Results 11 to 20 of about 9,614 (265)
Journal of Mathematical and Fundamental Sciences, 2019 Hα line variations of 8 B-emission (Be) stars are presented. Stars that are listed in the Bright Star Catalogue were observed in 2009 at the Bosscha Observatory, Lembang, Indonesia. It was found that 4 stars showed phase changing from Be double-peaked to
Aprilia Aprilia +7 more
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THE MASSIVE STELLAR POPULATION IN THE DWARF STARBURST GALAXIES
Odessa Astronomical Publications, 2017 The analysis of the long-slit spectral observations of 39 Wolf-Rayet (WR) galaxies with heavy element mass fraction ranging over 2 orders of magnitudes from Z☉/50 to 2Z☉ are presented.
N. G. Guseva
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Physical Properties of Radio Stars Based on LAMOST Spectral Survey
Universe, 2022 Radio emission has been detected for all types of stars in the Hertzsprung Russell diagram. Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) low and medium-resolution spectroscopic surveys provide a good opportunity to obtain the ...
Liyun Zhang +6 more
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Measurement of Interstellar Extinction in Emission Line Stars [PDF]
Symposium - International Astronomical Union, 1970 Usually selective interstellar extinction is derived by comparing the spectrum of a reddened star with an unreddened nearby star, preferably of the same spectral type. But in many cases this comparison is not possible, so that new methods have to be used.A direct measure of this quantity is possible when a spectrum shows a number of emission lines as ...
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Photometric and spectroscopic study of five pre-main sequence stars in the vicinity of NGC 7129 [PDF]
Serbian Astronomical Journal, 2019 We present results from long-term optical photometric and spectroscopic observations of five pre-main sequence stars, located in the vicinity of the bright nebula NGC 7129.
Semkov E.H., Ibryamov S.I., Peneva S.P.
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Line Variations of Hα Emissions and Absorptions of Be Stars
Journal of Physics: Conference Series, 2019 We present the spectroscopic variations of 14 program Be stars observed within 2008 - 2009 at the Bosscha Observatory, Lembang, Indonesia. The Be stars show spectroscopic profiles as Be and Be-shell, and sometimes as B-normal. These profiles come from the disk-like envelope or rings surrounded the star's equatorial plane. Our program stars are: 5 as Be
null Aprilia +5 more
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EUV Emission Lines in the Atmospheres of Cool Stars [PDF]
Physica Scripta, 1987 High resolution far ultraviolet (1200-2000 A) spectra of 17 cool giant and supergiant stars have been obtained using the IUE satellite of ESA, NASA and UK. We have measured the line intensities, wavelengths and widths of approximately 200 EUV emission lines in these spectra, using a least squares gaussian fitting technique. Line identification has been
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Gamma Cas Stars as Be+White Dwarf Binary Systems
The Astrophysical Journal Letters, 2022 The origin of the bright and hard X-ray emission flux among the γ Cas subgroup of B-emission line (Be) stars may be caused by gas accretion onto an orbiting white dwarf (WD) companion.
Douglas R. Gies +2 more
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The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
The Astronomical Journal, 2023 Close binary interactions may play a critical role in the formation of the rapidly rotating Be stars. Mass transfer can result in a mass gainer star spun up by the accretion of mass and angular momentum, while the mass donor is stripped of its envelope ...
Luqian Wang +3 more
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Emission Lines in Star Forming Galaxies [PDF]
Symposium - International Astronomical Union, 1995 Magris et al. (1993, Proceedings of the ESO/OHP Workshop on Dwarf Galaxies, ed. G. Meylan) have combined the spectral evolution population synthesis code of Bruzual & Charlot (1993, ApJ 405, 538) with the multipurpose photoionization-shock code MAPPINGS (Binette et al.
Gustavo A. Bruzual, Gladis C. Magris
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