What are the emission line filaments along the radio axis of Centaurus A?

2005 ◽  
pp. 87-91
Author(s):  
R. Morganti ◽  
C. N. Tadhunter ◽  
R. A. E. Fosbury ◽  
D. Malin
Keyword(s):  
Emission Line ◽  
Centaurus A

scholarly journals Emission Lines: Sign of a New Energy Source?

1982 ◽  
Vol 97 ◽  
pp. 69-70
Author(s):  
David S. De Young
Keyword(s):  
Energy Source ◽  
Interstellar Medium ◽  
Emission Line ◽  
Emission Lines ◽  
Class I ◽  
Radio Sources ◽  
Extended Radio ◽  
New Energy ◽  
Centaurus A

In addition to the occurrence of emission line regions coexistent with extended radio sources which have been discussed at this Symposium, this phenomenon has been observed earlier in 3C277.3 (Miley et al. 1981) and in Centaurus A (Graham and Price 1981). This gas has been detected only in the Fanaroff and Riley “Class I” radio sources. Data concerning this class of object suggest that outflow from the nucleus is proceeding at transonic or subsonic speeds and this correlation has led to the suggestion (De Young 1981) that the origin of the emission line gas arises from entrainment of the interstellar medium into the ejected material.

scholarly journals Taurus Observations of the Emission-Line Velocity Field of Centaurus A (NGC 5128)

1983 ◽  
Vol 100 ◽  
pp. 331-334
Author(s):  
Keith Taylor ◽  
Paul D. Atherton
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Spatial Resolution ◽  
Line Material ◽  
Fabry Perot ◽  
Dark Lane ◽  
Centaurus A

Using TAURUS – an Imaging Fabry Perot system in conjunction with the IPCS on the AAT, we have studied the velocity field of the Ha emission line at a spatial resolution of 1.7″ over the dark lane structure of Centaurus A. The derived velocity field is quite symmetrical and strongly suggests that the emission line material is orbiting the elliptical component, as a warped disc.

The Emission-line Filaments in Centaurus A

1991 ◽  
Vol 9 (1) ◽  
pp. 93-94 ◽  
Author(s):  
G. V. Bicknell
Keyword(s):  
Emission Line ◽  
Radio Source ◽  
Active Galaxies ◽  
Narrow Line ◽  
Extended Emission ◽  
Centaurus A

AbstractThis paper examines recent investigations of emission-line filaments along the edge of the radio source in Centaurus A. It shows how these studies have ramifications for the excitation of the narrow line regions and extended emission-line regions of other active galaxies.

Shock excitation of the emission-line filaments in Centaurus A

1993 ◽  
Vol 414 ◽  
pp. 510 ◽  
Author(s):  
Ralph S. Sutherland ◽  
Geoffrey V. Bicknell ◽  
Michael A. Dopita
Keyword(s):  
Emission Line ◽  
Shock Excitation ◽  
Centaurus A

FeXIV Line Emission Polarization of the July 11, 1991 Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 541-547
Author(s):  
J. Sýkora ◽  
J. Rybák ◽  
P. Ambrož
Keyword(s):  
High Resolution ◽  
Solar Corona ◽  
Emission Line ◽  
Solar Eclipse ◽  
White Light ◽  
Preliminary Analysis ◽  
Line Emission ◽  
Total Solar Eclipse ◽  
Degree Of Polarization ◽  
High Resolution Images

AbstractHigh resolution images, obtained during July 11, 1991 total solar eclipse, allowed us to estimate the degree of solar corona polarization in the light of FeXIV 530.3 nm emission line and in the white light, as well. Very preliminary analysis reveals remarkable differences in the degree of polarization for both sets of data, particularly as for level of polarization and its distribution around the Sun’s limb.

Structuring, Motions and Shapes of Corona Emission Line Profiles

1994 ◽  
Vol 144 ◽  
pp. 421-426
Author(s):  
N. F. Tyagun
Keyword(s):  
Emission Line ◽  
Filling Factor ◽  
Direct Relationship ◽  
Coronal Plasma ◽  
Line Of Sight ◽  
Line Profiles ◽  
The Difference ◽  
Yellow Line ◽  
Red Line

AbstractThe interrelationship of half-widths and intensities for the red, green and yellow lines is considered. This is a direct relationship for the green and yellow line and an inverse one for the red line. The difference in the relationships of half-widths and intensities for different lines appears to be due to substantially dissimilar structuring and to a set of line-of-sight motions in ”hot“ and ”cold“ corona regions.When diagnosing the coronal plasma, one cannot neglect the filling factor - each line has such a factor of its own.

White-Light Coronal Structures: Streamers and CMEs

1994 ◽  
Vol 144 ◽  
pp. 82
Author(s):  
E. Hildner
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
White Light ◽  
Coronal Mass Ejections ◽  
X Rays ◽  
Solar Cycles ◽  
Temperature Function ◽  
X Ray ◽  
Eclipse Observations ◽  
Coronal Structures

AbstractOver the last twenty years, orbiting coronagraphs have vastly increased the amount of observational material for the whitelight corona. Spanning almost two solar cycles, and augmented by ground-based K-coronameter, emission-line, and eclipse observations, these data allow us to assess,inter alia: the typical and atypical behavior of the corona; how the corona evolves on time scales from minutes to a decade; and (in some respects) the relation between photospheric, coronal, and interplanetary features. This talk will review recent results on these three topics. A remark or two will attempt to relate the whitelight corona between 1.5 and 6 R⊙to the corona seen at lower altitudes in soft X-rays (e.g., with Yohkoh). The whitelight emission depends only on integrated electron density independent of temperature, whereas the soft X-ray emission depends upon the integral of electron density squared times a temperature function. The properties of coronal mass ejections (CMEs) will be reviewed briefly and their relationships to other solar and interplanetary phenomena will be noted.

THEORETICAL ELECTRON DENSITY AND TEMPERATURE SENSITIVE EMISSION LINE RATIOS FOR HELIUM-LIKE Si XIII COMPARED TO DITE TOKAMAK OBSERVATIONS

1989 ◽  
Vol 50 (C1) ◽  
pp. C1-559-C1-564
Author(s):  
F. P. KEENAN ◽  
R. BARNSLEY ◽  
J. DUNN ◽  
K. D. EVANS ◽  
S. M. McCANN ◽  
...  
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Temperature Sensitive ◽  
Electron Density And Temperature
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