REVIEW 5 cited by
A Model for the X-Ray and UV Emission from Seyfert Galaxies and Galactic Black Holes
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
A Model for the X-Ray and UV Emission from Seyfert Galaxies and Galactic Black Holes
read the original abstract
We propose that the X--ray emission from radio quiet AGN and galactic black holes is due to Comptonization of soft thermal photons emitted by the underlying accretion disk in localized structures (blobs). The power per unit area produced by the blobs, impinging on the disk, can easily dominate the radiation internally produced by the disk. In this case the electron temperature and the high energy spectrum can be determined in a similar way as in the previously studied homogeneous model (Haardt \& Maraschi 1991). However in the present model: a) the emitted spectrum is largely independent of the {\it fraction} of gravitational power dissipated in the blobs; b) the X--ray spectrum can be harder depending on a form factor of the blobs; c) the UV (or soft X--ray for galactic objects) luminosity that is not intercepted by the blobs can be larger than the X--ray luminosity. In the framework of a simplified accretion disk $\alpha-\Omega$ dynamo model, we make order of magnitude estimates of the number of active blobs, their size, luminosity and hence their compactness, finding values in agreement with what is observed. The expected UV to X--ray spectra and correlations of X--ray and UV light curves are discussed.
Forward citations
Cited by 5 Pith papers
-
Comprehensive X-ray Study of Giant Radio Galaxies with XMM-Newton and Chandra
A systematic X-ray spectral analysis of 27 giant radio galaxies finds ~44% absorbed nuclei, Fe Kα lines, and hard photon indices, with tentative links to black hole mass.
-
AGNFormer I: Reconstruction of AGN spectra using a probabilistic transformer model
An uncertainty-aware transformer reconstructs masked AGN broad lines and spectral halves with 4-16% flux errors and beats eleven purpose-built Lyα-reconstruction algorithms on a blind benchmark.
-
Physically motivated AGN emissivity profiles and their effects on quasar microlensing signatures. 1. Multi-epoch accretion disc size inference
Interpreting composite disc-plus-BLR emission as a single compact disc systematically overestimates microlensing half-light radii, with the bias set mainly by the BLR flux fraction and the compact-disc emissivity shape.
-
HALO II: Constraining Hubble constant $H_{0}$ through continuum delay fitting of Fairall 9
Using simultaneous modeling of continuum lag-spectrum and broadband SED of Fairall 9 with the H0RIZON-AGN model, the authors obtain H0 = 72.4_{-3.7}^{+3.4} km s^{-1} Mpc^{-1}.
-
X-ray disc reverberation modelling of the X-ray/UV/optical spectral/timing properties of Fairall 9
X-ray reprocessing by the accretion disc in Fairall 9 simultaneously explains the SED, UV/optical power spectra, and interband time lags only if the corona is powered externally rather than by accretion.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.