Double eclipsing binary system KIC 3832716

Fedurco, M.; Parimucha, Š.

doi:10.1007/s10509-018-3487-7

Cited by 5 publications

(2 citation statements)

References 25 publications

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“…As pointed out by Paper II, Algol-type binaries, with sub-giant or giant primaries, Dormant Black Holes in OGLE Galactic Ellipsoidals 3 are famous counter examples. These systems, which probably went through a mass-transfer phase during their evolution (e.g., Fedurco & Parimucha 2018;Chen et al 2020), can have a mass ratio larger than unity and still have an MS secondary (e.g., Negu & Tessema 2018;Samadi Ghadim et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Search for Dormant Black Holes in Ellipsoidal Variables III. The OGLE BULGE Short-Period Sample

Gomel,

Faigler,

Mazeh

et al. 2021

Preprint

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This is the third of a series of papers that presents an algorithm to search for close binaries with massive, possibly compact, unseen secondaries. The detection of such a binary is based on identifying a star that displays a large ellipsoidal periodic modulation, induced by tidal interaction with its companion. In the second paper of the series we presented a simple approach to derive a robust modified minimum mass ratio (mMMR), based on the observed ellipsoidal amplitude, without knowing the primary mass and radius, assuming the primary fills its Roche lobe. The newly defined mMMR is always smaller than the actual mass ratio. Therefore, a binary with an mMMR larger than unity is a good candidate for having a massive secondary, which might be a black hole or a neutron star. This paper considers 10, 956 OGLE short-period ellipsoidals observed towards the Galactic Bulge. We re-analyse their modulation and identify 136 main-sequence systems with mMMR significantly larger than unity as candidates for having compact-object secondaries, assuming their observed periodic modulations reflect indeed the ellipsoidal effect. Obviously, one needs follow-up observations to find out the true nature of these companions.

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Section: Introductionmentioning

confidence: 99%

Search for Dormant Black Holes in Ellipsoidal Variables III. The OGLE BULGE Short-Period Sample

Gomel,

Faigler,

Mazeh

et al. 2021

Preprint

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“…As discussed by Gomel, Faigler, & Mazeh (2021a), Algol-type binaries, with sub-giant or giant primaries, are famous counterexamples. These systems, which probably went through a masstransfer phase during their evolution (e.g., Fedurco & Parimucha 2018;Chen et al 2020), can have a mass ratio larger than unity and still have a MS secondary (e.g., Negu & Tessema 2018;Samadi Ghadim et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Gaia Data Release 3: Ellipsoidal Variables with Possible Black-Hole or Neutron Star secondaries

Gomel¹,

T.²,

S.³

et al. 2022

Preprint

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As part of Gaia Data Release 3, supervised classification identified a large number of ellipsoidal variables, for which the periodic variability is presumably induced by tidal interaction with a companion in a close binary system. In this paper, we present 6306 shortperiod probable ellipsoidal variables with relatively large-amplitude Gaia G-band photometric modulations, indicating a possible massive, unseen secondary. In case of a main-sequence primary, the more massive secondary is probably a compact object -either a black hole or a neutron star, and sometimes a white dwarf. The identification is based on a robust modified minimum mass ratio (mMMR) suggested recently by Gomel, Faigler and Mazeh (2021), derived from the observed ellipsoidal amplitude only, without the use of the primary mass or radius. We also list a subset of 262 systems with mMMR larger than unity, for which the compact-secondary probability is higher. Follow-up observations are needed to verify the true nature of these variables.

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Doubly eclipsing systems

Zasche

Vokrouhlický

Wolf

et al. 2019

A&A

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Context. Only several doubly eclipsing quadruple stellar systems are known to date, and no dedicated effort to characterize population properties of these interesting objects has yet been made. Aims. Our first goal was to increase number of known doubly eclipsing systems such that the resulting dataset would allow us to study this category of objects via statistical means. In order to minimize biases, we used long-lasting, homogeneous, and well-documented photometric surveys. Second, a common problem of basically all known doubly eclipsing systems is the lack of proof that they constitute gravitationally bound quadruple system in the 2+2 architecture (as opposed to two unrelated binaries that are projected onto the same location in the sky by chance). When possible, we thus sought evidence for the relative motion of the two binaries. In that case, we tried to determine the relevant orbital periods and other parameters. Methods. We analysed photometric data for eclipsing binaries provided by the OGLE survey and we focused on the LMC fields. We found a large number of new doubly eclipsing systems (our discoveries are three times more numerous than the previously known cases in this dataset). In order to prove relative motion of the binaries about a common centre of mass, we made use of the fact that OGLE photometry covers several years. With a typical orbital period of days for the observed binaries, we sought eclipse time variations (ETVs) on the timescale comparable to a decade (this is the same method used for an archetype of the doubly eclipsing system, namely V994 Her). In the cases where we were able to detect the ETV period, the difference between the inner and outer periods in the quadruple system is large enough. This allows us to interpret ETVs primarily as the light-time effect, thus providing an interesting constraint on masses of the binaries.Results. In addition to significantly enlarging the database of known doubly eclipsing systems, we performed a thorough analysis of 72 cases. ETVs for 28 of them (39% of the studied cases) showed evidence of relative motion. Among these individual systems, we note OGLE BLG-ECL-145467, by far the most interesting case; it is bright (12.6 mag in I filter), consists of two detached binaries with periods of ≃ 3.3 d and ≃ 4.9 d (making it a candidate for a 3 : 2 resonant system) revolving about each other in only ≃ 1538 d. Distribution of the orbital period ratio P A /P B of binaries in 2+2 quadruples shows statistically significant excess at ≃ 1 and ≃ 1.5. The former is likely a natural statistical preference in weakly interacting systems with periods within the same range. The latter is thought to be evidence of a capture in the 3 : 2 mean motion resonance of the two binaries. This sets important constraints on evolutionary channels in these systems. Conclusions. The total number of doubly eclipsing systems increased to 146, more than 90% of which are at low declinations on the southern sky. This motivates us to use southern hemisphere facilities to further character...

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Double eclipsing binary system KIC 3832716

Cited by 5 publications

References 25 publications

Search for Dormant Black Holes in Ellipsoidal Variables III. The OGLE BULGE Short-Period Sample

Search for Dormant Black Holes in Ellipsoidal Variables III. The OGLE BULGE Short-Period Sample

Gaia Data Release 3: Ellipsoidal Variables with Possible Black-Hole or Neutron Star secondaries

Doubly eclipsing systems

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