Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...454l.105m&link_type=abstract
Astrophysical Journal Letters v.454, p.L105
Astronomy and Astrophysics
Astronomy
103
Galaxies: Seyfert, Galaxies: Quasars: Absorption Lines
Scientific paper
The broad (10--30,000 km s-1) UV absorption lines seen in some quasars can form in a radiatively driven wind. The driving operates on UV resonance lines of moderately ionized metals and is efficient at high velocity because the wind shields itself from soft X-rays emitted by the central source. This shielding is a natural consequence of the high-ionization parameter U = n gamma /n ~ 10 and column (1023 cm-2) at the inner edge of the wind. Compared to radio-quiet quasars, both radio-loud quasars and Seyfert nuclei are strong X-ray emitters (relative to their UV emission), so their winds are less well shielded. This tends to limit the width of blueshifted absorption in UV resonance lines such as C IV. This effect is enhanced in Seyferts by the lower wind column densities (1022 cm-2), a result of their lower luminosity. We predict that active galactic nuclei with intrinsic, broad (>~ 500 km s-1) blueshifted absorption in C IV will also have absorption edges near 1 keV due to O VII and/or O VIII. Objects with very broad C IV absorption (>~ 5000 km s-1) will be strongly absorbed at 1 keV and will also have Fe absorption edges. We suggest that the gas at the inner edge of the wind should be identified with the "warm absorber" found in objects showing blueshifted absorption in UV resonance lines.
Chiang James
Murray Nathan
No associations
LandOfFree
Active Galactic Nuclei Disk Winds, Absorption Lines, and Warm Absorbers does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Active Galactic Nuclei Disk Winds, Absorption Lines, and Warm Absorbers, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Active Galactic Nuclei Disk Winds, Absorption Lines, and Warm Absorbers will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1258024