What is the Accretion Rate in NGC 4258?

Abstract

We consider the implications of recent infrared and radio observations of the nucleus of NGC 4258. There is no direct evidence that the nucleus has been steadily accreting on the viscous timescale of the outer masing disk, which is >~ 10^9 \yr. Thus the mass accretion rate in the outer disk need not be the same as in the inner accretion flow where most of the gravitational binding energy is released. We show that an advection-dominated flow model with a transition radius of \sim (10-100) M (where M is the mass of the hole) and \mdot \approx 10^{-2}\msun \yr^{-1} is consistent with the observed spectrum from radio to X-rays. We also show that a thin (flat or warped) disk can fit the observed fluxes outside the X-ray band. The X-rays can be explained by means of a corona in such a model, but the absence of radio emission from the location of the putative central black hole provides a serious constraint on the properties of the corona. A wide range of accretion rates, 10^{-4} <~ \mdot <~ 10^{-2} \msun\yr^{-1}, can be made to fit the data, but the most ``natural&#39;&#39; models have 10^{-3} <~ \mdot <~ 10^{-2} \msun\yr^{-1}. Physical conditions in the observed VLBI jet features can also be related to conditions in the inner accretion flow. We conclude with a list of future observations that might help to constrain the accretion rate.