The Extreme‐Ultraviolet Emission of the Seyfert Galaxies Markarian 279, Markarian 478, and Ton S180

1997 ◽  
Vol 475 (2) ◽  
pp. 552-556 ◽  
Author(s):  
Chorng‐Yuan Hwang ◽  
Stuart Bowyer
2007 ◽  
Vol 91 (23) ◽  
pp. 231501 ◽  
Author(s):  
Yoshifumi Ueno ◽  
Georg Soumagne ◽  
Akira Sumitani ◽  
Akira Endo ◽  
Takeshi Higashiguchi

Science ◽  
1996 ◽  
Vol 274 (5291) ◽  
pp. 1335-1338 ◽  
Author(s):  
R. Lieu ◽  
J. P. D. Mittaz ◽  
S. Bowyer ◽  
J. O. Breen ◽  
F. J. Lockman ◽  
...  

2019 ◽  
Vol 21 (4) ◽  
pp. 045001
Author(s):  
Shiquan CAO ◽  
Maogen SU ◽  
Qi MIN ◽  
Duixiong SUN ◽  
Lei WU ◽  
...  

2000 ◽  
Vol 545 (2) ◽  
pp. 695-700 ◽  
Author(s):  
Thomas W. Berghofer ◽  
Stuart Bowyer ◽  
Eric Korpela

Comets II ◽  
2004 ◽  
pp. 631-644
Author(s):  
C. M. Lisse ◽  
T. E. Cravens ◽  
K. Dennerl

1996 ◽  
Vol 152 ◽  
pp. 309-316
Author(s):  
Frits Paerels ◽  
Min Young Hur ◽  
Christopher W. Mauche

A longstanding problem in the interpretation of the X-ray and extreme ultraviolet emission from strongly magnetic cataclysmic variables can be addressed definitively with high resolution EUV spectroscopy. A detailed photospheric spectrum of the accretion-heated polar cap of the white dwarf is sensitive in principle to the temperature structure of the atmosphere. This may allow us to determine where and how the bulk of the accretion energy is thermalized. The EUVE data on AM Herculis and EF Eridani are presented and discussed in this context.


1996 ◽  
Vol 152 ◽  
pp. 27-36
Author(s):  
Arieh Königl

EUV observations could provide valuable and unique information about the nature of active galactic nuclei. I discuss their potential usefulness and review some of the main results obtained so far with the ROSAT WFC and the EUVE instruments. About three dozen sources, mostly Seyfert galaxies and BL Lacertae objects, have already been identified, and spectroscopic measurements of several of them have yielded a number of surprises. However, more observations are clearly needed to confirm some of the reported spectral features and to validate their interpretation.


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