Results 1 to 10 of about 439,882 (181)
Infrared imaging of late-type stars [PDF]
Monthly Notices of the Royal Astronomical Society, 1996 Infrared imaging properties of dusty winds around late-type stars are investigated in detail, employing a self-consistent model that couples the equations of motion and radiative transfer. Because of general scaling properties, the angular profiles of surface brightness are self-similar. In any given star, the profile shape is determined essentially by
Ivezic, Zeljko, Elitzur, Moshe
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Spots and Flares in Hot Main Sequence Stars Observed by Kepler, K2, and TESS
Frontiers in Astronomy and Space Sciences, 2021 About 22,000 Kepler stars, 7,000 K2 stars, and nearly 60,000 TESS stars from sectors 1–24 have been classified according to variability type. A large proportion of stars of all spectral types appear to have periods in their light curves consistent with ...
Luis A. Balona
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The circularization time-scales of late–type binary stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2021 ABSTRACT We examine the consequences of, and apply, the formalism developed in Terquem (2021) for calculating the rate DR at which energy is exchanged between fast tides and convection. In this previous work, DR (which is proportional to the gradient of the convective velocity) was assumed to be positive in order to dissipate the tidal ...
Terquem, Caroline, Martin, Scott
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Progress report on the monitoring active late-type stars in 2005/2006 and the analysis of V523 Cas [PDF]
Serbian Astronomical Journal, 2006 We present the light curve analysis of late-type binary V523 Cas for the season 2005. The spot has been revealed on the secondary. According to theoretical considerations, the spot appeared to be hotter than the surrounding photosphere and located at ...
Zboril M., Đurašević G.
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A Mini Atlas of H-Band Spectra of Southern Symbiotic Stars
Galaxies, 2023 Symbiotic stars are interacting binary systems composed of an evolved star (generally a late-type red giant) and a degenerate or dwarf companion in orbit close enough for mass transfer to occur. Understanding the status of the late-type star is important
Paula Esther Marchiano +6 more
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Polyatomic Molecules in Late-Type Stars. [PDF]
The Astrophysical Journal, 1948 Some general problems connected with the presence of polyatomic molecules in stellar atmospheres are noted, and, in particular, reasons are advanced in favor of attributing at least part of the intensity drop and fluctuations in the spectra of the N-type stars violetward of λ 4100 to the triatomic molecule CH2.
Swings, Polydore, McKellar, A.
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Superflares on Late-Type Stars [PDF]
Proceedings of the International Astronomical Union, 2012 AbstractWe present the results of an extensive survey of superflares on late-type stars (G, K, and M-type main sequence stars) using the Kepler satellite data. Wefound about 6,800 superflares on late-type stars from the data of about 120,000 stars observed over 500 days.
Hiroyuki Maehara +7 more
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The masses of late-type WN stars [PDF]
Proceedings of the International Astronomical Union, 2006 AbstractWe present recent results for galactic WNL stars, obtained with the new Potsdam Wolf-Rayet (PoWR) hydrodynamic model atmospheres. Based on a combination of stellar wind modeling and spectral analysis we identify the galactic WNL subtypes as a group of extremely luminous stars close to the Eddington limit.
Gräfener, G., Hamann, W. -R.
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SULFUR ABUNDANCE IN THE GALACTIC DISC STARS
Odessa Astronomical Publications, 2013 The sulfur abundance was determined by the synthetic spectrum method in the stars with metallicity close to that of the Sun. The comparison with the results of other authors, as well as the nucleosynthesis computations were made.
O. P. Paramonova +2 more
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Odessa Astronomical Publications, 2013 Based on the spectra obtained with echelle spectrograph SOPHIE (1.93 mtelescope, OHP,France) and the selection of lines (Basak & Mishenina, 2012). we have redefined the parameters and have determined the abundances of the elements produced in the process
N. Yu. Basak, T. V. Mishenina
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