A Mechanism for Producing Short-Period Binaries

Eggleton, P. P.; Kisseleva-Eggleton, Ludmila

doi:10.1007/s10509-006-9078-z

Cited by 106 publications

(86 citation statements)

References 10 publications

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“…Bate et al (2002) shows how these close systems can be formed from wider systems through the processes associated with phase I with dynamical interactions being the dominant mechanism. Kozai cycles with tidal friction (KCTF; Eggleton & Kisseleva-Eggleton 2006) is an example of such a dynamical process. This evolution depends on the periods of the primary and tertiary components P 3 (P 3 /P 1 ).…”

Section: Multiplicity Fraction Across a Wide Mass Rangementioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2014

A&A

129

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Context. Dynamically undisrupted, young populations of stars are crucial in studying the role of multiplicity in relation to star formation. Loose nearby associations provide us with a great sample of close (<150 pc) pre-main sequence (PMS) stars across the very important age range (≈5−70 Myr) to conduct such research. Aims. We characterize the short period multiplicity fraction of the search for associations containing young stars (SACY) sample, accounting for any identifiable bias in our techniques and present the role of multiplicity fractions of the SACY sample in the context of star formation. Methods. Using the cross-correlation technique we identified double-lined and triple-lined spectroscopic systems (SB2/SB3s), in addition to this we computed radial velocity (RV) values for our subsample of SACY targets using several epochs of Fiber-fed Extended Range Optical Spectrograph (FEROS) and Ultraviolet and Visual Echelle Spectrograph (UVES) data. These values were used to revise the membership of each association that was then combined with archival data to determine significant RV variations across different data epochs characteristic of multiplicity; single-lined multiple systems (SB1). Results. We identified seven new multiple systems (SB1s: 5, SB2s: 2). We find no significant difference between the short period multiplicity fraction (F m ) of the SACY sample and that of close star-forming regions (≈1−2 Myr) and the field (F m ≤ 10%). These are seen both as a function of age and as a function of primary mass, M 1 , in the ranges P [1:200 day] and M 2 [0.08 M -M 1 ], respectively. Conclusions. Our results are consistent with the picture of universal star formation, when compared to the field and close star-forming regions (SFRs). We comment on the implications of the relationship between increasing multiplicity fraction with the primary mass within the close companion range in relation to star formation.

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Section: Multiplicity Fraction Across a Wide Mass Rangementioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2014

A&A

129

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“…Eggleton & Kisseleva-Eggleton (2006) explored the parameter space for triple systems, searching for those conditions where Kozai cycles plus tidal friction would lead to interactions that would result in orbital shrinkage of the inner pair of stars and produce close or contact binaries. They crudely estimated the outer period needed to cause Kozai cycles to operate on a given inner orbit.…”

Section: Discussionmentioning

confidence: 99%

The Spectroscopic Orbit of SAO 167450, Visual Companion of AA Ceti

Fekel

Willmarth

2009

PUBL ASTRON SOC PAC

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ABSTRACT. We have determined a spectroscopic orbit for SAO 167450, which is the visual secondary of the W UMa-type eclipsing binary AA Cet, and so the system is quadruple. Radial velocities from the coudé feed and 4 m telescopes at Kitt Peak National Observatory produce an orbit with a period of 25.68 days and an eccentricity of 0.50. We classify both the primary and secondary as G0 subgiant/dwarf stars and find that they are somewhat metal rich relative to the Sun. The high lithium abundances of both components argue that the stars are less than 1 Gyr old. If the components are dwarfs, they are pseudosynchronously rotating, while if they are subgiants, they are rotating more slowly than pseudosynchronous. We very roughly estimate a period of 5,000-15,000 yr for the visual pair. Although it has been suggested that in a multiple system, the combination of Kozai cycles and tidal friction may produce contact binaries, the separation between the visual components in this system appears to be much too large to accomplish that result.

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“…We note in passing, that even non-evolved (low mass) MS close binaries with orbits of a few days were most likely evolved from wider binaries in triple systems, that shrunk to their current orbit due to the processes of Kozai cycles and tidal friction (Mazeh & Shaham 1979;Eggleton & Kisseleva-Eggleton 2006;Tokovinin et al 2006;Fabrycky & Tremaine 2007). Formation of circumbinary close planetary systems even around short period MS binaries is therefore likely to be dynamically excluded, or would require a complicated and fine tuned dynamical history.…”

Section: Circumbinary Planetsmentioning

confidence: 91%

Planets in Evolved Binary Systems

Perets

2011

AIP Conference Proceedings

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Exoplanets are typically thought to form in protoplanetary disks left over from protostellar disk of their newly formed host star. However, additional planetary formation and evolution routes may exist in old evolved binary systems. Here we discuss the implications of binary stellar evolution on planetary systems in such environments. In these binary systems stellar evolution could lead to the formation of symbiotic stars, where mass is lost from one star and could be transferred to its binary companion, and may form an accretion disk around it. This raises the possibility that such a disk could provide the necessary environment for the formation of a new, second generation of planets in both circumstellar or circumbinary configurations. Pre-existing first generation planets surviving the post-MS evolution of such systems would be dynamically effected by the mass loss in the systems and may also interact with the newly formed disk. Such planets and/or planetesimals may also serve as seeds for the formation of the second generation planets, and/or interact with them, possibly forming atypical planetary systems. Second generation planetary systems should be typically found in white dwarf binary systems, and may show various observational signatures. Most notably, second generation planets could form in environment which are inaccessible, or less favorable, for first generation planets. The orbital phase space available for the second generation planets could be forbidden (in terms of the system stability) to first generation planets in the pre-evolved progenitor binaries. In addition planets could form in metal poor environments such as globular clusters and/or in double compact object binaries. Observations of exo-planets in such forbidden or unfavorable regions could possibly serve to uniquely identify their second generation character. Finally, we point out a few observed candidate second generation planetary systems, including Gl 86, HD 27442 and all of the currently observed circumbinary planet candidates. A second generation origin for these systems could naturally explain their unique configurations.

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A Mechanism for Producing Short-Period Binaries

Cited by 106 publications

References 10 publications

Search for associations containing young stars (SACY)

Search for associations containing young stars (SACY)

The Spectroscopic Orbit of SAO 167450, Visual Companion of AA Ceti

Planets in Evolved Binary Systems

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