Early Stage of Chemically Peculiar Stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F15%3A00081366" target="_blank" >RIV/00216224:14310/15:00081366 - isvavai.cz</a>

Výsledek na webu

—

DOI - Digital Object Identifier

—

Jazyk výsledku

angličtina

Název v původním jazyce

Early Stage of Chemically Peculiar Stars

Popis výsledku v původním jazyce

Chemically peculiar stars are known to be the main sequence objects and are characterized by a wide variety of element abundance patterns. They display abundance peculiarities of various chemical elements from helium to mercury in their photospheres. These are explained by the diffusion processes driven by the competition between the radiative levitation and gravitational settling. Current estimates suggest that about 10% of all the stars in the corresponding spectral range (B to F-type) belong to various CP groups. The most populous groups are the metallic line (Am) stars and the magnetic Bp/Ap objects. The reason and the time-scale for the rise of chemical peculiarities is still not known, so is for the role of the magnetic field. The investigation of very young CP stars can help to shed more light on these issues and to test the diffusion theory. However, so far only one pre-main sequence (PMS) Bp star is known.

Název v anglickém jazyce

Early Stage of Chemically Peculiar Stars

Popis výsledku anglicky

Chemically peculiar stars are known to be the main sequence objects and are characterized by a wide variety of element abundance patterns. They display abundance peculiarities of various chemical elements from helium to mercury in their photospheres. These are explained by the diffusion processes driven by the competition between the radiative levitation and gravitational settling. Current estimates suggest that about 10% of all the stars in the corresponding spectral range (B to F-type) belong to various CP groups. The most populous groups are the metallic line (Am) stars and the magnetic Bp/Ap objects. The reason and the time-scale for the rise of chemical peculiarities is still not known, so is for the role of the magnetic field. The investigation of very young CP stars can help to shed more light on these issues and to test the diffusion theory. However, so far only one pre-main sequence (PMS) Bp star is known.

Druh

D - Stať ve sborníku

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GP14-26115P" target="_blank" >GP14-26115P: Vstříc k jednotné škále metalicity pro otevřené hvězdokupy</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2015

Kód důvěrnosti údajů

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

Název statě ve sborníku

Physics and Evolution of Magnetic and Related Stars

ISBN

9781583818732

ISSN

—

e-ISSN

—

Počet stran výsledku

9

Strana od-do

148-156

Název nakladatele

Astronomical Society of the Pacific

Místo vydání

San Francisco

Místo konání akce

Nizhny Arkhyz, Russia

Datum konání akce

1. 1. 2014

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

000366452300018