Interpreting the spectral behavior of MWC 314
| Autor: | I. Busà, Antonio Frasca, Corinne Rossi, Michael Friedjung, E. Marilli, G. Muratorio, Anatoly S. Miroshnichenko |
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| Přispěvatelé: | Max-Planck-Institut für Radioastronomie (MPIFR), Génie Enzymatique et Cellulaire (GEC), Université de Technologie de Compiègne (UTC)-Université de Picardie Jules Verne (UPJV)-Centre National de la Recherche Scientifique (CNRS) |
| Rok vydání: | 2015 |
| Předmět: |
Absorption spectroscopy
Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Orbital eccentricity Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences 010309 optics symbols.namesake 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Emission spectrum 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Physics Orbital elements Balmer series Astronomy and Astrophysics Radial velocity Stars Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science symbols Astrophysics::Earth and Planetary Astrophysics Supergiant [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] |
| Zdroj: | Astronomy and Astrophysics-A&A Astronomy and Astrophysics-A&A, EDP Sciences, 2016, 585, ⟨10.1051/0004-6361/201527022⟩ |
| ISSN: | 0004-6361 |
| DOI: | 10.48550/arxiv.1510.06158 |
| Popis: | MWC 314 is one of the most luminous stars in the Milky Way. Its fundamental parameters are similar to those of LBVs, although no large photometric variations have been recorded. We analyzed the radial velocity (RV) variations displayed by the absorption lines from the star's atmosphere using high resolution optical spectra. The RV and profile variations of some permitted and forbidden emission lines of metallic ions and the behavior of the Balmer and HeI lines has been investigated as well. The RV of the absorption lines clearly shows a 60-day periodicity. A dense coverage of the RV curve allowed us to derive accurate orbital parameters. The RV of the FeII emission lines varies in the same way, but with a smaller amplitude. Additionally, the intensity ratio of the blue/red peaks of these emission lines correlates with the RV variations. The Balmer lines and {NII] lines display a nearly constant RV and no profile variations in phase with the orbital motion instead. The HeI-5876 \AA\ line shows a strongly variable profile with broad and blue-shifted absorption components reaching velocities of Comment: 9 pages, 9 figures, accepted for publication in Astronomy & Astrophysics |
| Databáze: | OpenAIRE |
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