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Phase-dependent optical and ultraviolet observations of the old nova V603 AQL (1918).
Drechsel, H.; Krautter, J.; Rahe, J. +1 more
Continuous photometric and ultraviolet spectroscopic observations of the old nova V 603 Aql (1918) were simultaneously carried out with the IUE satellite. Periodic visible light variations with an amplitude of about 0.3 m were discovered, and an orbital period of 3h18.3m was derived. The UV spectroscopy revealed strong variations of the emission l…
Detection of Lyman continuum absorption in the BL Lacertae object PKS0735+178.
Huggins, P. J.; Bregman, J. N.; Glassgold, A. E.
The detection of the Lyman edge in the BL Lac object PKS 0735+178 at the absorption red shift determined by optical measurements leads to a lower limit for the column density of atomic hydrogen, N(H I) not less than 4(17)/sq cm. The Lyman-alpha absorption line appears to have been detected, but only an approximate upper limit can be obtained from …
The abundance of carbon in HU 2-1.
Lutz, J. H.
A logarithmic carbon abundance of 8.61 + or - 0.3 is derived for the planetary nebula Hu 2-1 using data taken with the International Ultraviolet Explorer satellite. This value is close to the logarithmic carbon abundance of 8.67 + or - 0.1, found for the sun by other investigators. The carbon abundance of Hu 2-1 is compared to those of other plane…
Ultraviolet and Optical Observations of HDE245770 / A:0535+26 System during an X-Ray Flare
Giovannelli, F.; Persi, P.; Bartolini, C. +4 more
We present high and low dispersion UV spectra of HDE 245770, which is the optical counterpart of the recurrent transient X-ray pulsar A 0535+26,during a decay of an X-ray flare. UBV photometric measurements and medium dispersion optical spectra were simultaneously obtained. The energy distribution of the star in the 12 10 micron range is compared …
Ultraviolet observations of LMC X-4 and SMC X-1.
Hammerschlag-Hensberge, G.; van der Klis, M.; Willis, A. J. +4 more
Low-resolution IUE spectra of the massive X-ray binaries LMC X-4 and SMC X-1 have been obtained at both short and long wavelengths. The continua are consistent with expected early-type model atmosphere fluxes showing small amounts of reddening and exhibit the characteristic double-wave light curves seen at visible wavelengths.
Presence of MG II emission in R CrB at maximum light.
Kameswara-Rao, N.; Nandy, K.; Bappu, M. K. V.
The high dipersion spectrum of R CrB in the long wavelength obtained near its maximum with the International Ultraviolet Explorer shows the presence of chromospheric Mg II emission. For comparison the spectrum of Gamma Cyg was obtained immediately afterwards. The Mg II emission width of R CrB is found to be the same as that of Gamma Cyg.
UV observations of X-ray sources 2A 0311-227 and 2A 0526-328.
Coe, M. J.; Wickramasinghe, D. T.
IUE satellite observations of the X-ray sources 2A0311-227 and 2A0526-328, which are suspected to be AM Her-type dwarf novae, are reported. Spectra were obtained by the long-wavelength (1900-3200 A) and short-wavelength (110-1900 A) cameras at 10 A resolution over an 8-hr period. The short-wavelength emission lines and continua of 2A0311-227 are f…
Ultraviolet observations of 27 CMa, pi AQR and 48 Lib.
Ringuelet, A. E.; Rovira, M.; Fontenla, J. M.
An analysis of 27 CMa, Pi Aqr, and 48 Lib, Be stars and V/R variables is discussed to determine the physical conditions and the gaseous structure surrounding the stars. On the basis of two different types of absorption lines the narrow and deep, and the broad and shallow profiles, the gaseous structure is divided into two regions: (1) a geometrica…
On a more extended correlation between COS-B gamma rays and interstellar matter in the Orion region
Caraveo, P. A.; Bignami, G. F.; Hermsen, W. +7 more
Analysis of IUE observations of the galactic corona and the existence of molecular clouds in the halo
Hartquist, T. W.; Tallant, A.
IUE observations of ions in the galactic corona are reanalyzed and Savage and de Boer's (1979) conclusion that the detected hot phase has a temperature proportional to 80,000 K is confirmed. The cold phase must be at a temperature of less than 24,000 K and probably contains substantial amounts of molecular material. Molecules, such as CH(+), OH an…