HD 143 418 - an interacting binary with the subsynchronously rotating primary

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F09%3A00038109" target="_blank" >RIV/00216224:14310/09:00038109 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/09:00038174

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

HD 143 418 - an interacting binary with the subsynchronously rotating primary

Popis výsledku v původním jazyce

HD 143 418 is a non-eclipsing close binary with orbital period Porb = 2.282520 d. The photometrically and spectroscopically dominant primary component is a normal A5V star in the middle of its stay on the main sequence with extremely slow, subsynchronousrotation (Prot about 12 d!). Its photometric monitoring since 1982 revealed orbitally modulated variations with changing form and amplitude. PCA disentangling extracted a constant part of light curves obviously caused by the ellipticity of the primary.Seasonal components of light curves may be related to the expected incidence of circumstellar matter ejected from tidally spinning up primary component. A possible scenario of the synchronization process is also briefly discussed.

Název v anglickém jazyce

HD 143 418 - an interacting binary with the subsynchronously rotating primary

Popis výsledku anglicky

HD 143 418 is a non-eclipsing close binary with orbital period Porb = 2.282520 d. The photometrically and spectroscopically dominant primary component is a normal A5V star in the middle of its stay on the main sequence with extremely slow, subsynchronousrotation (Prot about 12 d!). Its photometric monitoring since 1982 revealed orbitally modulated variations with changing form and amplitude. PCA disentangling extracted a constant part of light curves obviously caused by the ellipticity of the primary.Seasonal components of light curves may be related to the expected incidence of circumstellar matter ejected from tidally spinning up primary component. A possible scenario of the synchronization process is also briefly discussed.

Druh

O - Ostatní výsledky

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/MEB080832" target="_blank" >MEB080832: Rozložení energie ve spektrech chemicky pekuliárních hvězd a jeho proměnnost</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2009

Kód důvěrnosti údajů

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