Continuum Energy Distribution of Bright Be Stars

2006 ◽  
Vol 306 (1-2) ◽  
pp. 93-98
Author(s):  
P. S. Goraya
Keyword(s):  
Energy Distribution ◽  
Be Stars ◽  
Continuum Energy

Continuum energy distribution of Be stars

1985 ◽  
Vol 113 (2) ◽  
pp. 325-331 ◽  
Author(s):  
Mahendra Singh
Keyword(s):  
Energy Distribution ◽  
Be Stars ◽  
Continuum Energy

scholarly journals Continuum energy distribution of quasars - Shapes and origins

1989 ◽  
Vol 347 ◽  
pp. 29 ◽  
Author(s):  
D. B. Sanders ◽  
E. S. Phinney ◽  
G. Neugebauer ◽  
B. T. Soifer ◽  
K. Matthews
Keyword(s):  
Energy Distribution ◽  
Continuum Energy

The Continuum Energy Distribution of the Old-Nova GK Per (1901)

1983 ◽  
Vol 72 ◽  
pp. 127-131
Author(s):  
A. Bianchini ◽  
F. Sabbadin
Keyword(s):  
Magnetic Field ◽  
Energy Distribution ◽  
White Dwarf ◽  
Late Type ◽  
X Ray ◽  
Physical Mechanisms ◽  
Continuum Energy ◽  
Field Lines ◽  
The Continuum ◽  
Standard Disc

ABSTRACTThe observed X-ray to IR continuum energy distribution of the old-nova GK Per, corrected for the contribution of the late-type secondary and for i.s. extinction,is found to be consistent with the model of an accreting magnetic white dwarf. Furthermore, we discuss plausible modifications of the standard disc structure caused by the presence of magnetic field lines threading the disc and evaluate the contribution to the observed radiation field from several physical mechanisms.

scholarly journals Infrared Emission from Four be Stars Optical Counterparts of Galactic X-Ray Sources

1982 ◽  
Vol 98 ◽  
pp. 247-251
Author(s):  
P. Persi ◽  
M. Ferrari-Toniolo ◽  
G.L. Grasdalen
Keyword(s):  
Energy Distribution ◽  
Electron Density ◽  
Stellar Wind ◽  
Infrared Emission ◽  
Circumstellar Disk ◽  
Be Stars ◽  
Infrared Excess ◽  
Infrared Observations ◽  
X Ray ◽  
Be Star

Preliminary results of our infrared observations from 2.3 up to 10 and 20 microns of the Be-X-ray stars X Per, γ Cas and HDE 245770, indicate the presence of an ionized circumstellar disk with an electron density law of the type ne ∝ r−3.5. x Per and γ Cas show besides, variable infrared excess at 10μ suggesting variability in the stellar wind. LS I+65°010 presents an anomalous infrared energy distribution for a Be star.

scholarly journals Spectral Energy Distribution (119–685 nm) in 16 Shell Stars and a Tentative Model for Accreting be Stars

1982 ◽  
Vol 98 ◽  
pp. 445-450
Author(s):  
Mirek J. Plavec ◽  
Jan J. Dobias ◽  
Janet L. Weiland ◽  
Remington P.S. Stone
Keyword(s):  
Energy Distribution ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Be Stars ◽  
Line Radiation ◽  
Shell Type ◽  
Tentative Model ◽  
Low Dispersion

I.U.E. low-dispersion spectra and spectral scans made with the Lick Observatory IDS scanners have been combined for 16 shell stars. Eleven objects can be represented by Kurucz model atmospheres, although some of them display strong shell-type line spectra. Five among them are known binaries. The six remaining objects (all interacting binaries) display complex spectra. A model involving continuum and line radiation from a hydrogen cloud surrounding the accreting component is proposed. A generalization of this model with optically thick segments of the cloud promises to explain even more exotic objects such as β Lyrae, W Serpentis and possibly ∊ Aurigae.

scholarly journals Spectral Energy Distribution and Interstellar Reddening (Review Paper)

1987 ◽  
Vol 92 ◽  
pp. 172-191
Author(s):  
L. Houziaux ◽  
J. Manfroid
Keyword(s):  
Energy Distribution ◽  
Flux Distribution ◽  
Review Paper ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Be Stars ◽  
Limited Sample ◽  
Main Current ◽  
Continuous Radiation ◽  
Spectral Ranges

AbstractWe review the recent results on flux distribution of Be stars from 320 to 850nm. It appears that data are available for only 10 to 15 % of the objects recognized as “normal” Be stars. The main current problems appear to be the variability of the continuous radiation, and the correction for interstellar reddening. Various attempts to solve these matters are discussed. We stress the need for fairly high (lnm) resolution spectral scans obtained simultaneously with data in other spectral ranges, repeated at appropriate intervals of time. Such requirements make it necessary to restrict the observing programmes to a limited sample of carefully chosen objects.

Absolute continuum energy distributions in Be stars

1988 ◽  
Vol 148 (1) ◽  
pp. 131-141 ◽  
Author(s):  
N. S. Tur ◽  
P. S. Goraya
Keyword(s):  
Be Stars ◽  
Energy Distributions ◽  
Continuum Energy
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