LIŠKA, Jiří. Analysis of the multiple system with chemically peculiar component phi Draconis. Monthly Notices of the Royal Astronomical Society. Priestley and Weale, roč. 461, č. 1, s. 939-947. ISSN 0035-8711. doi:10.1093/mnras/stw1355. 2016.
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Základní údaje
Originální název Analysis of the multiple system with chemically peculiar component phi Draconis
Autoři LIŠKA, Jiří (203 Česká republika, garant, domácí).
Vydání Monthly Notices of the Royal Astronomical Society, Priestley and Weale, 2016, 0035-8711.
Další údaje
Originální jazyk angličtina
Typ výsledku Článek v odborném periodiku
Obor 10308 Astronomy
Stát vydavatele Velká Británie a Severní Irsko
Utajení není předmětem státního či obchodního tajemství
WWW URL
Impakt faktor Impact factor: 4.961
Kód RIV RIV/00216224:14310/16:00094209
Organizační jednotka Přírodovědecká fakulta
Doi http://dx.doi.org/10.1093/mnras/stw1355
UT WoS 000383272500070
Klíčová slova anglicky binaries: spectroscopic; binaries: visual; stars: chemically peculiar; stars: individual: phi Dra; stars: variables: general
Štítky AKR, rivok
Změnil Změnila: Ing. Andrea Mikešková, učo 137293. Změněno: 11. 5. 2017 18:58.
Anotace
The star phi Dra comprises a spectroscopic binary and a third star that together form a visual triple system. It is one of the brightest chemically peculiar stars of the upper main sequence. Despite these facts, no comprehensive study of its multiplicity has been performed yet. In this work, we present a detailed analysis of the triple system based on available measurements. We use radial velocities taken from four sources in the literature in a re-analysis of the inner spectroscopic binary (Aab). An incorrect value of the orbital period of the inner system Aab about 27 d was accepted in literature more than 40 yr. A new solution of orbit with the 128-d period was determined. Relative position measurements of the outer visual binary system (AB) from Washington Double Star Catalog were compared with known orbital models. Furthermore, it was shown that astrometric motion in system AB is well described by the model of Andrade with a 308-yr orbital period. Parameters of A and B components were utilized to estimate individual brightness for all components and their masses from evolutionary tracks. Although we found several facts which support the gravitational bond between them, unbound solution cannot be fully excluded yet.
Návaznosti
GA13-10589S, projekt VaVNázev: Ztráta hmoty horkých hmotných hvězd
Investor: Grantová agentura ČR, Ztráta hmoty horkých hmotných hvězd
VytisknoutZobrazeno: 29. 3. 2024 02:36