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.
The Kiselev black hole is neither perfect fluid, nor is it quin tessence
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The general static spherical perfect fluid solution with EoS parameter w=-1/6 is obtained analytically via Buchdahl transformation of a known solution.
EHT observations of Sgr A* constrain deviations from GR black hole solutions including regular BHs, string-inspired spacetimes, and BH mimickers, with some limits exceeding cosmological bounds.
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.
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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The general static spherical perfect fluid solution with EoS parameter w=-1/6
The general static spherical perfect fluid solution with EoS parameter w=-1/6 is obtained analytically via Buchdahl transformation of a known solution.
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Horizon-scale tests of gravity theories and fundamental physics from the Event Horizon Telescope image of Sagittarius A$^*$
EHT observations of Sgr A* constrain deviations from GR black hole solutions including regular BHs, string-inspired spacetimes, and BH mimickers, with some limits exceeding cosmological bounds.
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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.