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Calibration of stellar evolution using stellar pulsations

Calibration of stellar evolution using stellar pulsations. Marian Doru Suran, Nedelia Antonia Popescu Astronomical Institute of the Romanian Academy e-mail: suran@aira.astro.ro Supported by the Romanian Space Agency (ROSA) contract Nr. 124/30.09.2004. Abstract.

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Calibration of stellar evolution using stellar pulsations

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  1. Calibration of stellar evolution using stellar pulsations Marian Doru Suran, Nedelia Antonia Popescu Astronomical Institute of the Romanian Academy e-mail: suran@aira.astro.ro Supported by the Romanian Space Agency (ROSA) contract Nr. 124/30.09.2004

  2. Abstract Close to the main sequence the HR diagram is confusing as stars of similar global properties but with different stages of evolution occupy the same position. Pulsating stars (both pms and post-ms) have been discovered in this area. In some cases the young pms stars are recognized through specific characteristics – for instance the presence of nebulosity or high degree of activity. An alternative is to take advantage of the seismological information whenever it is possible. In this case the discrimination between pms and post-ms can be made using differences in their oscillatory frequency distributions in the low frequency range.

  3. Calibration method: • Stellar evolution: - CESAM vs. HENYEY(Bucharest); - 1.8M track (Figure 1, Table 2). • Evolutive pulsational diagram: - CESAM (osc.ad+nad) +LNANR (linear, nonadiabatic, nonradial, Suran, Bucharest); - 1.8M track(l=0-2, g,f,p,); - from pms  post-ms (Figure 2a,b); - 3 common points (pms/post-ms): a.,b.,c, (see Figure 1 and Table 1).

  4. Results - HAEBE stars: • Evolutive status: pms vs. post-ms: - V351 Ori (pt. c.)  t [P=14.33 (f2), penetrative post-ms ?!] [BKW,C,M,RP] Table 3, Figure 3a,b. • Physical parameters: - V1366 Ori (pts. a.,d.,e.) Te [A] Table 4, Figure 4 a,b,c.

  5. References: • Amado, P. J.; Moya, A.; Suárez, J. C.; Martín-Ruiz, S.; Garrido, R.; Rodríguez, E.; Catala, C.; Goupil, M. J., 2004, M.N.R.A.S.,352, pp. L11-L15 [A]; • Balona, L. A.; Koen, C.; van Wyk, F., 2003, M.N.R.A.S., 333, pp. 923-931 [BKW]; • Catala, C., 2003, Astrophysics and Space Science, pp. 53-60l [C] • Marconi, M.; Ripepi, V.; Palla, F.; Ruoppo, A., 2004, Communications in Asteroseismology, 145, pp. 61-66 [M]; • Ripepi, V.; Marconi, M.; Bernabei, S.; Palla, F.; Pinheiro, F. J. G.; Folha, D. F. M.; Oswalt, T. D.; Terranegra, L.; Arellano Ferro, A.; Jiang, X. J., 2003, Astronomy and Astrophysics, v.408, pp.1047-1055 (2003) [RP].

  6. Table 1. Common pms and post-ms points on the track of 1.8M star.

  7. Table 2. Physical data used in the models of V351 Ori and V1366 Ori

  8. Table 3. Pulsational spectra for V351 Ori.

  9. Table 4. Pulsational spectra for V1366 Ori.

  10. Figure 1. Evolutive tracks of 1.8 M star in the HRdiagram. [CESAM(C) vs. HENYEY(H)]. Common points pre/postMS labeled by a,b,c. In the figure also is indicated the main instability strip.

  11. Figure 2.a. Evolutive pulsational diagram for a star of 1.8M[R] [l = 0 (square), l = 1 (*), l = 2 (+)]

  12. Figure 2.b. Evolutive pulsational diagram for a star of 1.8M[I] . [l = 0 (square), l = 1 (*), l = 2 (+)]

  13. Figure 3.a. Pulsational diagram for V351 Ori. Brown and light brown: observations (see table 3). Red and green (pms: l = 0,l = 2). Blue and magenta (post-ms: l = 0,l = 2).

  14. Figure 3.b. Zoom of the figure 3.a.

  15. Figura 4a. Pulsational diagram for V1366 Ori (point a.). Green points observations. Red and blue points: theoretical model [pms, point a., l = 0,l = 2] (see table 4)

  16. Figura 4b. Pulsational diagram for V1366 Ori (point d.). Notations as in Figure 4a.

  17. Figura 4c. Pulsational diagram for V1366 Ori (point e.). Notations as in Figure 4a.

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