1989
DOI: 10.1007/bf00215932
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The relation between RS CVn and Algol

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Cited by 104 publications
(105 citation statements)
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“…In only one case, TT Aur, the course of the period changes appears more complex but the cyclic term and its parameters can be well explained in terms of LITE. This detailed analysis brought further evidences that the period changes in ET-systems really have significantly less complicated course than in LL-Algols and the finding of Hall (1989) was thus confirmed. These results, that is absence of alternate period changes in ET-systems, strengthen the evidence for an important role of the outer convective layer of a component of a binary in the period changes of LL-Algols.…”
Section: Discussionsupporting
confidence: 54%
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“…In only one case, TT Aur, the course of the period changes appears more complex but the cyclic term and its parameters can be well explained in terms of LITE. This detailed analysis brought further evidences that the period changes in ET-systems really have significantly less complicated course than in LL-Algols and the finding of Hall (1989) was thus confirmed. These results, that is absence of alternate period changes in ET-systems, strengthen the evidence for an important role of the outer convective layer of a component of a binary in the period changes of LL-Algols.…”
Section: Discussionsupporting
confidence: 54%
“…It was found that the course of the period variations is monotonic and in some systems the period is even constant. This detailed analysis of extensive sets of timings covering several decades brings a strong support to an earlier finding of Hall (1989) and develops it further. We show that all systems with the orbital periods shorter than nine days display constant period or its increase, with the exception of an uncertain case of V 337 Aql.…”
supporting
confidence: 72%
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“…Short period close binaries (e.g., EP And) i.e., those having an orbital period P , 5À6 days, possess the above mentioned characteristics, due to rapid rotation (Richard & Albright 1993). Many authors (see e.g., Richards 1993Richards , 1992Hall 1989& Olson 1981 have discussed that the secondary and/or primary in the close binaries having a late type component show a variety of time dependent magnetic properties, which may cause, brightness variations in the LC (particularly at mid primary eclipse), radiations of X-ray, Ultraviolet, infrared, and cyclic variations in the orbital period of the binary (through a mechanism purposed by Applegate 1992 and modified by Lanza et al 1998& Lanza 2005. This mechanism is based on the variation of the active star shape through a change in the Gravitational Quadrupole Moment (GQM) of the star.…”
Section: Magnetic Cycle Effectmentioning
confidence: 99%