Search for CO absorption bands in IUE far-ultraviolet spectra of cool stars

1994 ◽  
Vol 107 ◽  
pp. 747 ◽  
Author(s):  
S. E. Gessner ◽  
K. G. Carpenter ◽  
R. D. Robinson
1973 ◽  
Vol 78 (1) ◽  
pp. 258-264 ◽  
Author(s):  
G. J. Rottman ◽  
P. D. Feldman ◽  
H. W. Moos

2004 ◽  
Vol 607 (1) ◽  
pp. 369-383 ◽  
Author(s):  
Gregory J. Herczeg ◽  
Brian E. Wood ◽  
Jeffrey L. Linsky ◽  
Jeff A. Valenti ◽  
Christopher M. Johns‐Krull

1969 ◽  
Vol 3 (8) ◽  
pp. 649-651 ◽  
Author(s):  
G. Bélanger ◽  
P. Sauvageau ◽  
C. Sandorfy

1996 ◽  
Vol 463 ◽  
pp. 110 ◽  
Author(s):  
David A. Turnshek ◽  
Michael, Jr. Kopko ◽  
Eric Monier ◽  
Donette Noll ◽  
Brian R. Espey ◽  
...  

2001 ◽  
Vol 552 (1) ◽  
pp. 278-288 ◽  
Author(s):  
Carmen Morales ◽  
Veronica Orozco ◽  
Jose F. Gomez ◽  
Joaquin Trapero ◽  
Antonio Talavera ◽  
...  

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.


1986 ◽  
Vol 141 ◽  
pp. 1-12 ◽  
Author(s):  
C. Sandorfy ◽  
L.S. Lussier ◽  
G. Richer ◽  
A. Goursot ◽  
E. Pénigault ◽  
...  

2004 ◽  
Vol 219 ◽  
pp. 623-634 ◽  
Author(s):  
A. K. Dupree

Recent spectroscopic results from the far ultraviolet and X-ray region coupled with infrared observations demonstrate that winds from luminous stars can be warm (300000K) and fast (speeds of several hundred km s—1) linking the hot solar wind to the cool, massive winds of luminous M-type supergiant stars. Hot coronal material (T ∼107 K) appears to be confined near the star, and not expanding in the wind. These new spectra enable a comprehensive picture to be constructed of the presence and character of winds in cool stars.


1968 ◽  
Vol 1 (12) ◽  
pp. 595-596 ◽  
Author(s):  
Y. Harada ◽  
J.N. Murrell ◽  
H.H. Sheena

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