WOLF, M., Hana KUČÁKOVÁ, P. ZASCHE, J. VRAŠTIL, K. HOŇKOVÁ, K. HORNOCH, M. LEHKÝ, M. MAŠEK, L. ŠMELCER, M. TYLŠAR, R. NOVÁK, L. ČERVINKA and M. BĚLÍK. Possible substellar companions in low-mass eclipsing binaries: GU Bootis and YY Geminorum. Astronomy & Astrophysics. 2018, vol. 620, December, p. "A72-1"-"A72-7", 7 pp. ISSN 0004-6361. Available from: https://dx.doi.org/10.1051/0004-6361/201833708.
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Basic information
Original name Possible substellar companions in low-mass eclipsing binaries: GU Bootis and YY Geminorum
Authors WOLF, M., Hana KUČÁKOVÁ (203 Czech Republic, guarantor, belonging to the institution), P. ZASCHE, J. VRAŠTIL, K. HOŇKOVÁ, K. HORNOCH, M. LEHKÝ, M. MAŠEK, L. ŠMELCER, M. TYLŠAR, R. NOVÁK, L. ČERVINKA and M. BĚLÍK.
Edition Astronomy & Astrophysics, 2018, 0004-6361.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher France
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19240/18:A0000356
Organization Filozoficko-přírodovědecká fakulta – Slezská univerzita v Opavě – Repository
Doi http://dx.doi.org/10.1051/0004-6361/201833708
UT WoS 000452389400002
Keywords in English binaries: eclipsing; stars: late-type; stars: individual: GU Bootis; stars: individual: YY Geminorum; stars: fundamental parameters
Tags ÚF
Tags International impact, Reviewed
Changed by Changed by: Jan Hladík, učo 1305. Changed: 5/4/2019 16:11.
Abstract
We present the next results of our long-term observational project to analyze the variations in the orbital periods of low-mass eclipsing binaries. About 70 new precise mid-eclipse times recorded with a CCD were obtained for two eclipsing binaries with short orbital periods: GU Boo (P = 0.^{d}49) and YY Gem (0.^{d}81). Observed-minus-calculated diagrams of the stars were analyzed using all reliable timings, and new parameters of the light-time effect were obtained. We derived for the first time or improved the short orbital periods of possible third bodies of 11 and 54 years for these low-mass binaries, respectively. We calculated that the minimum masses of the third components are close to 50 M_{Jup}, which corresponds to the mass of brown dwarfs. The multiplicity of these systems also plays an important role in the precise determination of their physical parameters.
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