Hostname: page-component-848d4c4894-m9kch Total loading time: 0 Render date: 2024-06-02T19:09:10.501Z Has data issue: false hasContentIssue false
  • English
  • Français

A Model for Estimating the Number of Stars for which Terrestrial Planets can be Detected Using Transits

Published online by Cambridge University Press:  19 September 2017

David Koch
David Koch*
Affiliation:
NASA Ames Research Center, MS245-6, Moffett Field, CA 94035, USA

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.

Borucki & Summers (1984) have suggested that extrasolar terrestrial planets can be detected by looking for transits. A discussion is presented of a model used to estimate the number and distance of stars for which planets can be detected as a function of spectral type and luminosity class, apparent brightness, planetary size and orbit, and realistic noise sources that must be considered. A choice for an optimum location of the field to search is described given the realistic constraints of a space mission and maximizing the number of available stars.

Type
Extrasolar Planets
Information
Symposium - International Astronomical Union , Volume 213: Bioastronomy 2002: Life Among the stars , 2004 , pp. 85 - 88
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Allen, C. W. 1976, Astrophysical Quantities 3rd ed., (Athlone Press), 247 Google Scholar
Borucki, W. J., & Summers, A. L. 1984, Icarus 58, 121 Google Scholar
Borucki, W. J., et al. 2002, SPIE Conf 4854 Google Scholar
Koch, D., & Borucki, W. 1996, in Circumstellar Habitable Zones, ed. Doyle, L., (Menlo Park: Travis House Pub), 229 Google Scholar