Počet záznamů: 1
V346 Centauri: early-type eclipsing binary with apsidal motion and abrupt change of orbital period
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SYSNO ASEP 0471733 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název V346 Centauri: early-type eclipsing binary with apsidal motion and abrupt change of orbital period Tvůrce(i) Mayer, P. (CZ)
Harmanec, P. (CZ)
Wolf, M. (CZ)
Nemravová, J. (CZ)
Prsa, A. (US)
Frémat, Y. (BE)
Zejda, M. (CZ)
Liška, J. (CZ)
Juryšek, Jakub (FZU-D) ORCID
Hoňková, K. (CZ)
Mašek, Martin (FZU-D) ORCIDCelkový počet autorů 11 Číslo článku A129 Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 591, Jul (2016), s. 1-9Poč.str. 9 s. Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova early-type stars ; binaries ; close stars Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika Obor OECD Astronomy (including astrophysics,space science) CEP LG15014 GA MŠMT - Ministerstvo školství, mládeže a tělovýchovy LG13007 GA MŠMT - Ministerstvo školství, mládeže a tělovýchovy GA14-17501S GA ČR - Grantová agentura ČR Způsob publikování Open access Institucionální podpora FZU-D - RVO:68378271 UT WOS 000379141300138 EID SCOPUS 84977138516 DOI 10.1051/0004-6361/201628655 Anotace New physical elements of the early B-type eclipsing binary V346 Cen are derived using the HARPS spectra downloaded from the ESO archive and also numerous photometric observations from various sources. A model of the observed times of primary and secondary minima that fits them best is a combination of the apsidal motion and an abrupt decrease in the orbital period from 6(d).322123 to 6(d).321843 (shortening by 24 s), which occurred somewhere around JD 2 439 000. Assumption of a secularly decreasing orbital period provides a significantly worse fit. Local times of minima and the final solution of the light curve were obtained with the program PHOEBE. Radial velocities of both binary components, free of line blending, were derived via 2D cross-correlation with a program built on the principles of the program TODCOR. The oxygen lines in the secondary spectra are weaker than those in the model spectra of solar chemical composition. Using the component spectra disentangled with the program KOREL,we find that both components rotate considerably faster than would correspond to the synchronization at periastron. The apside rotation known from earlier studies is confirmed and compared to the theoretical value. Pracoviště Fyzikální ústav Kontakt Kristina Potocká, potocka@fzu.cz, Tel.: 220 318 579 Rok sběru 2017 Elektronická adresa http://hdl.handle.net/11104/0269071
Počet záznamů: 1