BVRcIcOBSERVATIONS AND ANALYSES OF THE DWARF DETACHED BINARY V1043 CASSIOPEIA AND A COMMENT ON PRECONTACT W UMa'S

Samec, R. G.; Smith, Paul M.; Chamberlain, H.; Faulkner, D. R.; Hamme, W. Van

doi:10.1088/0004-6256/145/1/14

Cited by 7 publications

(1 citation statement)

References 14 publications

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“…Some close binaries were observed as progenitors of W UMa binaries (e.g. Ka lużny 1990;Maceroni & Rucinski 1999;Samec et al 2013). At present, many observational studies mainly focused on detached binaries with periods shorter than 1d as the progenitors of W UMa binaries.…”

Section: Introductionmentioning

confidence: 99%

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Jiang

2019

Monthly Notices of the Royal Astronomical Society

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Close detached binaries were theoretically predicted to evolve into contact by three subtypes of case A binary evolution: case AD, AR, and AS, which correspond to the formation of contact during dynamic-, thermal-, and nuclear-timescale mass transfer phase, respectively. It is unclear, however, what is the difference between contact binaries in these subtypes, and whether all of these subtypes can account for the formation of observed W UMa binaries. Using Eggleton's stellar evolution code with the nonconservative assumption, I obtained the low-mass contact binaries produced by case AD, AR, and AS at the moment of contact, and their parameter spaces. The results support that the progenitors of low-mass contact binaries are detached binaries with orbital periods shorter than ∼ 2 − 5 d, and their borderlines depend strongly on the primary mass. In addition, the period-colour relations for case AR and AS can be in better agreement with that for observed W UMa candidates, but case AD shows a significantly worse agreement. Moreover, case AR and AS can produce a short-period limit (corresponding to a low-mass limit) at almost any age, e.g. from young age (∼ 0.2 Gyr) to old age (∼ 13 Gyr), agreeing with observed W UMa binaries in star clusters, but no such limit occurs for case AD at any age. These results support that case AR and AS, as opposed to case AD, can lead to W UMa binaries (including young W UMa binaries).

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Section: Introductionmentioning

confidence: 99%

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Jiang

2019

Monthly Notices of the Royal Astronomical Society

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Astrometric observations of the main Uranian satellites at the Pulkovo Observatory in 2007–2016

Ershova

Roshchina

Izmailov

2016

Planetary and Space Science

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BVR_cI_cOBSERVATIONS AND ANALYSES ON V2421 CYGNI, A PRECONTACT W UMa BINARY

Samec

Shebs

Faulkner

et al. 2013

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BVR_cI_cOBSERVATIONS AND ANALYSES OF THE DWARF DETACHED BINARY V1043 CASSIOPEIA AND A COMMENT ON PRECONTACT W UMa'S

Cited by 7 publications

References 14 publications

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Astrometric observations of the main Uranian satellites at the Pulkovo Observatory in 2007–2016

BVR_cI_cOBSERVATIONS AND ANALYSES ON V2421 CYGNI, A PRECONTACT W UMa BINARY

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BVRcIcOBSERVATIONS AND ANALYSES OF THE DWARF DETACHED BINARY V1043 CASSIOPEIA AND A COMMENT ON PRECONTACT W UMa'S

Cited by 7 publications

References 14 publications

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Astrometric observations of the main Uranian satellites at the Pulkovo Observatory in 2007–2016

BVRcIcOBSERVATIONS AND ANALYSES ON V2421 CYGNI, A PRECONTACT W UMa BINARY

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Product

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BVR_cI_cOBSERVATIONS AND ANALYSES OF THE DWARF DETACHED BINARY V1043 CASSIOPEIA AND A COMMENT ON PRECONTACT W UMa'S

BVR_cI_cOBSERVATIONS AND ANALYSES ON V2421 CYGNI, A PRECONTACT W UMa BINARY