Torn accretion disks around Kerr black holes erode the inner shadow and create bifurcated, crescent, and multi-ring shadow features driven by sub-disk discontinuities and outer tilt angle.
Shadows of Kerr black holes with and without scalar hair
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
For an observer, the Black Hole (BH) shadow is the BH's apparent image in the sky due to the gravitational lensing of nearby radiation, emitted by an external source. A recent class of solutions dubbed Kerr BHs with scalar hair possess smaller shadows than the corresponding Kerr BHs and, under some conditions, novel exotic shadow shapes can arise. Thus, these hairy BHs could potentially provide new shadow templates for future experiments such as the Event Horizon Telescope. In order to obtain the shadows, the backward ray-tracing algorithm is briefly introduced, followed by numerical examples of shadows of Kerr BHs with scalar hair contrasting with the Kerr analogues. Additionally, an analytical solution for the Kerr shadow is derived in closed form for a ZAMO observer at an arbitrary position.
citation-role summary
background 1
citation-polarity summary
fields
gr-qc 2roles
background 1polarities
background 1representative citing papers
Numerical on-axis scalar scattering cross sections by Kerr-Newman black holes match classical and semiclassical results.
citing papers explorer
-
Reshaping the inner shadow of a Kerr black hole by a torn accretion disk
Torn accretion disks around Kerr black holes erode the inner shadow and create bifurcated, crescent, and multi-ring shadow features driven by sub-disk discontinuities and outer tilt angle.
-
On-axis scattering of scalar fields by charged rotating black holes
Numerical on-axis scalar scattering cross sections by Kerr-Newman black holes match classical and semiclassical results.