BROAD EMISSION LINES Lα, C IV AND Hβ IN NGC 5548

2003 ◽  
Vol 22 (4-5) ◽  
pp. 681-689
Author(s):  
L. S. Nazarova
Keyword(s):  
Emission Lines ◽  
Broad Emission ◽  
Ngc 5548

scholarly journals Profile variability of the H$\mathsf{\alpha}$ and H$\mathsf{\beta}$ broad emission lines in NGC 5548

2004 ◽  
Vol 422 (3) ◽  
pp. 925-940 ◽  
Author(s):  
A. I. Shapovalova ◽  
V. T. Doroshenko ◽  
N. G. Bochkarev ◽  
A. N. Burenkov ◽  
L. Carrasco ◽  
...  
Keyword(s):  
Emission Lines ◽  
Broad Emission ◽  
Ngc 5548

PROFILE VARIABILITY OF THE Hα AND Hβ BROAD EMISSION LINES IN NGC 5548

2004 ◽  
Author(s):  
A.I. SHAPOVALOVA ◽  
V.T. DOROSHENKO ◽  
N.G. BOCHKAREV ◽  
A.N. BURENKOV ◽  
L. CARRASCO ◽  
...  
Keyword(s):  
Emission Lines ◽  
Broad Emission ◽  
Ngc 5548

scholarly journals A Falling Corona Model for the Anomalous Behavior of the Broad Emission Lines in NGC 5548

2018 ◽  
Vol 857 (2) ◽  
pp. 86 ◽  
Author(s):  
Mouyuan Sun ◽  
Yongquan Xue ◽  
Zhenyi Cai ◽  
Hengxiao Guo
Keyword(s):  
Anomalous Behavior ◽  
Emission Lines ◽  
Broad Emission ◽  
Ngc 5548

scholarly journals Space Telescope and Optical Reverberation Mapping Project. XI. Disk-wind Characteristics and Contributions to the Very Broad Emission Lines of NGC 5548

2020 ◽  
Vol 898 (2) ◽  
pp. 141 ◽  
Author(s):  
M. Dehghanian ◽  
G. J. Ferland ◽  
G. A. Kriss ◽  
B. M. Peterson ◽  
K. T. Korista ◽  
...  
Keyword(s):  
Emission Lines ◽  
Space Telescope ◽  
Disk Wind ◽  
Reverberation Mapping ◽  
Broad Emission ◽  
Wind Characteristics ◽  
Ngc 5548

scholarly journals Space Telescope and Optical Reverberation Mapping Project. IX. Velocity–Delay Maps for Broad Emission Lines in NGC 5548

2021 ◽  
Vol 907 (2) ◽  
pp. 76
Author(s):  
Keith Horne ◽  
G. De Rosa ◽  
B. M. Peterson ◽  
A. J. Barth ◽  
J. Ely ◽  
...  
Keyword(s):  
Emission Lines ◽  
Space Telescope ◽  
Reverberation Mapping ◽  
Broad Emission ◽  
Ngc 5548

scholarly journals Measuring the supermassive black hole parameters with space missions

2006 ◽  
Vol 2 (S238) ◽  
pp. 475-476
Author(s):  
Alexander F. Zakharov
Keyword(s):  
Black Hole ◽  
Spectral Line ◽  
Accretion Disks ◽  
Seyfert Galaxies ◽  
Emission Lines ◽  
X Ray ◽  
Line Shapes ◽  
Supermassive Black Hole ◽  
Broad Emission ◽  
Different Types

AbstractRecent X-ray observations of microquasars and Seyfert galaxies reveal broad emission lines in their spectra, which can arise in the innermost parts of accretion disks. Recently Müller & Camenzind (2004) classified different types of spectral line shapes and described their origin. Zakharov (2006b) clarified their conclusions about an origin of doubled peaked and double horned line shapes in the framework of a radiating annulus model and discussed s possibility to evaluate black hole parameters analyzing spectral line shapes.

scholarly journals The broad line region of AGN: Kinematics and physics

2006 ◽  
pp. 1-11 ◽  
Author(s):  
L.C. Popovic
Keyword(s):  
Electron Temperature ◽  
Accretion Disk ◽  
Emission Lines ◽  
Physical Parameters ◽  
Broad Line ◽  
Physical Conditions ◽  
Broad Line Region ◽  
Broad Emission ◽  
Line Region

In this paper a discussion of kinematics and physics of the Broad Line Region (BLR) is given. The possible physical conditions in the BLR and problems in determination of the physical parameters (electron temperature and density) are considered. Moreover, one analyses the geometry of the BLR and the probability that (at least) a fraction of the radiation in the Broad Emission Lines (BELs) originates from a relativistic accretion disk.

scholarly journals Modeling Line Emission from Disk Winds

2009 ◽  
Vol 5 (S267) ◽  
pp. 398-398
Author(s):  
Patrick B. Hall ◽  
Laura S. Chajet
Keyword(s):  
Emission Line ◽  
Accretion Disk ◽  
Line Emission ◽  
Emission Lines ◽  
Broad Emission

Murray & Chiang (1997) developed a model wherein broad emission lines come from the optically thick base of a rotating, outwardly accelerating wind at the surface of an accretion disk. Photons preferentially escape radially in such a wind, explaining why broad emission lines are usually single-peaked. Less well understood are the observed shifts of emission-line peaks (from 1000 km s−1 redshifted to 2500 km s−1 blueshifted in C iv, with an average 800 km s−1 blueshift).

Sign in / Sign up

Export Citation Format

Share Document