1 Konkoly Observatory, MTA CSFK, Konkoly Thege M. út 15-17, 1121 Budapest, Hungary
2 Institut für Astrophysik, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria
3 Centro de Astrofísica, Universidade do Porto, rua das Estrelas, 4150-762 Porto, Portugal
4 Baja Astronomical Observatory, Szegedi út, Kt. 766, 6500 Baja, Hungary
5 ELTE Gothard-Lendület Research Group, Szent Imre herceg út 112, 9700 Szombathely, Hungary
6 Koninklijke Sterrenwacht van België, Ringlaan 3, 1180 Brussel, Belgium
7 INAF Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy
8 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
9 LESIA, Observatoire de Paris, site de Meudon, UMR CNRS 8109, associé à l’Université Pierre et Marie Curie (Paris 6) et à l’Université Paris-Diderot (Paris 7), 5 place J. Janssen, 92195 Meudon Cedex, France
10 Institut d’Astrophysique Spatiale, UMR8617, CNRS, Université Paris XI, Bâtiment 121, 91405 Orsay Cedex, France
Received: 13 March 2014
Accepted: 31 May 2014
Context. Pulsating stars in binary systems are ideal laboratories to test stellar evolution and pulsation theory, since a direct, model-independent determination of component masses is possible. The high-precision CoRoT photometry allows a detailed view of the frequency content of pulsating stars, enabling detection of patterns in their distribution. The object HD 51844 is such a case showing periastron brightening instead of eclipses.
Aims. We present a comprehensive study of the HD 51844 system, where we derive physical parameters of both components, the pulsation content and frequency patterns. Additionally, we obtain the orbital elements, including masses, and the chemical composition of the stars.
Methods. Time series analysis using standard tools was employed to extract the pulsation frequencies. Photospheric abundances of 21 chemical elements were derived by means of spectrum synthesis. We derived orbital elements both by fitting the observed radial velocities and the light curves, and we did asteroseismic modelling as well.
Results. We found that HD 51844 is a double lined spectroscopic binary. The determined abundances are consistent with δ Delphini classification. We determined the orbital period (33.498 ± 0.002 d), the eccentricity (0.484 ± 0.020), the mass ratio (0.988 ± 0.02), and the masses to 2.0 ± 0.2 M⊙ for both components. Only one component showed pulsation. Two p modes (f22 and f36) and one g mode (forb) may be tidally excited. Among the 115 frequencies, we detected triplets due to the frequency modulation, frequency differences connected to the orbital period, and unexpected resonances (3:2, 3:5, and 3:4), which is a new discovery for a δ Sct star. The observed frequency differences among the dominant modes suggest a large separation of 2.0−2.2 d-1, which are consistent with models of mean density of 0.063 g cm-3, and with the binary solution and TAMS evolutionary phase for the pulsating component. The binary evolution is in an intermediate evolutionary phase; the stellar rotation is super-synchronised, but circularisation of the orbit is not reached.
Key words: binaries: spectroscopic / stars: variables: δScuti / stars: abundances / stars: individual: HD 51844
Based on observations obtained with the HERMES spectrograph attached to the Mercator Telescope which is operated on the island of La Palma by the University of Leuven (IvS) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. The HERMES spectrograph is supported by the Fund for Scientific Research of Flanders (FWO), Belgium, the Research Council of K.U. Leuven, Belgium, the Fonds National de la Recherche Scientifique (FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland and the Thüringer Landessternwarte Tautenburg, Germany. Based on CoRoT space-based photometric data; the CoRoT space mission was developed and operated by the French space agency CNES, with the participation of ESA’s RSSD and Science Programmes, Austria, Belgium, Brazil, Germany, and Spain. Based on observations collected at La Silla Observatory, ESO (Chile) with the HARPS spectrograph at the 3.6 m telescope, under programme LP185.D-0056.
Table 9 is available in electronic form at http://www.aanda.org
© ESO, 2014