WOLF, M., Hana KUČÁKOVÁ, P. ZASCHE, K. HORNOCH, J. KARA, J. MERC and M. ZEJDA. Possible substellar companions in dwarf eclipsing binaries SDSS J143547.87+373338.5, NSVS 7826147, and NSVS 14256825. Astronomy & Astrophysics. FR - Francouzská republika, 2021, vol. 647, March, p. "A65-1"-"A65-7", 7 pp. ISSN 0004-6361. Available from: https://dx.doi.org/10.1051/0004-6361/202039851.
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Basic information
Original name Possible substellar companions in dwarf eclipsing binaries SDSS J143547.87+373338.5, NSVS 7826147, and NSVS 14256825
Authors WOLF, M., Hana KUČÁKOVÁ (203 Czech Republic, belonging to the institution), P. ZASCHE, K. HORNOCH, J. KARA, J. MERC and M. ZEJDA.
Edition Astronomy & Astrophysics, FR - Francouzská republika, 2021, 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/47813059:19630/21:A0000165
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1051/0004-6361/202039851
UT WoS 000629518900003
Keywords in English binaries: eclipsing;binaries: close;stars: fundamental parameters;stars: general;planets and satellites: detection;subdwarfs
Tags 2022, FÚ, RIV22
Tags International impact, Reviewed
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 9/3/2022 11:52.
Abstract
We present the new results of our long-term observational project to detect the small variations in the orbital periods of low-mass and short-period eclipsing binaries. About 120 new precise mid-eclipse times were obtained for three relatively well-known dwarf eclipsing binaries: SDSS J143547.87+373338.5 (P = 0.126 d), NSVS 07826147 (0.162 d), and NSVS 14256825 (0.110 d). Observed-minus-calculated diagrams of these systems were analyzed using all accurate timings, and, where possible, new parameters of the light-time effect were calculated. For the first time, we derive (or improve upon previous findings with regard to) the short orbital periods of 13 and 10 years of possible third bodies for SDSS J143547.87+373338.5 and NSVS 07826147, respectively. In these binaries, our data show that period variations can be modeled simply on the basis of a single circumbinary object. For the first two objects, we calculated the minimum mass of the third components to be 17 M-jup and 1.4 M-jup respectively, which corresponds to the mass of a brown dwarf or a giant planet. For NSVS 14256825, the cyclical period changes caused by a single additional body cannot be confirmed by our recent eclipse time measurements. More complex behavior connected with two orbiting bodies, or yet unknown effects, should be taken into account.
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