A survey for transient accretion disks in short-period Algol systems. II

Kaitchuck, R. H.; Honeycutt, R. K.; Schlegel, Eric M.

doi:10.1086/131682

Cited by 58 publications

(39 citation statements)

References 11 publications

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“…In the literature there is no spectroscopic evidence of mass transfer in the AB Cas system. Kaitchuck, Honeycutt, & Schlegel (1985) presented an investigation of many classic Algol-type stars as part of a search for emission lines from accretion disks around the primary star, but in the H and H spectral region no emission effects were seen for AB Cas. Although Kreiner (1971) and Ahnert (1973) reported an orbital period change in this system, a detailed orbital period study is absent so far.…”

Section: Introductionmentioning

confidence: 99%

Orbital Period Changes of Algol-type Binaries: S Equulei and AB Cassiopeiae

et al. 2003

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The orbital periods of two Algol-type binaries, S Equ and AB Cas, are studied based on all available times of minima. It is found that the OÀC variations of both systems can be represented by a parabolic and a periodic term. S Equ has an accretion region due to mass transfer as shown by Richards and coworkers and Richards & Albright. On the other hand, Zola obtained a light-curve solution with a third light. Our study reveals evidence of mass transfer and third component stars in both systems. The parabolic terms in the OÀC variations are due to mass transfer from less massive to more massive components, which is consistent with the semidetached nature of both systems. The periodic terms are explained with the additional third stars in the systems. It is interesting that there is no sign of a magnetic braking effect from the cool secondary in the OÀC variation of either system.

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Section: Introductionmentioning

confidence: 99%

Orbital Period Changes of Algol-type Binaries: S Equulei and AB Cassiopeiae

et al. 2003

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“…behavior has also been seen to occur in RW Tau (Kaitchuck and Honeycutt 1982a), and TZ Eri (Kaitchuck and Park, 1988).…”

Section: Rotational Velocity Field and Emission Linementioning

confidence: 79%

“…To obtain some basic statistics on transient disks, we undertook a spectroscopic survey of short-period Algol systems (Kaitchuck and Honeycutt 1982b;Kaitchuck, Honeycutt and Schlegel 1985). There have been few modern surveys of the accretion disks in Algol systems (Plavec and Polidan 1976;Peters 1980).…”

Section: Survey For Transient Disksmentioning

confidence: 99%

Time-Resolved Spectroscopy of Accretion Disks in Algols

Kaitchuck

1989

International Astronomical Union Colloquium

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ABSTRACT. Time-resolved spectroscopy during the eclipse of shortperiod Algol systems, has shown their accretion disks to be small, turbulent structures with non-Keplerian velocity fields and asymmetries between the leading and trailing sides of the disk. These transient disks are produced by the impact of the gas stream on the mass-gaining star, and occur in systems where the star is just large enough to ensure the stream collision is complete. These emission line disks and the excess continuum emission do not always occur together. The permanent accretion disks in at least a few of the long-period Algol systems have features in common with the transient disks including nonKeplerian velocity fields.

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“…The stream strikes the gainer almost perpendicular to its surface and generates enough turbulence to keep the friction timescale short (Biermann & Hall 1973;Kaitchuck et al 1985). As a result, tidal interaction seems efficient enough to keep both components in a strong coupling regime, canceling the angular momentum flows within the binary (e.g., Hut & Paczynski 1984;Verbunt & Rappaport 1988), i.e.J 2 ≈ −J 1 .…”

Section: Mass Transfer In the Absence Of An Accretion Diskmentioning

confidence: 99%

Efficiency of ETV diagrams as diagnostic tools for long-term period variations

Nanouris

Kalimeris

Antonopoulou

et al. 2015

A&A

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Context. The credibility of an eclipse timing variation (ETV) diagram analysis is investigated for various manifestations of the mass transfer and gravitational radiation processes in binary systems. The monotonicity of the period variations and the morphology of the respective ETV diagrams are thoroughly explored in both the direct impact and the accretion disk mode of mass transfer, accompanied by different types of mass and angular momentum losses (through a hot-spot emission from the gainer and via the L2/L3 points). Aims. Our primary objective concerns the traceability of each physical mechanism by means of an ETV diagram analysis. Also, possible critical mass ratio values are sought for those transfer modes that involve orbital angular momentum losses strong enough to dictate the secular period changes even when highly competitive mechanisms with the opposite direction act simultaneously. Methods. TheJ −Ṗ relation that governs the orbital evolution of a binary system is set to provide the exact solution for the period and the function expected to represent the subsequent eclipse timing variations. The angular momentum transport is parameterized through appropriate empirical relations, which are inferred from semi-analytical ballistic models. Then, we numerically determine the minimum temporal range over which a particular mechanism is rendered measurable, as well as the critical mass ratio values that signify monotonicity inversion in the period modulations. Results. Mass transfer rates comparable to or greater than 10 −8 M yr −1 are measurable for typical noise levels of the ETV diagrams, regardless of whether the process is conservative. However, the presence of a transient disk around the more massive component defines a critical mass ratio (q cr ≈ 0.83) above which the period turns out to decrease when still in the conservative regime, rendering the measurability of the anticipated variations a much more complicated task. The effects of gravitational radiation proved to be rather undetectable, except for systems with physical characteristics that only refer to cataclysmic variables. Conclusions. The monotonicity of the period variations and the curvature of the respective ETV diagrams depend strongly on the accretion mode and the degree of conservatism of the transfer process. Unlike the hot-spot effects, the Lagrangian points L2 and L3 support very efficient routes of strong angular momentum loss. It is further shown that escape of mass via the L3 point -when the donor is the less massive component -safely provides critical mass ratios above which the period is expected to decrease, no matter how intense the process is.

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A survey for transient accretion disks in short-period Algol systems. II

Cited by 58 publications

References 11 publications

Orbital Period Changes of Algol-type Binaries: S Equulei and AB Cassiopeiae

Orbital Period Changes of Algol-type Binaries: S Equulei and AB Cassiopeiae

Time-Resolved Spectroscopy of Accretion Disks in Algols

Efficiency of ETV diagrams as diagnostic tools for long-term period variations

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