Physics
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21642002f&link_type=abstract
American Astronomical Society, AAS Meeting #216, #420.02; Bulletin of the American Astronomical Society, Vol. 41, p.831
Physics
Scientific paper
Observations have cumulatively revealed the presence of blueshifted absorption features from various astrophysical objects hosting central black holes (i.e. Seyferts, quasars, galactic black holes). These are thought to be the result of absorption by specific ionic species of a wind/outflow of relatively high column density in our line of sight (LoS). Chandra/XMM-Newton observations have indicated that the spectra of Seyfert 1 galaxies appear to exhibit a roughly constant absorption measure distribution (AMD) - i.e. global column distribution over a wide range of ionization parameter - in their spectra. This implies that the density profile of the putative absorbers should scale as n 1/r along the LoS. Further analysis also indicates that the outflow velocity depends also on the ionization of a specific ion. Thus, the moderately ionized Fe (Fe XVII) typically shows a blueshift of a few hundred km/sec while He-like Fe (Fe XXV) tends to show a few thousand km/sec. Recently we have modeled the UV/X-ray absorbers in the context of hydromagnetic accretion-disk wind, presumably ubiquitous amongst these objects, with particular emphasis on their observational signatures (including the AMD data) as well as the theoretical implications. To this end we employ steady-state, axisymmetric, self-similar magnetohydrodynamical (MHD) disk-wind model to simulate the two-dimensional structure of these winds, followed by radiative transfer calculations using the photoionization code XSTAR, in order to determine their detailed ionization structure along the observer's LoS. Our calculations show, under typical boundary conditions for AGNs, that the observations (including AMD) of several AGNs are well explained by this model (IRAS13349+2438,MCG-6-30-15,NGC3783/5548/7469). Furthermore, this model can account for high-velocity UV/X-ray absorbers (v/c 0.04-0.6) of high column recently reported in certain quasar populations (e.g. APM08279+5255). We will overview the "physics of absorbers from the perspective of MHD disk-wind” based on the previous UV/X-ray observations.
Behar Ehud
Contopoulos Ioannis
Fukumura Keigo
Kazanas Demos
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