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IUE observations of the symbiotic star CH Cygni during an active phase
Hack, M.
THE spectrum of CH Cygni usually has the appearance of a normal M6 III star, but at intervals of several years, it has outbursts during which it shows the characteristics of a symbiotic star, that is a blue continuum extending shortward of the B almer discontinuity, and emission lines of He I, Fe II, [Fe II], [S II], [O III]; the Balmer lines and …
The ultraviolet spectrum of LSI +61 303.
Hutchings, J. B.
IUE spectroscopy is presented of the radio variable emission-line star LSI +61°303, which may also be a source of X and γ rays. The UV continuum is complex and dues nut fit a single stellar model or power law. The UV flux and line spectrum suggest the primary is a mass-losing Ib supergiant but all possibilities involve some peculiarities compared …
Gamma rays from the Cygnus region and the nature of CG 78+1.
Strong, A. W.; Wolfendale, A. W.; Protheroe, R. J.
Interpretation of the galactic gamma-ray flux above 100 MeV has been complicated by the presence of a component due to 'point' sources of gamma-rays and by the lack of measurements of the molecular hydrogen (except along the galactic equator) which forms a large fraction of the interstellar medium (ISM). Recent CO observations of the Cygnus X regi…
The UV spectrum of VV Cep in 1978.
Faraggiana, R.; Selvelli, P. L.
VV Cep spectra taken by IUE in June and July 1978 are examined. At this initial phase of the chromospheric eclipse following the totality of the 1977 eclipse, the chromospheric line spectrum is well developed in the region 2500-3000 A, superimposed on the spectrum of the hot companion. The flux distribution derived from the low-resolution and larg…
IUE spectra of the massive close binary V382 Cygni.
Koch, R. H.; Siah, M. J.; Fanelli, M. N.
The massive close binary, V382 Cyg, was observed with the low-dispersion spectrograph on the IUE satellite. The dereddened spectrum can be reasonably represented by a 40,000-K model atmosphere. The spectra show interstellar, photospheric, and shell absorption blends and one shell emission feature. From one of the shell absorptions, it is possible …
IUE observations of an active region of HD206860
Blanco, C.; Catalano, S.; Marilli, E.
THE chromospheric Mg II h and k lines seem to have doubly reversed emission core in the spectra of the Sun and of solar and late type stars. In the solar spectrum the general appearance of Mg II h and k is very similar to the H and K of Ca II, but with larger intensity fluctuations. Current ideas suggest that the h and k lines are strongly sensiti…
Ultraviolet P Cygni profiles of the C IV resonance line for O-type stars in the open cluster IC 1805.
Burki, G.; de Andres, F. L.
The ultraviolet C IV resonance lines of seven O-type stars in IC 1805 were observed with the IUE satellite in the low dispersion mode in the 1150-1950 A and 1900-3200 A wavelength ranges. The spectra showed very large and deep P Cygni profiles of the C IV resonance doublet at 1548.20 A and 1550.77 A, and P Cygni characteristics increased with bolo…
The ultraviolet spectrum of the hot halo star Feige 86.
Hack, M.
The ultraviolet spectrum of the hot halo star Feige 86 has been observed with IUE in the low-resolution mode. The energy distribution gives an effective temperature of 18000 K, in agreement with the value previously derived by Baschek and Sargent (1976) from the visual spectrum. Comparison of the line spectrum with those of two standard stars havi…
Mg II and Ca II emissions from three G dwarfs.
Rego, M.; Fernandez-Figueroa, M. J.
The stars Eta Cet, Beta CnV, and Beta Com have been observed from the ground and the IUE satellite. The Ca II and Mg II K emission line intensities have been compared and show a correlation. The full widths at the base (FWB) corresponding to the Mg II K emission are in the dispersion band of the luminosity-FWB relationship.
A geometrical analysis of the gamma-ray light curves of pulsars.
Massaro, E.; Buccheri, R.; Salvati, M.
In the light curves of the COS-B gamma-ray pulsars, some common features are clearly recognizable; two main peaks always occur, and the intervening phase lag has not the natural value of 0.5. An interpretation is proposed which only involves a simplified geometrical description of the emission pattern, viz. two opposite hollow cones with a first-o…