric, gravitationally bound objects. We consider the full general-relativistic treatment of this problem and obtain exact solutions for various forms of the equation of state connecting the radial and tangential pressures. It is shown that pressure anisotropy can have significant effects on the structure and properties of stellar objects. In particular, the maximum value of 2M / R can approach unity (2M / R < 8/9 for isotropic objects) and the surface redshift can be arbitrarily large.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3fc50a2b7c2c340acb59ef6fa278964e249d7e65

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In Astronomy and Astrophysics

1. Paolo Pani
2. V. Cardoso
3. C. Chirenti
4. L. Crispino
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6. Man Kwong Mak
7. S. Ilijić
8. Tiberiu Harko

Citations in the corpus

• Radial pulsations and stability of anisotropic stars with a quasi-local equation of state (2010, methodology): “In the context of anisotropic stars the normal modes technique was applied to study the stability of some specific configurations in [16] and also [17, 18].”
• How to tell a gravastar from a black hole (2007, background): “This is no longer true for polar perturbations (for which the pressure anisotropy plays an important role) and a study on radial perturbations of stars with anisotropi c pressures was recently presented in [ 19 , 20].”
• Anisotropic stars in general relativity (2001, methodology): “metric case. Then, the resulting expression is used by Herrera, Prisco, Ospino and Fuenmayor (2001) to find new, conformally flat, interior solutions to Einstein equations for locally anisotropic fluid. Dev and Gleiser (2000) presented several exact solutions for anisotropic stars of constant density. ”
• INTO THE LAIR: GRAVITATIONAL-WAVE SIGNATURES OF DARK MATTER (2013, background): “1 Constant density solutions exist – both in Newtonian gravity and in general relativity – also when the fluid is anisotropic, as in the case of selfgravitating scalar fields (Dev & Gleiser 2002).”