About: CNO driven winds of hot first stars

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Description	We show that hot first stars do not have any wind driven purely by hydrogen or helium. However, during the evolution of these stars the CNO elements may emerge on their surfaces due to the mixing processes. Contrary to hydrogen and helium, these elements are able to drive a stellar wind. Consequently, evolved first stars may have winds driven purely by CNO elements. We study the properties of such stellar winds for different abundance of CNO elements and discuss their influence on the surrounding environment. We show that CNO driven winds exist in more luminuous stars. Moreover, for very hot stars CNO elements are too much ionized to drive a wind. In most cases the derived mass-loss rate is smaller than that calculated with solar mixture of elements. This is connected with the fact that in the present hot stars heavier elements (as iron) are the most important element that influence the wind mass-loss rate. We show that hot first stars do not have any wind driven purely by hydrogen or helium. However, during the evolution of these stars the CNO elements may emerge on their surfaces due to the mixing processes. Contrary to hydrogen and helium, these elements are able to drive a stellar wind. Consequently, evolved first stars may have winds driven purely by CNO elements. We study the properties of such stellar winds for different abundance of CNO elements and discuss their influence on the surrounding environment. We show that CNO driven winds exist in more luminuous stars. Moreover, for very hot stars CNO elements are too much ionized to drive a wind. In most cases the derived mass-loss rate is smaller than that calculated with solar mixture of elements. This is connected with the fact that in the present hot stars heavier elements (as iron) are the most important element that influence the wind mass-loss rate. (en)
Title	CNO driven winds of hot first stars CNO driven winds of hot first stars (en)
skos:prefLabel	CNO driven winds of hot first stars CNO driven winds of hot first stars (en)
skos:notation	RIV/00216224:14310/09:00029216!RIV10-GA0-14310___
http://linked.open...avai/riv/aktivita	P
http://linked.open...avai/riv/aktivity	P(GA205/07/0031)
http://linked.open...vai/riv/dodaniDat	2010
http://linked.open...aciTvurceVysledku	Krtička, Jiří Kubát, Jiří
http://linked.open.../riv/druhVysledku	D - Článek ve sborníku
http://linked.open...iv/duvernostUdaju	S - Úplné a pravdivé údaje nepodléhající ochraně podle zvláštních právních předpisů
http://linked.open...titaPredkladatele	Masarykova univerzita / Přírodovědecká fakulta
http://linked.open...dnocenehoVysledku	307367
http://linked.open...ai/riv/idVysledku	RIV/00216224:14310/09:00029216
http://linked.open...riv/jazykVysledku	eng - angličtina
http://linked.open.../riv/klicovaSlova	hot stars - first stars - stellar wind - hydodynamics (en)
http://linked.open.../riv/klicoveSlovo	hot stars
http://linked.open...ontrolniKodProRIV	[5215151422EC]
http://linked.open...v/mistoKonaniAkce	Rapallo, Italie
http://linked.open...i/riv/mistoVydani	Cambridge, Velka Britanie
http://linked.open...i/riv/nazevZdroje	Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies
http://linked.open...in/vavai/riv/obor	BN
http://linked.open...ichTvurcuVysledku	2 (xsd:int)
http://linked.open...cetTvurcuVysledku	2 (xsd:int)
http://linked.open...vavai/riv/projekt	Stellar winds of first stars in the Universe
http://linked.open...UplatneniVysledku	2009
http://linked.open...iv/tvurceVysledku	Krtička, Jiří Kubát, Jiří
http://linked.open...vavai/riv/typAkce	WRD - Světová
http://linked.open...ain/vavai/riv/wos	000262601300027
http://linked.open.../riv/zahajeniAkce	2008-01-01 (xsd:date)
number of pages	1 (xsd:int)
http://purl.org/ne...btex#hasPublisher	Cambridge University Press
https://schema.org/isbn	978-0-521-88986-5
http://localhost/t...ganizacniJednotka	14310
is http://linked.open...avai/riv/vysledek of	CNO driven winds of hot first stars CNO driven winds of hot first stars CNO driven winds of hot first stars CNO driven winds of hot first stars

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