Hostname: page-component-586b7cd67f-rcrh6 Total loading time: 0 Render date: 2024-12-01T02:49:39.205Z Has data issue: false hasContentIssue false
  • English
  • Français

Empirical surface gravities

Published online by Cambridge University Press:  25 May 2016

P. F. L. Maxted
P. F. L. Maxted*
Affiliation:
University of Southampton, UK

Abstract

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.

The surface gravity of a star (log g) is a fundamental parameter in models of stellar atmospheres. Given suitable spectra, log g can be determined from such models with an accuracy of 0.1dex, at best. Detached eclipsing binary stars can provide values of log g an order of magnitude more accurate than this, though for a more limited range of stars. Naturally, less accurate surface gravities can be obtained for a wider range of eclipsing binary stars.

These facts are well known, so in this short review I will outline the types of stars to which the two methods have be usefully applied and might be applied in the near future. This naturally leads to the question of where the two ranges overlap and the comparison of results from the two methods. Techniques for allowing this comparison to made directly will be described. Surface gravities derived from winds in hot stars and (indirectly) from gravitational redshifts in white dwarf stars will also be covered briefly.

Type
Stellar Masses and Surface Gravities
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 119 - 124
Copyright
Copyright © Kluwer 1997 

References

Bagnuolo, W.G. and Gies, D.R., (1991) Astroph. J. 376 pp. 266–271 Google Scholar
Balona, L.A. (1985) Mon. Not. R. Astron. Soc. 211, pp. 973–980 Google Scholar
Bonnell, J.T. and Bell, R.A., (1993) Mon. Not. R. Astron. Soc. 264, pp. 334–344 Google Scholar
Clayton, G.C., (1996) Pub. Astron. Soc. Pacific 108, pp. 401–403 Google Scholar
Edvardsson, B. (1988) Astron. & Astrophys. 190, pp. 148–166 Google Scholar
Gustafsson, B. (1989) Ann. Rev. Astron. Astrophys. 27, pp. 701–756 Google Scholar
Hadrava, P., (1995) Astron. Astrophys. Suppl. Ser. 114, pp. 393–396 Google Scholar
Herrero, A., Kudritzki, R.P., Vilchez, D. Kunze, K., Butler, K. and Haser, S. (1992) Ann. Rev. Astron. Astrophys. 261, pp. 209–234 Google Scholar
Kudritzki, R.P. and Hummer, D.G., (1990) Ann. Rev. Astron. Astrophys. 28, pp. 303–345 Google Scholar
Marsh, T.R., Dillon, V.S. and Duck, S.R., (1995) Mon. Not. R. Astron. Soc. 275, pp. 89–99 CrossRefGoogle Scholar
Metcalfe, T.S., Mathieu, R.D., Latham, D.W. and Torres, G. (1996) Astroph. J. 456, pp. 356–364 Google Scholar
Moon, T.T. and Dworetsky, M.M., (1985) Mon. Not. R. Astron. Soc. 217, pp. 305–316 Google Scholar
Reid, I.N. (1996) Astron. J 111, pp. 2000–2016 Google Scholar
Relyea, L.J. and Kurucz, R.L., (1978) Astroph. J. Suppl. 37, pp. 45 Google Scholar
Simon, K.P., Sturm, E. and Fiedler, A. (1994) Astron. & Astrophys. 292, pp. 507–518 Google Scholar