Other
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...381..418z&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 381, Nov. 10, 1991, p. 418-425.
Other
81
Active Galactic Nuclei, Galactic Structure, Radio Galaxies, Accretion Disks, Astronomical Models, H Lines
Scientific paper
A comparison of the H-alpha and H-beta profiles of the radio galaxy 3C 390.3 at different epochs shows that the H-beta/H-alpha ratio is significantly higher in the line 'humps' than in the rest of the profiles. No humps are found in the Ly-alpha profile, although Ly-alpha is as broad as the Balmer lines. Therefore, the profile humps are probably produced in a region of higher density. A double-stream model fitted to the H-alpha profiles requires that the conical structure is close to the line of sight and subtends a large angle (not less than 60 deg) and a limited radial distance (Rmax/Rmin not greater than 10). The pair of humps in the profile may arise from gas lumps or a narrow stream inside the cone. Fluctuations in the blue-to-red hump flux ratio may be due to variations in the relative intensity of the ionizing continuum in the two cones or to changes in the orientation of these cones. Another model is a disk with a corotating enhanced emission region ('hot patch'). With a significant angular size (about 90 deg), such a region would contribute a time-dependent emission component which migrates between the two humps and changes their relative intensity.
Grandi Steven A.
Veilleux Sylvain
Zheng Wei
No associations
LandOfFree
3C 390.3 - Modeling variable profile humps 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 3C 390.3 - Modeling variable profile humps, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and 3C 390.3 - Modeling variable profile humps will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1716782