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  • 1
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    The region of formation of the ultraviolet high temperature resonance lines in the eclipsing binary Beta Persei (Algol) (1989)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: A new series of IUE observations of Beta Persei has shown that the high temperature resonance lines of Si IV and C IV arise in a region that surrounds the brighter, early-type component of the system. The continuum spectrum corresponds to that of a B8V object, and the value of E(B-V) that yielded the best match between the two IUE regions was 0.06, the value quoted for Beta Per in Jamar et al.'s (1976) Catalog.
    Keywords: ASTROPHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 215; 2, Ma
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  • 2
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    IUE observations of symbiotic stars (1981)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: The IUE observations suggest that the symbiotic stars can be placed in two broad groups. One of the groups is characterized by strong, narrow emissions arising from a wide range of excitation energies, while the other one typically shows a strong continuum with absorption lines and very few or no emissions at all. Both broad groups appear to suggest that these are binary systems and that they probably differ in the characteristics and extent of the chromosphere-corona formation that is present in the system.
    Keywords: ASTROPHYSICS
    Type: NASA. Goddard Space Flight Center The Universe of Ultraviolet Wavelengths: The First Two Yrs. of Intern. Ultraviolet Explorer; p 451-454
    Format: application/pdf
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  • 3
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    Wind collision effects in the early-type close binaries HD 47129 and AO Cassiopeiae (1991)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Selected regions of IUE spectra of the binaries HD 47129 and AO Cassiopeiae are analyzed, and evidence for the effect of wind collision in both objects is found. A possible alternative explanation for the behavior of the spectral lines of the 'secondary' component in HD 47129 is suggested.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 379; 706-714
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  • 4
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    An interpretation of the line profile variations in the IUE spectrum of the Wolf-Rayet binary Gamma(2) Velorum (1989)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: An analysis of the variable profiles of the high-temperature resonance lines of Si IV in the IUE spectrum of gamma(2) Vel has made it possible to describe these profiles as a superposition of two different profiles, namely, a P Cygni profile that remains practically stationary throughout the orbital cycle and an absorption profile that moves back and forth with phase. To these two profiles is added a very sharp, strong absorption that ought to arise in the layers of the extended gaseous envelope that merge with the interstellar medium. The absorption that moves back and forth during the system's orbital revolution has been interpreted as suggesting a stream going away from the system at an angle of some 110 deg from the direction of the radius vector joining the Wolf-Rayet star with its companion. Such a stream seems to project upon a dense concentration of matter that is located somewhere in the volume between the two stars and moves away at some -700 km/s, and should result from the collision of the winds from the two components. The high-temperature resonance lines of N V and C IV very likely behave similarly to Si IV.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 340; 1091-110
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  • 5
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    A study of the continuum flux and the line structure in the IUE spectrum of Beta Lyrae (1988)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: A study of the available archival IUE images of Beta Lyrae has led to the following results: (1) for lambda in the range of 1250 - 1500 A, the eclipse depth at second conjunction is slightly larger than the eclipse depth at primary conjunction; they are equal at about 1670 A; (2) the profiles of the resonance lines of SiIV (and the same seems to be true for NV and CIV) can be described as composite, formed by the superposition of a stationary P Cygni profile that suggests a velocity of approach of -170 km/s and a broad, less strong, emission that seems to yield a velocity distribution in antiphase with the velocity curve of the B8 II component of the system; and (3) the emission lines of the intercombination doublet of semiforbidden N II at about 2140 A suggest a velocity of about -130 km/s. The interpretation of the latter composite profile appears similar to the one suggested by Sahade (1966) to describe H-alpha and He I 5876 and He I 6678, and by Batten and Sahade (1973) to describe H-alpha.
    Keywords: ASTROPHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 193; 1-2; 202-210
    Format: text
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