Ivan L. Andronov, K. D. Andrych, K. A. Antoniuk, A. V. Baklanov, P. Beringer, V. V. Breus, V. Burwitz, L. L. Chinarova, D. Chochol, L. M. Cook, M. Cook, P. Dubo… 展开作者
Ivan L. Andronov, K. D. Andrych, K. A. Antoniuk, A. V. Baklanov, P. Beringer, V. V. Breus, V. Burwitz, L. L. Chinarova, D. Chochol, L. M. Cook, M. Cook, P. Dubovský, W. Godłowski, T. Hegedüs, K. Hoňková, L. Hric, Young-Beom Jeon, J. Juryšek, Chun-Hwey Kim, Yonggi Kim, Young-Hee Kim, S. V. Kolesnikov, L. S. Kudashkina, A. V. Kusakin, V. I. Marsakova, P. A. Mason, M. Mašek, N. Mishevskiy, R. H. Nelson, A. Oksanen, S. Parimucha, Ji-Won Park, K. Petrík, C. Quiñones, K. Reinsch, J. W. Robertson, I. M. Sergey, M. Szpanko, M. G. Tkachenko, L. G. Tkachuk, I. Traulsen, J. Tremko, V. S. Tsehmeystrenko, Joh-Na Yoon, S. Zoła, N. M. Shakhovskoy
备注：
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 press
The types of instability in the interacting binary stars are reviewed. The project "Inter-Longitude Astronomy" is a series of smaller projects on concrete stars or groups of stars. It has no special funds, and is supported from resources and grants of participating organizations, when informal working groups are created. Totally we studied 1900+ variable stars of different types. The characteristic timescale is from seconds to decades and (extrapolating) even more. The monitoring of the first star of our sample AM Her was initiated by Prof. V.P. Tsesevich (1907-1983). Since more than 358 ADS papers were published. Some highlights of our photometric and photo-polarimetric monitoring and mathematical modelling of interacting binary stars of different types are presented: classical, asynchronous, intermediate polars and magnetic dwarf novae (DO Dra) with 25 timescales corresponding to different physical mechanisms and their combinations (part "Polar"); negative and positive superhumpers in nova-like and many dwarf novae stars ("Superhumper"); eclipsing "non-magnetic" cataclysmic variables; symbiotic systems ("Symbiosis"); super-soft sources (SSS, QR And); spotted (and not spotted) eclipsing variables with (and without) evidence for a current mass transfer ("Eclipser") with a special emphasis on systems with a direct impact of the stream into the gainer star's atmosphere, or V361 Lyr-type stars. Other parts of the ILA project are "Stellar Bell" (interesting pulsating variables of different types and periods - M, SR, RV Tau, RR Lyr, Delta Sct) and "Novice"(="New Variable") discoveries and classification with a subsequent monitoring for searching and studying possible multiple components of variability. Special mathematical methods have been developed to create a set of complementary software for statistically optimal modelling of variable stars of different types.
Polidan（1976）认为，在发射中显示CaII红外三重态的Be星是相互作用的双星。随着盖亚卫星的出现，它将拥有一个光谱仪来观察8470- 8750光年范围内的恒星，我们对150颗Be星进行了光谱调查，包括Be双星。我们发现，钙II三重态的发射，往往与帕邢线的发射，是一个特殊的环境中的一个被星盘，而不是一个相互作用的二进制被星的签名的指标。然而，钙II发射没有可见的帕邢线的发射被观察到在相互作用的双星，以及在特殊的对象。在巡天期间，发现了一个新的相互作用的Be双星- HD 81357。
Eta Carinae: an evolving view of the central binary, its interacting winds and its foreground ejecta
Eta Car的FUV光谱，在二十年的时间里用HST/STIS记录，记录了我们视线中消散消光引起的共振线的多次变化。FUV通量增加了近十倍，这导致了侏儒体内多个壳层的电离增加和分子氢的光破坏。观测到的共振线剖面与CMFGEN模式剖面的比较，允许分离的风-风碰撞和壳approptions从主风，天鹅座P profiles.The消散的掩星优先掩盖中心双星和相互作用的风相对于非常广泛的主风。我们现在能够监测碰撞风与轨道相位的变化。在最近的近星点通道上发生了高速瞬态扰动，表明次级风加速了主风，导致了下游的高速弓形激波，这是每个轨道周期新产生的。没有证据表明双星风的性质发生了变化。
Interacting Binary Stars as Progenitors for Interacting Supernovae
National Taiwan University（国立台湾大学）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Heidelberger Institut für Theoretische Studien（海德堡理论研究所）；Kyoto University（京都大学）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学中心）；Astronomisches Rechenzentrum（天文计算中心）；Institut für Theoretische Astrophysik（理论天体物理研究所）
Response to Comment on "A Non-Interacting Low-Mass Black Hole -- Giant Star Binary System"
van den Heuvel和Tauris认为，如果系统2 MASS J 05215658 +4359220中的红巨星质量为1个太阳质量（M $_\odot$），那么它看不见的伴星可能是由两颗0.9 M的$_\odot$组成的双星，形成一个三重系统。我们认为，现有的数据与质量为$3.2^{+1.0}_{-1.0}$ M $_\odot$的巨星最一致，这意味着$3.3^{+2.8}_{-0.7}$ M $_\odot$的黑洞伴星。
