1 / 10

Characterization and Analysis of Gamma Doradus Stars within the SISMO Field of View

The Gamma Doradus Thematic Team consists of 35 researchers from various institutes specializing in astrophysics, focusing on the characterization of Gamma Doradus (g Dor) stars. Our primary goals include analyzing variability using spectroscopy and photometry, identifying oscillation modes, and simulating the behavior of g Dor stars within the EXO field of view. We aim to enhance our understanding of these stars' abundances, binarity, and fundamental parameters while offering insights into expected variable types like pulsating stars. Join us in exploring the complexities of g Dor stars.

galvin-hatfield
Download Presentation

Characterization and Analysis of Gamma Doradus Stars within the SISMO Field of View

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Doradus Thematic Team http://www.obs-nice.fr/gdor_corot/index.html wggdor@obs-nice.fr About 35 persons involved in different institutes: OCA/Gemini/Cassiopée, LUAN, Institut d’Astrophysique de Liège, KU Leuven, IAA, IAC, UNAM, Vienna University, Royal Observatory Belgium, OAB, Observatoire de Genève, Observatoire de Paris, Konkoly Observatory Different skills: Ground based observations, frequency analysis, mode identification, modelling

  2. Goals of the Thematic Team • Characterization of g Dor in the SISMO FoV • Variability: spectroscopy and photometry (timescales, LPV…) • Mode identification (moments, FDI, photometric amplitudes…) • Abundances • Binarity & fundamental parameters • Simulation of g Dor behaviour in the EXO FoV • Expected variables (pulsating, geometric, cataclysmic) • Signal determination (relative photometric precision ~10-4) • Mode identification from CDC 3-colour light curves

  3. Candidates in the SISMO fields • From COROTSKY: • HD 49434 [9]: • Teff = 7346 +- 69 K • log g = 4.14 +- 0.2 • [Fe/H] = -0.13 +- 0.14 dex • v sini = 82 km/s • M ~ 1.55 Mo • HD 171834 [10]: • Teff = 6879 +- 67 K • log g = 4.05 +- 0.3 • [Fe/H] = -0.22 +- 0.2 dex • v sini = 64 km/s • M ~ 1.40 Mo Poretti et al. 2005

  4. HD 49434 Last photometry (Konkoly) in 2006, but too scarce data Spectroscopy (OHP) in 2003 & 2006, but bad weather: no periodic signal determined

  5. HD 49434 SPM & SN photometry, winter 2005-2006, from Poretti et al.:

  6. HD 171834: AURELIE spectra

  7. HD 171834: MEZCAL spectra

  8. Modelling See poster “Structure & Evolution of Gamma Doradus Stars” by A. Miglio, J. Montalban & S. Theado Study of Dupret & Grighacène:

  9. Modelling: expected frequencies From Dupret & Grighacène: HD 49434 HD 171834

  10. Runs LRA1: HD 49434 IREM01 (~60 d): HD 49434 LRC2: HD 171834 SRA: NGC 2264 field: HD 49015 PMS thematic team (K. Zwintz) ? SRC2: HD 175337 (bf): • Teff = 7117+- 67 K • log g = 4.18 +- 0.09 • [FE/H] = 0.06 +- 0.04 • v. sini = 38 km/s

More Related