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Detection of the binarity of the star J1158+4239. / Khovrichev, M. Yu; Kulikova, A. M.; Sokov, E. N.; Dyachenko, V. V.; Rastegaev, D. A.; Beskakotov, A. S.; Balega, Yu Yu; Safonov, B. S.; Dodin, A. V.; Vozyakova, O. V.

в: Astronomy Letters, Том 42, № 10, 01.10.2016, стр. 686-692.

Результаты исследований: Научные публикации в периодических изданияхстатьяРецензирование

Harvard

Khovrichev, MY, Kulikova, AM, Sokov, EN, Dyachenko, VV, Rastegaev, DA, Beskakotov, AS, Balega, YY, Safonov, BS, Dodin, AV & Vozyakova, OV 2016, 'Detection of the binarity of the star J1158+4239', Astronomy Letters, Том. 42, № 10, стр. 686-692. https://doi.org/10.1134/S1063773716100054

APA

Khovrichev, M. Y., Kulikova, A. M., Sokov, E. N., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A. S., Balega, Y. Y., Safonov, B. S., Dodin, A. V., & Vozyakova, O. V. (2016). Detection of the binarity of the star J1158+4239. Astronomy Letters, 42(10), 686-692. https://doi.org/10.1134/S1063773716100054

Vancouver

Khovrichev MY, Kulikova AM, Sokov EN, Dyachenko VV, Rastegaev DA, Beskakotov AS и пр. Detection of the binarity of the star J1158+4239. Astronomy Letters. 2016 Окт. 1;42(10):686-692. https://doi.org/10.1134/S1063773716100054

Author

Khovrichev, M. Yu ; Kulikova, A. M. ; Sokov, E. N. ; Dyachenko, V. V. ; Rastegaev, D. A. ; Beskakotov, A. S. ; Balega, Yu Yu ; Safonov, B. S. ; Dodin, A. V. ; Vozyakova, O. V. / Detection of the binarity of the star J1158+4239. в: Astronomy Letters. 2016 ; Том 42, № 10. стр. 686-692.

BibTeX

@article{cb575916e6b14935a5bdca36dfd39e09,
title = "Detection of the binarity of the star J1158+4239",
abstract = "One of the goals of the Pulkovo program of research on stars with large proper motions is to reveal among the low-luminosity stars those that have evidence of binarity. Twelve astrometric binary candidates from the Pulkovo list have been included in the program of speckle observations with the BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS) and the 2.5-m telescope at the Caucasus Observatory (CO) of the Sternberg Astronomical Institute of the Moscow State University to confirm their binarity and then to determine the parameters of the revealed stellar pairs. The binarity of the brightest of these stars, J1158+4239 (GJ 3697), has been confirmed. Four sessions of speckle observations with the BTA SAO RAS telescope and one session with the 2.5-m CO telescope have been carried out in 2015–2016. The weighted mean estimates of the pair parameters are ρ = 286.5 ± 1.2 mas and θ = 230.24◦ ± 0.16◦ at the epoch B2015.88248. The magnitude difference between the pair stars is Δm = 0.55 ± 0.03 (a filter with a central wavelength of 800 nm and a FWHM of 100 nm) and Δm = 0.9 ± 0.1 (an R filter).",
keywords = "astrometry, binary stars, individual stars: J1158+4239 (GJ 3697), techniques: image processing",
author = "Khovrichev, {M. Yu} and Kulikova, {A. M.} and Sokov, {E. N.} and Dyachenko, {V. V.} and Rastegaev, {D. A.} and Beskakotov, {A. S.} and Balega, {Yu Yu} and Safonov, {B. S.} and Dodin, {A. V.} and Vozyakova, {O. V.}",
note = "Publisher Copyright: {\textcopyright} 2016, Pleiades Publishing, Inc. Copyright: Copyright 2016 Elsevier B.V., All rights reserved.",
year = "2016",
month = oct,
day = "1",
doi = "10.1134/S1063773716100054",
language = "English",
volume = "42",
pages = "686--692",
journal = "Astronomy Letters",
issn = "1063-7737",
publisher = "МАИК {"}Наука/Интерпериодика{"}",
number = "10",

}

RIS

TY - JOUR

T1 - Detection of the binarity of the star J1158+4239

AU - Khovrichev, M. Yu

AU - Kulikova, A. M.

AU - Sokov, E. N.

AU - Dyachenko, V. V.

AU - Rastegaev, D. A.

AU - Beskakotov, A. S.

AU - Balega, Yu Yu

AU - Safonov, B. S.

AU - Dodin, A. V.

AU - Vozyakova, O. V.

N1 - Publisher Copyright: © 2016, Pleiades Publishing, Inc. Copyright: Copyright 2016 Elsevier B.V., All rights reserved.

PY - 2016/10/1

Y1 - 2016/10/1

N2 - One of the goals of the Pulkovo program of research on stars with large proper motions is to reveal among the low-luminosity stars those that have evidence of binarity. Twelve astrometric binary candidates from the Pulkovo list have been included in the program of speckle observations with the BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS) and the 2.5-m telescope at the Caucasus Observatory (CO) of the Sternberg Astronomical Institute of the Moscow State University to confirm their binarity and then to determine the parameters of the revealed stellar pairs. The binarity of the brightest of these stars, J1158+4239 (GJ 3697), has been confirmed. Four sessions of speckle observations with the BTA SAO RAS telescope and one session with the 2.5-m CO telescope have been carried out in 2015–2016. The weighted mean estimates of the pair parameters are ρ = 286.5 ± 1.2 mas and θ = 230.24◦ ± 0.16◦ at the epoch B2015.88248. The magnitude difference between the pair stars is Δm = 0.55 ± 0.03 (a filter with a central wavelength of 800 nm and a FWHM of 100 nm) and Δm = 0.9 ± 0.1 (an R filter).

AB - One of the goals of the Pulkovo program of research on stars with large proper motions is to reveal among the low-luminosity stars those that have evidence of binarity. Twelve astrometric binary candidates from the Pulkovo list have been included in the program of speckle observations with the BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS) and the 2.5-m telescope at the Caucasus Observatory (CO) of the Sternberg Astronomical Institute of the Moscow State University to confirm their binarity and then to determine the parameters of the revealed stellar pairs. The binarity of the brightest of these stars, J1158+4239 (GJ 3697), has been confirmed. Four sessions of speckle observations with the BTA SAO RAS telescope and one session with the 2.5-m CO telescope have been carried out in 2015–2016. The weighted mean estimates of the pair parameters are ρ = 286.5 ± 1.2 mas and θ = 230.24◦ ± 0.16◦ at the epoch B2015.88248. The magnitude difference between the pair stars is Δm = 0.55 ± 0.03 (a filter with a central wavelength of 800 nm and a FWHM of 100 nm) and Δm = 0.9 ± 0.1 (an R filter).

KW - astrometry

KW - binary stars

KW - individual stars: J1158+4239 (GJ 3697)

KW - techniques: image processing

UR - http://www.scopus.com/inward/record.url?scp=84992109788&partnerID=8YFLogxK

U2 - 10.1134/S1063773716100054

DO - 10.1134/S1063773716100054

M3 - Article

AN - SCOPUS:84992109788

VL - 42

SP - 686

EP - 692

JO - Astronomy Letters

JF - Astronomy Letters

SN - 1063-7737

IS - 10

ER -

ID: 76242788