The Synchrotron Self-absorbed Spectrum of a Spherically Accreting Nuclear Radio Source

Details The Synchrotron Self-absorbed Spectrum of a Spherically Accreting Nuclear Radio Source The Synchrotron Self-absorbed Spectrum of a Spherically Accreting Nuclear Radio Source

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.1503o&link_type=abstract

American Astronomical Society, 186th AAS Meeting, #15.03; Bulletin of the American Astronomical Society, Vol. 27, p.830

Astronomy and Astrophysics

Astronomy

Scientific paper

I consider a scenario in which stellar winds within the dense stellar nucleus are intercepted by the dormant massive black hole (BH) sitting at the galaxian center, and quasi-sperical accretion of the wind onto the BH occurs resulting in acceleration of relativistic electrons to produce the spectrum N(gamma )~ gamma (-p) . Under assumption on equipartition between the local energy density of the magnetic field and that of relativistic electrons, the spectrum of synchrotron radio emission is derived to be alpha =(13+2p)/(22+5p). It ranges between alpha =0.51 to 0.56 for the range of p=3 to 1. The radius of the source is predicted to vary with frequency as r~ nu (m) , where m=-4(4+p)/(22+5p)~ -0.7; the higher the frequency, the more inner parts of the source are seen. Since at radii r nu_0 . Inverse Compton emission offers additional tests of this model in the X-ray energy range. Two different states of accretion, a ``low" and a ``high", depending on the accretion rate dot M, are discussed to predict the variability patterns. This model is applicable to nuclear radio sources in the nuclei of nearby spiral galaxies such as M 81, M 104, etc., which have revealed the presence of a central compact radio source whose prototype in the Milky Way galaxy is Sgr A(star ) . Similarly, in many early-type galaxies, parsec-scale radio cores have been found. The most important common feature of these sources is the inverted radio spectrum S~ nu (alpha ) with alpha =+0.3 to +0.5, which is consistent with the above model. The observed radio spectra enable us to evaluate some important physical parameters of the accreting sources.

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