Searching for δ Scuti-type pulsation and characterising northern pre-main-sequence field stars

• Published in: Astronomy and astrophysics (Berlin) 2014-08, Vol.568, p.1-14
• Main Authors: Díaz-Fraile, D., Rodríguez, E., Amado, P. J.
• Format: Article
• Language: English
• Subjects: asteroseismology; Astronomy; Herbig Ae/Be; Hertzsprung-Russell and C-M diagrams; Hertzsprung-Russell diagram; Instability; Luminosity; Photometry; Pulsation; Searching; Stability; Stars; stars: fundamental parameters; stars: pre-main sequence; stars: variables: T Tauri; stars: variables: δScuti
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201423478

Context. Pre-main-sequence (PMS) stars are objects evolving from the birthline to the zero-age main sequence (ZAMS). Given a mass range near the ZAMS, the temperatures and luminosities of PMS and main-sequence stars are very similar. Moreover, their evolutionary tracks intersect one another causing some ambiguity in the determination of their evolutionary status. In this context, the detection and study of pulsations in PMS stars is crucial for differentiating between both types of stars by obtaining information of their interiors via asteroseismic techniques. Aims. A photometric variability study of a sample of northern field stars, which previously classified as either PMS or Herbig Ae/Be objects, has been undertaken with the purpose of detecting δ Scuti-type pulsations. Determination of physical parameters for these stars has also been carried out to locate them on the Hertzsprung-Russell diagram and check the instability strip for this type of pulsators. Methods. Multichannel photomultiplier and CCD time series photometry in the uvby Strömgren and BVI Johnson bands were obtained during four consecutive years from 2007 to 2010. The light curves have been analysed, and a variability criterion has been established. Among the objects classified as variable stars, we have selected those which present periodicities above 4 d-1, which was established as the lowest limit for δ Scuti-type pulsations in this investigation. Finally, these variable stars have been placed in a colour–magnitude diagram using the physical parameters derived with the collected uvbyβ Strömgren-Crawford photometry. Results. Five PMS δ Scuti- and three probable β Cephei-type stars have been detected. Two additional PMS δ Scuti stars are also confirmed in this work. Moreover, three new δ Scuti- and two γ Doradus-type stars have been detected among the main-sequence objects used as comparison or check stars.