Ultraviolet and visual flux and line variations of one of the least variable Bp stars HD 64740

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F13%3A00066262" target="_blank" >RIV/00216224:14310/13:00066262 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201221018" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201221018</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201221018" target="_blank" >10.1051/0004-6361/201221018</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Ultraviolet and visual flux and line variations of one of the least variable Bp stars HD 64740

Popis výsledku v původním jazyce

The light variability of hot magnetic chemically peculiar stars is typically caused by the flux redistribution in spots with peculiar abundance. This raises the question why some stars with surface abundance spots show significant rotational light variability, while others do not. Aims: We study the Bp star HD 64740 to investigate how its remarkable inhomogeneities in the surface distribution of helium and silicon, and the corresponding strong variability of many spectral lines, can result in one of thefaintest photometric variabilities among the Bp stars. Methods: We used model atmospheres and synthetic spectra calculated for the silicon and helium abundances from surface abundance maps to predict the ultraviolet and visual light and line variabilityof HD 64740. The predicted fluxes and line profiles were compared with the observed ones derived with the IUE, HST, and Hipparcos satellites and with spectra acquired using the FEROS spectrograph at the 2.2 m MPG/ESO telescope in La Sill

Název v anglickém jazyce

Ultraviolet and visual flux and line variations of one of the least variable Bp stars HD 64740

Popis výsledku anglicky

The light variability of hot magnetic chemically peculiar stars is typically caused by the flux redistribution in spots with peculiar abundance. This raises the question why some stars with surface abundance spots show significant rotational light variability, while others do not. Aims: We study the Bp star HD 64740 to investigate how its remarkable inhomogeneities in the surface distribution of helium and silicon, and the corresponding strong variability of many spectral lines, can result in one of thefaintest photometric variabilities among the Bp stars. Methods: We used model atmospheres and synthetic spectra calculated for the silicon and helium abundances from surface abundance maps to predict the ultraviolet and visual light and line variabilityof HD 64740. The predicted fluxes and line profiles were compared with the observed ones derived with the IUE, HST, and Hipparcos satellites and with spectra acquired using the FEROS spectrograph at the 2.2 m MPG/ESO telescope in La Sill

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%2F12%2F0217" target="_blank" >GAP209/12/0217: Multispektrální proměnnost horkých hvězd a její příčiny</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

2013

Kód důvěrnosti údajů

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

Název periodika

Astronomy and Astrophysics

ISSN

0004-6361

e-ISSN

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Svazek periodika

556

Číslo periodika v rámci svazku

léto

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

11

Strana od-do

"A18"-"1"-"A18"-"11"

Kód UT WoS článku

000323893500018

EID výsledku v databázi Scopus

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