OAO-2 and Mariner 9 Ultraviolet Observations of δ Persei

1973 ◽  
Vol 85 ◽  
pp. 307
Author(s):  
Michael R. Molnar
Keyword(s):  
Ultraviolet Observations ◽  
Mariner 9

Complex refractive index of Martian dust: Mariner 9 ultraviolet observations

Icarus ◽  
1976 ◽  
Vol 27 (1) ◽  
pp. 55-67 ◽  
Author(s):  
Kevin Pang ◽  
Joseph M. Ajello ◽  
Charles W. Hord ◽  
Walter G. Egan
Keyword(s):  
Refractive Index ◽  
Complex Refractive Index ◽  
Ultraviolet Observations ◽  
Mariner 9

Ultraviolet Observations of the Powering Source of the Supergiant Shell in IC 2574

2000 ◽  
Vol 120 (4) ◽  
pp. 1794-1800 ◽  
Author(s):  
Susan G. Stewart ◽  
Fabian Walter
Keyword(s):  
Ultraviolet Observations

scholarly journals Mars: Mariner 9 Spectroscopic Evidence for H2O Ice Clouds

Science ◽  
1973 ◽  
Vol 182 (4110) ◽  
pp. 381-383 ◽  
Author(s):  
R. J. Curran ◽  
B. J. Conrath ◽  
R. A. Hanel ◽  
V. G. Kunde ◽  
J. C. Pearl
Keyword(s):  
Ice Clouds ◽  
Spectroscopic Evidence ◽  
Mariner 9

Viewing Phobos and Deimos for Navigating Mariner 9

1974 ◽  
Vol 11 (4) ◽  
pp. 215-222 ◽  
Author(s):  
T. C. DUXBURY ◽  
G. H. BORN ◽  
N. JERATH
Keyword(s):  
Mariner 9

scholarly journals ULTRAVIOLET OBSERVATIONS OF SUPERNOVAE

2007 ◽  
Author(s):  
Nino Panagia ◽  
Stefan Immler ◽  
Kurt Weiler
Keyword(s):  
Ultraviolet Observations

scholarly journals Ultraviolet Observations of Some Close Binary Systems by the Astronomical Netherlands Satellite-Ans

1976 ◽  
Vol 73 ◽  
pp. 213-223
Author(s):  
Chi-Chao Wu
Keyword(s):  
Binary Systems ◽  
Hot Spot ◽  
Close Binary ◽  
Spectral Energy ◽  
Dwarf Novae ◽  
Energy Distributions ◽  
Primary Star ◽  
Higher Temperature ◽  
Far Ultraviolet ◽  
Ultraviolet Observations

Observations of δ Pic, a β Lyr type of eclipsing binary and seven dwarf novae are reported. The ultraviolet light curves of δ Pic indicate the accumulation of matter at the triangular Lagrangian points L4 and L5, the presence of a hot spot and a higher temperature for the primary star. The implication is that the cooler secondary fills its Roche lobe and is transfering mass to the primary; mass loss to the circumstellar space and possibly to the system may also be appreciable. The temperatures of dwarf novae are derived by comparing their ultraviolet spectral energy distributions with those for normal stars of luminosity classes IV and V. Piecing together observations for different objects, the SSCyg systems have temperatures of 28 500 K, 10 000 K and 9500 K, respectively, when they are at minimum, immediately before outburst and at the beginning of rise to maximum. At maximum, the temperature is 22 500 K or 17 300 K depending on the interstellar reddening correction for AR And. Immediately before outburst, there is a large excess of flux in the far ultraviolet as indicated by the large value of the ratio of flux at 1550 Å to that at 1800 Å. The observations of Z Cam during standstill gives a temperature of 14 900 K. No excess of flux in the far ultraviolet was observed during the maximum of AR And and the standstill of Z Cam.

scholarly journals OPTICAL AND ULTRAVIOLET OBSERVATIONS OF THE VERY YOUNG TYPE IIP SN 2014cx IN NGC 337

2016 ◽  
Vol 832 (2) ◽  
pp. 139 ◽  
Author(s):  
Fang Huang ◽  
Xiaofeng Wang ◽  
Luca Zampieri ◽  
Maria Letizia Pumo ◽  
Iair Arcavi ◽  
...  
Keyword(s):  
Ultraviolet Observations

Mariner 9

1984 ◽  
pp. 120-137
Author(s):  
Wolfgang Engelhardt
Keyword(s):  
Mariner 9

scholarly journals Ultraviolet Observations of Cataclysmic Variables

1987 ◽  
Vol 93 ◽  
pp. 205-205 ◽  
Author(s):  
F. Verbunt
Keyword(s):  
Orbital Period ◽  
Cataclysmic Variables ◽  
Type Systems ◽  
Terminal Velocity ◽  
Dwarf Novae ◽  
Preliminary Results ◽  
System Type ◽  
International Ultraviolet Explorer ◽  
Flux Level ◽  
Ultraviolet Observations

AbstractThe preliminary results of the analysis of more than 1000 spectra of cataclysmic variables in the archive of the International Ultraviolet Explorer were presented at the meeting. To characterize the slope of the spectra I use F = log(f1460Å/f2880Å). For most spectra F lies between 0.2 and 0.7. No correlation of F with orbital period, inclination, system type or (for dwarf novae) length of the interoutburst interval are found, apart from somewhat lower values of F for DQ Her type systems. Out of 16 dwarf novae for which spectra both at outburst maximum and minimum are available 11 show no large difference in F between maximum and minimum, and in 5 F declines with the flux level. Out of 6 dwarf novae 5 show very red spectra during the rise to maximum, and 1 shows slopes during rise similar to those during decline.In the ultraviolet resonance lines, due to a wind from the disc, no correlation is found between inclination and terminal velocity.

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