THE PERIOD ANALYSIS OF V418 AQL, SU BOO, RV CVn, CR CAS, GV CYG, V432 PER, AND BD+42 2782

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F14%3A10286205" target="_blank" >RIV/00216208:11320/14:10286205 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-6256/147/6/130" target="_blank" >http://dx.doi.org/10.1088/0004-6256/147/6/130</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-6256/147/6/130" target="_blank" >10.1088/0004-6256/147/6/130</a>

Jazyk výsledku

angličtina

Název v původním jazyce

THE PERIOD ANALYSIS OF V418 AQL, SU BOO, RV CVn, CR CAS, GV CYG, V432 PER, AND BD+42 2782

Popis výsledku v původním jazyce

The minimum timings of eclipsing binaries V418 Aql, SU Boo, RV CVn, CR Cas, GV Cyg, V432 Per, and BD+ 42 2782 were collected and analyzed. Their long-term behavior was studied via period analysis, revealing a periodic term in eclipse times. We derived 576 new times of minimum. Hence, to describe the periodic variation, a thirdbody hypothesis was proposed and the resulting orbital periods are as follows: 70, 7.4, 53, 37, 27, 53, and 18 yr, respectively. For the system V432 Per an additional 9.5 yr variation was also found. The predicted minimum masses of these distant bodies were calculated and their detectability discussed. The light curves of SU Boo and RV CVn were analyzed using the PHOEBE program, resulting in physical parameters of the components.New variable stars in the field of V418 Aql were discovered.

Název v anglickém jazyce

THE PERIOD ANALYSIS OF V418 AQL, SU BOO, RV CVn, CR CAS, GV CYG, V432 PER, AND BD+42 2782

Popis výsledku anglicky

The minimum timings of eclipsing binaries V418 Aql, SU Boo, RV CVn, CR Cas, GV Cyg, V432 Per, and BD+ 42 2782 were collected and analyzed. Their long-term behavior was studied via period analysis, revealing a periodic term in eclipse times. We derived 576 new times of minimum. Hence, to describe the periodic variation, a thirdbody hypothesis was proposed and the resulting orbital periods are as follows: 70, 7.4, 53, 37, 27, 53, and 18 yr, respectively. For the system V432 Per an additional 9.5 yr variation was also found. The predicted minimum masses of these distant bodies were calculated and their detectability discussed. The light curves of SU Boo and RV CVn were analyzed using the PHOEBE program, resulting in physical parameters of the components.New variable stars in the field of V418 Aql were discovered.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GAP209%2F10%2F0715" target="_blank" >GAP209/10/0715: Přesné fyzikální vlastnosti horkých hvězd získané studiem dvojhvězd a vícenásobných soustav</a><br>

Návaznosti

Z - Vyzkumny zamer (s odkazem do CEZ)<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2014

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomical Journal

ISSN

0004-6256

e-ISSN

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Svazek periodika

147

Číslo periodika v rámci svazku

6

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

9

Strana od-do

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Kód UT WoS článku

000336262600006

EID výsledku v databázi Scopus

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