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Astronomy Astrophysics A&A 408, 1047–1055 (2003) Astronomy DOI: 10.1051/0004-6361:20031011 & c ESO 2003 Astrophysics Multisite observations of the PMS δ Scuti star V351 Ori?;?? V. Ripepi1,M.Marconi1,S.Bernabei2;3,F.Palla4,F.J.G.Pinheiro5,D.F.M.Folha5,T.D.Oswalt6,L.Terranegra1, A. Arellano Ferro7,X.J.Jiang8,J.M.Alcal´a1, S. Marinoni2,M.J.P.F.G.Monteiro5, M. Rudkin6, and K. Johnston6 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 Astrof´ısica, Universidad de La Laguna, Avda. Astrofisico F. S´anchez sn, 30071 La Laguna, Spain 4 INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy 5 Centro de Astrof´ısica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 6 Florida Inst. Technology, 150 W Univ. Blvd., Melbourne, FL 32901-6988, USA 7 Instituto de Astronom´ıa, UNAM, Apdo. Postal 70-264, M´exico D.F., CP 04510, M´exico 8 National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, PR China Received 5 September 2002 / Accepted 20 June 2003 Abstract. We present the results of multisite observations spanning two years on the pre–main-sequence (PMS) star V351 Ori. A total of around 180 hours of observations over 29 nights have been collected, allowing us to measure five different periodic- ities, most likely related to the δ Scuti variability of V351 Ori. Comparison with the predictions of linear nonadiabatic radial pulsation models put stringent constraints on the stellar parameters and indicate that the distance to V351 Ori is intermediate between the lower limit measured by Hipparcos (210 pc) and that of the Orion Nebula (450 pc). However, radial pulsation mod- els are unable to reproduce all of the observed frequencies with a single choice of (M , L ,andTeff), suggesting the presence of additional nonradial modes. ∗ ∗ Key words. stars: variables: δ Scuti – stars: oscillations – stars: pre-main sequence – stars: fundamental parameters – stars: individual: V351 Ori 1. Introduction The initial evidence has stimulated the theoretical inves- tigation of the PMS instability strip, based on nonlinear con- δ Scuti stars are usually associated with the main- vective hydrodynamical models (Marconi & Palla 1998). As a sequence (MS) or post-MS evolutionary phases. To date, about result, the topology of the instability strip for the first three ra- ten intermediate-mass pre–main-sequence (PMS) stars have dial modes was identified and a list of possible PMS pulsating been found to pulsate with timescales typical of δ Scuti candidates, mainly Herbig Ae stars, was selected on the ba- variables and a growing interest in these young objects has sis of their spectral types. Then, a series of observing runs has developed in the last few years (see Marconi et al. 2001, here- been carried out searching for δ Scuti-type photometric vari- after M01; Marconi et al. 2002, hereafter M02, and refer- ations with periods of minutes to a few hours and amplitudes ences therein). The first two candidates were discovered by less than a few tenths of a magnitude among those stars in- Breger (1972) in the young cluster NGC 2264. The existence side or close to the theoretical instability strip. These studies of PMS δ Scuti stars was later confirmed by observations of the have confirmed the δ Scuti variability of HD 104237 (Kurtz & short term variability of the Herbig Ae stars HR 5999 (Kurtz & Muller 1999), HR 5999 (Kurtz & Catala 2001), and eight ad- Marang 1995) and HD 104237 (Donati et al. 1997). ditional candidates have been identified (see Kurtz & Muller 2001; M01; M02, Ripepi & Marconi 2003). Among the new discoveries, V351 Ori is a particularly in- Send offprint requests to: V. Ripepi, e-mail: [email protected] teresting object. The star is characterized by strong long-term ? Based on observations collected at the: Loiano Observatory photometric variations, attributed to extinction by circumstellar (Italy), San Pedro Martir Observatory (M´exico), OGS at Teide Observatory (Spain), JKT at Roque de los muchachos Observatory dust clouds. This property has been considered a sign of youth, (Spain), Beijing Astronomical Observatory (China), SARA signaling the transition from an active PMS phase to the arrival Observatory at Kitt Peak, which is owned and operated by the on the main sequence. Similar behavior has been observed in Southeastern Association for Research in Astronomy. other well known Herbig Ae stars, such as BN Ori, LkHα 234 ?? Table 3 in only available in electronic form at and UX Ori (e.g., Herbst & Shevchenko 1998). The spectral http://www.edpsciences.org properties of V351 Ori include the presence of Hα