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Interacting Binary White Dwarf Stars [PDF]

Symposium - International Astronomical Union, 1992
This group of stars consists of 4 systems, also called helium cataclysmics. Three of them show photometric variations and have been studied by the Whole Earth Telescope (WET), which have revealed multiperiodic light curves showing the signature of g-mode non-radial pulsations on the accreting star.
J.‐E. Solheim
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Be Stars as Interacting Binaries [PDF]

Symposium - International Astronomical Union, 1982
At the last IAU Symposium on Be stars held in Bass River, MA in 1975, several of us (including P. Harmanec, M. Plavec, R.S. Polidan, and myself) suggested that Be stars are mass transfer binaries and represent the higher mass counterparts to the familiar Algol systems.
Geraldine J. Peters
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Ultraviolet Observations of Interacting Binary Be Stars [PDF]

Symposium - International Astronomical Union, 1982
Initial results from the analysis of a series of timed, high resolution IUE observations of HR 2142, ϕ Per, CX Dra, KX And, AU Mon, and TT Hya are presented. The data base for HR 2142 also includes Copernicus U1 and U2 observations. Variable absorption lines, indicative of mass flow in the system, are observed in all objects except ϕ Per.
Geraldine J. Peters, Ronald S. Polidan
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Interacting Binaries as Be Stars [PDF]

International Astronomical Union Colloquium, 1987
AbstractSemidetached close binary stars of the Algol type often have primary components of spectral type A0 or earlier and display emission at Hα (sometimes also at higher Balmer lines). They are therefore Be stars. Many binaries of this type are not eclipsing and must look like “ordinary” Be stars.
M. Plavec
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Instabilities in Interacting Binary Stars [PDF]

, 2017
Non-Stable Universe: Energetic Resources, Activity Phenomena and Evolutionary Processes, 19-23 September 2016, ed. Areg Mickaelian, Haik Harutyunian and Elena Nikoghosyan, Astronomical Society of the Pacific (ASP) Conference Series, 2017, in ...
Andronov, I. L., Andrych, K. D., Antoniuk, K. A., Baklanov, A. V., Beringer, P., Breus, V. V., Burwitz, V., Chinarova, L. L., Chochol, D., Cook, L. M., Cook, M., Dubovský, P., Godlowski, W., Hegedüs, T., Hoňková, K., Hric, L., Jeon, Y.-B., Juryšek, J., Kim, C.-H., Kim, Y., Kim, Y.-H., Kolesnikov, S. V., Kudashkina, L. S., Kusakin, A. V., Marsakova, V. I., Mason, P. A., Mašek, M., Mishevskiy, N., Nelson, R. H., Oksanen, A., Parimucha, S., Park, J.-W., Petrík, K., Quiñones, C., Reinsch, K., Robertson, J. W., Sergey, I. M., Szpanko, M., Tkachenko, M. G., Tkachuk, L. G., Traulsen, I., Tremko, J., Tsehmeystrenko, V. S., Yoon, J.-N., Zoła, Stanisław, Shakhovskoy, N. M.   +45 more
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"INTER-LONGITUDE ASTRONOMY" (ILA) PROJECT: CURRENT HIGHLIGHTS AND PERSPECTIVES. I. MAGNETIC VS. NON-MAGNETIC INTERACTING BINARY STARS [PDF]

Odessa Astronomical Publications, 2010
We present a review of highlights of our photometric and photo-polarimetric monitoring and mathematical modeling of interacting binary stars of different types classical, asynchronous, intermedi ate polars with 25 timescales corresponding to differ ent ...
I. L. Andronov, K. A. Antoniuk, A. V. Baklanov, V. V. Breus, V. Burwitz, L. L. Chinarova, D. Chochol, P. A. Dubovsky, W. Han, T. Hegedus, A. Henden, L. Hric, Chun-Hwey Kim, Yonggi Kim, S. V. Kolesnikov, I. Kudzej, A. Liakos, P. G. Niarchos, A. Oksanen, L. Patkos, K. Petrik, N. V. Pit', N. M. Shakhovskoy, N. A. Virnina, J. Yoon, S. Zola   +25 more
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Be Stars in Roche-Lobe Interacting Binaries [PDF]

International Astronomical Union Colloquium, 2000
AbstractDifferent types of massive interacting binaries with Be components are discussed. Due to mass exchange, Be stars in these systems have some peculiar characteristics. Often it is even difficult to find traces of the Be star and/or mass-losing star in the optical region of the spectrum. Using the value of the orbital period as a primary parameter,
А. Е. Тарасов
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AGB winds in interacting binary stars [PDF]

Monthly Notices of the Royal Astronomical Society, 2020
ABSTRACT We perform numerical simulations to investigate the stellar wind from interacting binary stars. Our aim is to find analytical formulae describing the outflow structure. In each binary system the more massive star is in the asymptotic giant branch (AGB) and its wind is driven by a combination of pulsations in the stellar surface ...
L Sabin, W Steffen, G García-Segura, Luis C Bermúdez-Bustamante   +3 more
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Calcium Emission in Interacting Binary Be Stars [PDF]

, 2012
3 pages, 1 figure, conference ...
Koubský, Pavel, Kotková, Lenka, Votruba, Viktor, Šlechta, Mirek, Škoda, Petr, Harmanec, Petr, Nemravová, Jana, Šejnová, Klára, Dvořáková, Šárka, Korčáková, Daniela   +9 more
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A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis

The Astrophysical Journal
W Serpentis is an eclipsing binary system and the prototype of the Serpentid class of variable stars. These are interacting binaries experiencing intense mass transfer and mass loss.
Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar   +8 more
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