Oscillations in the PMS delta Scuti star V346 Ori

• Type: Article in International Scientific Journal
• Date: 2003

Authors

Pinheiro, FJG (Author) Other; Folha, DFM (Author) Other; Marconi, A (Author) Other; Ripepi, V (Author) Other; Palla, F (Author) Other; Monteiro, MJPFG (Author) FCUP; Bernabei, S (Author) Other

Journal

Title: Astronomy and Astrophysics

Vol. 399

Pages: 271-274

ISSN: 0004-6361

Publisher: EDP Sciences

Indexing

ISI Web of Knowledge - 13 Citations

Scopus - 15 Citations

Scientific classification

FOS: Natural sciences > Physical sciences

CORDIS: Physical sciences ; Physical sciences > Astronomy > Astrophysics ; Physical sciences > Astronomy

Other information

Authenticus ID: P-000-HSZ

DOI: 10.1051/0004-6361:20021792

Resumo (PT): We report the discovery of periodicities in the light curve of the Pre-Main Sequence (PMS) Herbig Ae star V346 Ori. We interpret variations in the light curve of the star as the superposition of at least two periodic signals that result from delta Scuti-type stellar oscillations. The computation of linear non-adiabatic radial pulsation models for PMS stars reproduces these periods for a 1.55 Msun star with Teff = 7410 K and log L/Lsun = 0.74 pulsating in the fundamental and in the second overtone. If our assumption of radial oscillations is indeed correct, the star's location on the HR diagram places it at a distance significantly smaller than that of the Orion star forming region, hence raising questions regarding the evolutionary status of V346 Ori. Observations with better time sampling and spanning a longer period of time are needed if the latter question is to be addressed fully.

Abstract (EN): We report the discovery of periodicities in the light curve of the Pre-Main Sequence (PMS) Herbig Ae star V346 Ori. We interpret variations in the light curve of the star as the superposition of at least two periodic signals that result from delta Scuti-type stellar oscillations. The computation of linear non-adiabatic radial pulsation models for PMS stars reproduces these periods for a 1.55 M(circle dot) star with T(eff) = 7410 K and log L/L(circle dot) = 0.74 pulsating in the fundamental and in the second overtone. If our assumption of radial oscillations is indeed correct, the star's location on the HR diagram places it at a distance significantly smaller than that of the Orion star forming region, hence raising questions regarding the evolutionary status of V346 Ori. Observations with better time sampling and spanning a longer period of time are needed if the latter question is to be addressed fully.

Language: English

Type (Professor's evaluation): Scientific

No. of pages: 4