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Neutral material around the B[e] supergiant star LHA115-S 65 An outflowing disk or a detached Keplerian rotating disk?
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SYSNO ASEP 0354843 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Neutral material around the B[e] supergiant star LHA115-S 65 An outflowing disk or a detached Keplerian rotating disk? Tvůrce(i) Kraus, Michaela (ASU-R) RID, ORCID
Borges Fernandes, M. (BR)
de Araújo, F. X. (BR)Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
July, č. 517 (2010), A30/1-A30/13Poč.str. 13 s. Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova supergiants ; circumstellar matter ; outflows Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika CEP KJB300030701 GA AV ČR - Akademie věd CEZ AV0Z10030501 - ASU-R (2005-2011) UT WOS 000280929400040 DOI 10.1051/0004-6361/200913964 Anotace The B[e] supergiant LHA 115-S 65 (in short: S 65) in the Small Magellanic Cloud is one of the two most rapidly rotating B[e] stars known. Its almost edge-on orientation allows a detailed kinematical study of its optically thin forbidden emission lines. With a focus on the rather strong [Oi] lines, we intend to test the two plausible disk scenarios: the outflowing and the Keplerian rotating disk. Both disk scenarios deliver reasonably good fits to the line luminosities and profiles of the [Oi] lines. Nevertheless, the Keplerian disk model seems to be the more realistic one, because it also agrees with the kinematics derived from the large number of additional lines in the spectrum. As additional support for the presence of a high-density, gaseous disk, the spectrum shows two very intense and clearly double-peaked [Caii] lines. We discuss a possible disk-formation mechanism, and similarities between S 65 and the group of Luminous Blue Variables. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2011
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