Other
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.4816b&link_type=abstract
American Astronomical Society, 201st AAS Meeting, #48.16; Bulletin of the American Astronomical Society, Vol. 34, p.1182
Other
Scientific paper
Ionized reflection has often been considered as the explanation for the unusual Fe Kα line variability observed in MCG--6-30-15. In this paper, we present ionized reflection fits to a 325 ks observation of MCG--6-30-15 by XMM-Newton and BeppoSAX to test this model. The data are fit between 2.5 and 80 keV using the constant density models of Ross & Fabian. Our best fit model requires the Fe Kα line to be split into two reprocessing events: one from the inner disc to build up the red wing, and the other from more distant material to fit the blue horn. A good fit was obtained with a solar abundance of iron and a reflection fraction (R) of one for the inner reflector. However, the combination of the two reflection spectra mimics one with R>2 as required by the BeppoSAX data. The inner reflector is ionized with log ξ =3.8, and the outer reflector is neutral. The distant reflector has an inner radius of 71 gravitational radii (rg) which corresponds to a light crossing time of about an hour for a 107 Msun black hole. Thus, the double reflector model can explain many of the Fe Kα variability characteristics previously observed in MCG--6-30-15. However, the ionized reflection spectrum from the inner component, which contributes 94% of the 2--10 keV flux, is constrained to arise from a narrow annulus between 4.93 and 5.01 rg. This is extremely difficult to produce without resorting to other energy sources such as the black hole spin.
Ballantyne David R.
Fabian Andrea C.
Vaughan Stewart
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