emission Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20031011 1048 V. Ripepi et al.: Multisite observations of the PMS δ Scuti star V351 Ori Table 1. List of telescopes and instruments involved in the multisite campaign. Observatory Telescope Instrument Comp. Star SAAO (S. Africa) 0.5 m Modular Photometer HD 290826 Roque de los Muchachos (Spain) 1.0 m JKT SITe2 2048 2048 CCD HD 290826 × Beijing Astronomical Observatory – BAO (China) 0.85 m Three Channel Photometer HD 290826 Loiano (Italy) 1.5 m Three Channel Photometer (TTCP) HD 290826 San Pedro Martir – SPM (Mexico) 1.5 m Danish (uvby) Photometer HD 290826 Kitt Peak National Observatory (USA) 0.9 m SARA 512 512 CCD HD 38248 Teide (Spain) 1.0 m OGS 1024× 1024 CCD HD 38248 × Table 2. Properties of V351 Ori and comparison stars. five different countries. In this paper, we present the results of this campaign. The organization of the paper is the following: Star AR Dec V Sp. T. in Sect. 2 we present details on observations and data reduc- (J2000) (J2000) (mag) tion; the frequency analysis is reported in Sect. 3 and results are compared with those obtained in other works and with the pre- V351 Ori 05 44 18.8 +00 08 40.4 8.9 A7 dictions of pulsating models in Sect. 4; the conclusions close HD 38248 05 44 23.8 +00 05 08.2 9.0 A3 HD 290826 05 44 00.4 +00 15 33.0 10.0 F5 the paper. 2. Observations and data reduction and a pronounced inverse P Cygni profile (van den Ancker et al. 1996), the SI λ1296 Å and OI λ1304 Å ultraviolet lines (Valenti Six observatories were involved in the observational campaign. et al. 2000), and a broad infrared excess (van den Ancker et al. They are listed in Table 1 together with the telescopes and in- 1997). Altogether, these features clearly reveal an active phase struments used. The observations have been supplemented by of interaction with the circumstellar environment. On the other data obtained at the SAAO during the same period (see BKW). hand, the possibility that V351 Ori is a post-MS star has been Two comparison stars (HD 38248 and HD 290826) have been put forward in the literature. Evidence in this sense comes from used during the observations, depending on the constraints set the lack of a reflection nebulosity, the absence of dense molecu- by the different instruments (e.g by the field of view of the CCD lar gas around the star, and a space velocity which indicates that etc.). Some information on these objects is given in Table 2, the star is approaching Orion and hence is not kinematically along with the same data for V351 Ori. For completeness, the linked to the star forming region. Spectral analysis of hydrogen last column of Table 1 indicates the comparison star used at absorption lines also show some peculiarities (Koval’chuck & each telescope. Pugach 1998; see also M01 for details). Recently, on the basis The multisite observations on V351 Ori were performed in of high dispersion echelle spectra, Balona et al. (2002, here- the Johnson V filter over around 2 years. We can divide the after BKW) have provided further evidence that V351 Ori is campaigns in: 1) winter 2001 (Sept. 2001–Feb. 2002); 2) win- indeed a PMS star. ter 2002 (Oct.–Dec. 2002). In total, we gathered about 180 hour As already remarked, the interest for V351 Ori lies in the of observations over 29 nights. The detailed log of the observa- fact that it pulsates. Marconi et al. (2000) and M01 have inter- tions is given in Table 3. preted the frequencies observed in the light curve of V351 Ori as due to pulsations in a mixture of several radial modes. In par- 2.1. Details on single site observations ticular, in M01 four of the six observed frequencies have been simultaneously reproduced by a linear nonadiabatic pulsation The observations obtained at SAAO are described in BKW. model with mass M = 1:8 M , luminosity L = 13:87 L and Considering the BAO and Loiano observations, in both ∗ ∗ effective temperature Teff = 7350 K. However, the compari- cases the instrument was a three channel photome- son of the observed periods with model predictions could not ter (see www.bao.ac.cn for the BAO instrument and help distinguishing whether the star is in the PMS or post-MS www.na.astro.it/ silvotti/TTCP.html for the TTCP in evolutionary phase of its evolution, even if the solution is con- Loiano). These instruments∼ allow the simultaneous observa- sistent with the distance determined by Hipparcos. The latter, tion of the variable and comparison stars, as well as the sky. if correct, implies that V351 Ori is much closer than the Orion Thus, the time sampling can be very short: for V351 Ori we complex.
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