Quintessence black holes produce observer-dependent shadow angular sizes, with infalling observers seeing smaller shadows than static ones, yielding stronger equation-of-state constraints from M87* observations.
Schwarzschild black hole surrounded by quintessence: Null geodesics
3 Pith papers cite this work, alongside 155 external citations. Polarity classification is still indexing.
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abstract
We have studied the null geodesics of the Schwarzschild black hole surrounded by quintessence matter. Quintessence matter is a candidate for dark energy. Here, we have done a detailed analysis of the geodesics and exact solutions are presented in terms of Jacobi-elliptic integrals for all possible energy and angular momentum of the photons. The circular orbits of the photons are studied in detail. As an application of the null geodesics, the angle of deflection of the photons are computed.
fields
gr-qc 3years
2026 3representative citing papers
Lowering the quintessence state parameter w_q in Kiselev black holes produces ultra-slow evaporation distinct from PFDM and Horndeski cases, offering a possible constraint on w_q.
Epicyclic frequencies, periapsis shift, and gravitational Larmor precession are derived for charged particles in the weak-magnetic limit of a magnetized Kiselev black hole.
citing papers explorer
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Shadows of quintessence black holes: spherical accretion, photon trajectories, and geodesic observers
Quintessence black holes produce observer-dependent shadow angular sizes, with infalling observers seeing smaller shadows than static ones, yielding stronger equation-of-state constraints from M87* observations.
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Kiselev black hole and the ultra-slow evaporating behavior
Lowering the quintessence state parameter w_q in Kiselev black holes produces ultra-slow evaporation distinct from PFDM and Horndeski cases, offering a possible constraint on w_q.
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Epicyclic motion of charged particles around a weakly magnetized Kiselev black hole
Epicyclic frequencies, periapsis shift, and gravitational Larmor precession are derived for charged particles in the weak-magnetic limit of a magnetized Kiselev black hole.