Relativistic Electron Energy Spectra of Active Galactic Nuclei in the Thin Synchrotron Limit. I. The Method

1995 ◽  
Vol 447 ◽  
pp. 505 ◽  
Author(s):  
Luis Salas ◽  
Irene Cruz-Gonzalez ◽  
Luis Carrasco
Keyword(s):  
Active Galactic Nuclei ◽  
Relativistic Electron ◽  
Electron Energy ◽  
Galactic Nuclei ◽  
Energy Spectra

High‐Energy Spectra of Active Galactic Nuclei. II. Absorption in Seyfert Galaxies

1997 ◽  
Vol 113 (2) ◽  
pp. 311-331 ◽  
Author(s):  
A. Malizia ◽  
L. Bassani ◽  
J. B. Stephen ◽  
G. Malaguti ◽  
G. G. C. Palumbo
Keyword(s):  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Seyfert Galaxies ◽  
High Energy ◽  
Energy Spectra

scholarly journals Relativistic Neutrons in Active Galactic Nuclei

1989 ◽  
Vol 134 ◽  
pp. 215-216
Author(s):  
Marek Sikora ◽  
Bronisław Rudak ◽  
Mitchell Begelman
Keyword(s):  
Active Galactic Nuclei ◽  
Electron Energy ◽  
Active Galactic Nucleus ◽  
Galactic Nuclei ◽  
Substantial Fraction ◽  
Proton Proton ◽  
Proton Collisions ◽  
Central Engine ◽  
Proton Proton Collisions

A substantial fraction of the radiation from an active galactic nucleus (AGN) is apparently nonthermal in origin, and is probably produced by ultrarelativistic electrons. How much energy goes into relativistic protons is uncertain, but it is likely to be comparable to the electron energy or larger. Indeed, several authors (Sikora et al. 1987; Kazanas and Ellison 1986; Zdziarski 1986) have shown that proton-photon and proton-proton collisions can be efficient sources of relativistic pairs in the central engine of an AGN. Thus it is not necessary for electrons to be accelerated directly in AGNs, provided that protons are accelerated with high enough efficiency.

scholarly journals EGRET High-Energy Gamma-ray Observations of AGN: Energy Spectra and Time Variability

1994 ◽  
Vol 159 ◽  
pp. 49-52 ◽  
Author(s):  
D.J. Thompson ◽  
D.L. Bertsch ◽  
B.L. Dingus ◽  
J. A. Esposito ◽  
C.E. Fichtel ◽  
...  
Keyword(s):  
Active Galactic Nuclei ◽  
Gamma Ray ◽  
Galactic Nuclei ◽  
High Energy ◽  
Energy Spectra ◽  
Time Variability ◽  
High Energy Gamma ◽  
Energy Gamma

The Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory has detected more than 20 Active Galactic Nuclei (AGN) at photon energies above 30 MeV.

scholarly journals Physical Conditions in Active Galactic Nuclei

1989 ◽  
Vol 134 ◽  
pp. 535-536
Author(s):  
V. S. Artyukh
Keyword(s):  
Magnetic Field ◽  
Synchrotron Radiation ◽  
Active Galactic Nuclei ◽  
Relativistic Electron ◽  
Angular Resolution ◽  
Low Frequency ◽  
Galactic Nuclei ◽  
Radio Sources ◽  
Electron Number ◽  
Physical Conditions

Self-absorption of synchrotron radiation in compact radio sources gives rise to a low-frequency cutoff in their spectra. To study this effect it is necessary to observe the radio sources at meter wavelengths with angular resolution < 1″. Such observations of compact radio sources located in active galactic nuclei lead to estimates of magnetic field strengths and relativistic electron number densities in the AGNs.

scholarly journals Origin of Radio Emission from Nonthermal Electrons in ADAF for LLAGNs

2012 ◽  
Vol 8 (S290) ◽  
pp. 341-342
Author(s):  
H. Liu ◽  
Q. W. Wu
Keyword(s):  
Steady State ◽  
Radio Emission ◽  
Active Galactic Nuclei ◽  
Electron Energy ◽  
Galactic Nuclei ◽  
Electron Population ◽  
Nonthermal Electrons ◽  
State Electron

AbstractWe explore the origin of the radio emission from the low-luminosity active galactic nuclei (LLAGNs), by investigating the ADAF model with a hybrid of thermal and nonthermal electrons. We find that the radio emission of LLAGNs is severely underpredicted by pure ADAF model, and can be naturally explained by the ADAF model with a hybrid electron population. Our model can roughly reproduce the anti-correlation between the mass-corrected radio loudness and the Eddington ratio for the LLAGNs. We further model the SEDs of each source, and find that roughly all sources can be well fitted if a small fraction of the steady state electron energy is ejected into the nonthermal electrons.

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