A multisite photometric campaign on the pre-main-sequence δ Scuti pulsator IP Persei

¹ INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131, Napoli, Italy
² INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
³ Departimento de Astrofísica, Universidad de La Laguna, Avda. Astrofisico F. Sánchez sn, 30071 La Laguna, Spain
⁴ INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy
⁵ Instituto de Astronomía, UNAM, Apdo. Postal 70-264, México D.F., CP 04510, México
⁶ INAF-Osservatorio Astrofisico di Catania, Città Universitaria, 95125 Catania, Italy
⁷ National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, PR China
⁸ Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea
⁹ Dipartimento di Fisica e Astronomia dell'Universitá, Sezione Astrofisica, Cittá Universitaria, 95123 Catania, Italy.
¹⁰ DMA-Faculdade de Ciências and Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
¹¹ Florida Institute Technology, 150 W Univ. Blvd., Melbourne, FL 32901-6988, USA
¹² Institute for Astronomy (IfA), University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
¹³ Institute of Theoretical Physics & Astronomy, Vilnius University, Gostauto 12 Vilnius, Lithuania
¹⁴ Instituto de Astrofísica de Andalucía, CSIC, Apdo. 3004, 18080 Granada, Spain
¹⁵ Dipartimento di Scienze Fisiche, Università Federico II, Complesso Monte S. Angelo, 80126, Napoli, Italy

Received: 6 September 2005
Accepted: 1 December 2005

Abstract

We present the results of a photometric multisite campaign on the δ Scuti Pre-Main-Sequence star IP Per. Nine telescopes have been involved in the observations, with a total of about 190 h of observations over 38 nights. Present data confirms the multiperiodic nature of this star and leads to the identification of at least nine pulsational frequencies. Comparison with the predictions of linear non-adiabatic radial pulsation models allowed us to identify only five of the nine observed frequencies, and to constrain the position of IP Per in the HR diagram. The latter is in good agreement with the empirical determination of the stellar parameters obtained by Miroshnichenko et al. (2001, A&A, 377, 854). An initial interpretation of the observed frequencies using the Aarhus non-radial pulsation code suggests that three frequencies could be associated with non-radial () modes. Finally, we present new evolutionary and pulsation models at lower metallicity () to take into account the possibility that IP Per is metal deficient, as indicated by Miroshnichenko et al. (2001, A&A, 377, 854).