scholarly journals High‐Resolution Ultraviolet Spectra of the Dwarf Seyfert 1 Galaxy NGC 4395: Evidence for Intrinsic Absorption

2004 ◽  
Vol 612 (1) ◽  
pp. 152-158 ◽  
Author(s):  
D. M. Crenshaw ◽  
S. B. Kraemer ◽  
J. R. Gabel ◽  
H. R. Schmitt ◽  
A. V. Filippenko ◽  
...  
2001 ◽  
Vol 557 (1) ◽  
pp. 2-17 ◽  
Author(s):  
M. J. Collinge ◽  
W. N. Brandt ◽  
Shai Kaspi ◽  
D. Michael Crenshaw ◽  
Martin Elvis ◽  
...  

1980 ◽  
Vol 88 ◽  
pp. 237-241
Author(s):  
Yoji Kondo ◽  
George E. McCluskey ◽  
Robert E. Stencel

The eclipsing binary U Cephei has proven to be of great interest in the study of stellar evolution in close binary systems. Batten (1974), Hall and Walter (1974), Rhombs and Fix (1976), Markworth (1977), and Olson (1978), among others, have recently reported on their intensive ground based studies of U Cephei. Kondo, McCluskey and Wu (1978) have investigated the ultraviolet light curves of U Cephei obtained with Astronomical Netherlands Satellite (ANS). Kondo, McCluskey and Stencel (1979) have discussed the International Ultraviolet Explorer (IUE) spectra of U Cephei. This paper discusses results incorporating additional IUE high resolution spectra of U Cephei obtained in both far-ultraviolet and mid-ultraviolet spectral regions.


1996 ◽  
Vol 53 (1) ◽  
pp. 122-125 ◽  
Author(s):  
Hidetsuka Imajo ◽  
Kazuhiro Hayasaka ◽  
Ryuzo Ohmukai ◽  
Utako Tanaka ◽  
Masayoshi Watanabe ◽  
...  

1988 ◽  
Vol 102 ◽  
pp. 383-386
Author(s):  
B. Boer ◽  
C. de Jager ◽  
H. Nieuwenhuijzen

AbstractIn order to study the apparent near instability of supergiant atmospheres high-resolution (λ/Δ λ = 8×104) BUSS (Balloon-borne Ultraviolet Stellar Spectrometer) spectra of the supergiant Alpha Cyg have been investigated. Equivalent widths of lines yield the variation of the line-of-sight microturbulent velocity component ζµwith optical depth τ. We find at τ5= 0.1: ζµequal to the velocity of sound. The consequent turbulent acceleration is directed outward, it increases outward and is about half the effective acceleration at τ5= 0.01. The macroturbulent velocity profile is double peaked with up- and downward velocities of 14 km s−1. We suggest that these motions are stochastic pulsations of large elements. At any time there are 30 to 40 such elements on the visible disk.


1991 ◽  
Vol 377 ◽  
pp. L25 ◽  
Author(s):  
J. B. Hutchings ◽  
F. Bruhweiler ◽  
A. Boggess ◽  
S. R. Heap ◽  
D. Ebbets ◽  
...  

1999 ◽  
Vol 516 (2) ◽  
pp. 750-768 ◽  
Author(s):  
D. Michael Crenshaw ◽  
Steven B. Kraemer ◽  
Albert Boggess ◽  
Stephen P. Maran ◽  
Richard F. Mushotzky ◽  
...  

2013 ◽  
Vol 435 (2) ◽  
pp. 1233-1264 ◽  
Author(s):  
Rajib Ganguly ◽  
Ryan S. Lynch ◽  
Jane C. Charlton ◽  
Michael Eracleous ◽  
Todd M. Tripp ◽  
...  

1997 ◽  
Vol 478 (1) ◽  
pp. 80-86 ◽  
Author(s):  
Fred Hamann ◽  
Thomas A. Barlow ◽  
Vesa Junkkarinen ◽  
E. M. Burbidge

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