Hostname: page-component-586b7cd67f-rcrh6 Total loading time: 0 Render date: 2024-11-29T10:38:43.407Z Has data issue: false hasContentIssue false
  • English
  • Français

Physical Parameter Determination for the δ Scuti Star HD 200925

Published online by Cambridge University Press:  12 April 2016

J. H. Peña ,
M. Paparó ,
R. Peniche ,
M. Rodríguez ,
M. A. Hobart  and
C. de la Cruz
J. H. Peña
Affiliation:
Institute de Astronomía, UNAM, Ap. Postal 70-264, Mexico D. F. 04510, México
M. Paparó
Affiliation:
Konkoly Observatory, Box 67, H-1525 Budapest XII, Hungary
R. Peniche
Affiliation:
Institute de Astronomía, UNAM, Ap. Postal 70-264, Mexico D. F. 04510, México
M. Rodríguez
Affiliation:
Institute de Astronomía, UNAM, Ap. Postal 70-264, Mexico D. F. 04510, México Facultad de Ciencias, UNAM, Cd. Investigacion Mexico D. F. 04510, México
M. A. Hobart
Affiliation:
Facultad de Ciencias, Universidad Veracruzana, Xalapa, México Instituto de Astrofísica de Andalucia, Apartado 3004, Granada, España
C. de la Cruz
Affiliation:
Facultad de Ciencias, Universidad Veracruzana, Xalapa, México

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

HD 200925 is an unusual star: the period is stable on a time scale of many years, yet it shows variations which are either large and irregular, or small, suggesting a possible Blazhko effect (Poretti 1984; Joner & Johnson 1985); it has larger values of Teff and log g derived from uvbyβ than those of dwarf Cepheids of similar period; and it has a somewhat higher metal abundance, [Fe/H], than the Hyades. Furthermore, in conflict to what Joner and McNamara (1983) determined – that m1 index shows no variation with temperature – HD 200925 shows a definite variation, unlike that predicted in Crawford (1979). No explanation of this has yet been found. Johnson & Joner (1986) also derived an unusual and unexpected value of [Fe/H]. Finally, with respect to the pulsation periods of this star, Mantegazza & Poretti (1986) determined the existence of two periods: one definite, 0.26730 d and a possible second one of 0.2138 d which yield a ratio of P2/P1 = 0.800, the theoretical ratio expected between the first and the second overtones, found in other pulsating variables. All of these facts make HD 200925 an interesting star, motivating the present study.

Type
Part 6. Variables Close to the Main Sequence
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 467 - 468
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Crawford, D.L. 1979, AJ, 84, 185 CrossRefGoogle Scholar
Johnson, M.D. & Joner, S.B. 1986, PASP, 98, 581 Google Scholar
Joner, S.B. & Johnson, M.D. 1985, PASP, 97, 53 Google Scholar
Joner, S.B. & McNamara, D.H. 1983, PASP, 95, 433 CrossRefGoogle Scholar
Mantegazza, L. & Poretti, E. 1986, A&A, 158, 389 Google Scholar
McNamara, D. H. 1997, PASP, 109, 1221 CrossRefGoogle Scholar
Peña, J. H., Peniche, R., Hobart, A., Rolland, A., López de Coca, P., Paparo, M., Parrao, L., de la Cruz, C., Olivares, J.L., Costa, V., Ibanoglu, C., Ertan, A.Y., Tümer, O., Tunca, Z., & Evren, S. 1998, A&AS, 129, 9 Google Scholar
Poretti, E. 1984, A&AS, 57, 35 Google Scholar
Relyea, L.J. & Kurucz, R.L. 1978, ApJS, 37, 45 Google Scholar