Quartically self-interacting massive boson stars are stable only up to the first mass maximum; their head-on mergers yield a boson-star remnant, a black hole at contact, or two black holes formed before contact, with radiated energy varying non-monotonically at strong coupling.
Shadows of boson and Proca stars with thin accretion disks
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
citation-role summary
background 2
citation-polarity summary
roles
background 2polarities
background 2representative citing papers
Compact boson stars exhibit broader gravitational lensing rings than black holes, resulting in images and visibilities that depend more strongly on the structure of the accretion flow.
Fitting GRAVITY flare astrometry to solitonic boson star models requires masses larger than 4.3 million solar masses, with more diffuse models yielding values closer to the standard black hole mass and thus placing stringent but incomplete constraints on such interpretations of Sgr A*.
Numerical construction of Hayward boson stars shows that frozen states produce Schwarzschild-like shadows with no extra photon rings while non-frozen states show multiple photon rings inside the shadow.
Bayesian analysis shows current near-IR astrometry data cannot distinguish massive boson stars from Schwarzschild black holes for Sgr A*.
Hairy black hole shadows and disks grow with horizon scalar value but can mimic Schwarzschild by adjusting horizon radius, with the potential parameter Lambda constrained by supermassive black hole observations.
citing papers explorer
-
Massive boson stars: Stability and GW emission in head-on mergers
Quartically self-interacting massive boson stars are stable only up to the first mass maximum; their head-on mergers yield a boson-star remnant, a black hole at contact, or two black holes formed before contact, with radiated energy varying non-monotonically at strong coupling.
-
Broadened Lensing Rings of Compact Boson Stars: Enhanced Imprint of Accretion Flow in Images and Visibilities
Compact boson stars exhibit broader gravitational lensing rings than black holes, resulting in images and visibilities that depend more strongly on the structure of the accretion flow.
-
Testing solitonic boson star interpretations of Sagittarius A* with near-infrared flare astrometry
Fitting GRAVITY flare astrometry to solitonic boson star models requires masses larger than 4.3 million solar masses, with more diffuse models yielding values closer to the standard black hole mass and thus placing stringent but incomplete constraints on such interpretations of Sgr A*.
-
Light Rings, Accretion Disks and Shadows of Hayward Boson Stars
Numerical construction of Hayward boson stars shows that frozen states produce Schwarzschild-like shadows with no extra photon rings while non-frozen states show multiple photon rings inside the shadow.
-
Bayesian Analysis of Massive Boson Star Models for Sagittarius A* Using Near-Infrared Astrometry Data
Bayesian analysis shows current near-IR astrometry data cannot distinguish massive boson stars from Schwarzschild black holes for Sgr A*.
-
Shadow of the Scalar Hairy Black Hole with Inverted Higgs Potential
Hairy black hole shadows and disks grow with horizon scalar value but can mimic Schwarzschild by adjusting horizon radius, with the potential parameter Lambda constrained by supermassive black hole observations.