THE PHYSICAL NATURE AND ORBITAL BEHAVIOR OF THE ECLIPSING SYSTEM DK CYGNI
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F15%3A10315340" target="_blank" >RIV/00216208:11320/15:10315340 - isvavai.cz</a>
Výsledek na webu
<a href="http://dx.doi.org/10.1088/0004-6256/149/6/194" target="_blank" >http://dx.doi.org/10.1088/0004-6256/149/6/194</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1088/0004-6256/149/6/194" target="_blank" >10.1088/0004-6256/149/6/194</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
THE PHYSICAL NATURE AND ORBITAL BEHAVIOR OF THE ECLIPSING SYSTEM DK CYGNI
Popis výsledku v původním jazyce
New CCD photometry is presented for the hot overcontact binary DK Cyg together with reasonable explanations for the light and period variations. Historical light and velocity curves from 1962 to 2012 were simultaneously analyzed with the Wilson-Devinney(W-D) synthesis code. The brightness disturbances were satisfactorily modeled by applying a magnetic cool spot on the primary star. Based on 261 times of minimum light that include 116 new timings and span more than 87 years, a period study reveals thatthe orbital period has varied due to a periodic oscillation superimposed on an upward parabola. The period and semi-amplitude of the modulation are about 78.1 years and 0.0037 days, respectively. This detail is interpreted as a light-travel-time effect due to a circumbinary companion with a minimum mass of M-3 = 0.065M(circle dot), within the theoretical limit of similar to 0.07M(circle dot) for a brown dwarf star. The observed period increase at a fractional rate of +2.74 x 10(-10) is i
Název v anglickém jazyce
THE PHYSICAL NATURE AND ORBITAL BEHAVIOR OF THE ECLIPSING SYSTEM DK CYGNI
Popis výsledku anglicky
New CCD photometry is presented for the hot overcontact binary DK Cyg together with reasonable explanations for the light and period variations. Historical light and velocity curves from 1962 to 2012 were simultaneously analyzed with the Wilson-Devinney(W-D) synthesis code. The brightness disturbances were satisfactorily modeled by applying a magnetic cool spot on the primary star. Based on 261 times of minimum light that include 116 new timings and span more than 87 years, a period study reveals thatthe orbital period has varied due to a periodic oscillation superimposed on an upward parabola. The period and semi-amplitude of the modulation are about 78.1 years and 0.0037 days, respectively. This detail is interpreted as a light-travel-time effect due to a circumbinary companion with a minimum mass of M-3 = 0.065M(circle dot), within the theoretical limit of similar to 0.07M(circle dot) for a brown dwarf star. The observed period increase at a fractional rate of +2.74 x 10(-10) is i
Klasifikace
Druh
J<sub>x</sub> - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)
CEP obor
BN - Astronomie a nebeská mechanika, astrofyzika
OECD FORD obor
—
Návaznosti výsledku
Projekt
—
Návaznosti
Z - Vyzkumny zamer (s odkazem do CEZ)
Ostatní
Rok uplatnění
2015
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Astronomical Journal
ISSN
0004-6256
e-ISSN
—
Svazek periodika
149
Číslo periodika v rámci svazku
6
Stát vydavatele periodika
US - Spojené státy americké
Počet stran výsledku
8
Strana od-do
—
Kód UT WoS článku
000355250400017
EID výsledku v databázi Scopus
2-s2.0-84934875456