Hostname: page-component-cc8bf7c57-hbs24 Total loading time: 0 Render date: 2024-12-12T04:38:03.606Z Has data issue: false hasContentIssue false
  • English
  • Français

Results from Microlensing Searches for Extrasolar Planets

Published online by Cambridge University Press:  26 May 2016

Penny D. Sackett
Penny D. Sackett*
Affiliation:
Kapteyn Institute, 9700 AV Groningen, The Netherlands

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.

Specially-designed microlensing searches, some of which have been underway for several years, are sensitive to extrasolar planets orbiting the most common stars in our Galaxy. Microlensing is particularly well-suited to the detection of Jupiter-mass planets orbiting their parent stars at several AU. Since Jovian analogs are thought to influence the subsequent evolution of most planetary systems, they are particularly important to study. The orbital radii and distances to the planetary systems probed by microlensing are larger than those currently studied by radial velocity techniques; the two methods are thus complementary. Recent results from microlensing searches are discussed, including constraints on Jovian analogs orbiting typical Galactic stars. Benefits and drawbacks of the technique for the characterization of planetary systems, and future prospects are briefly reviewed.

Type
Part I: Discovery and study of extrasolar planets - current
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 44 - 51
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Albrow, M.D. et al. 2000a, ApJ, 534, 894.Google Scholar
Albrow, M.D. et al. 2000b, ApJ, 535, 176.Google Scholar
Albrow, M.D. et al. 2000c, ApJ, submitted (astro-ph/0008078).Google Scholar
Alcock, C. et al. 2000, ApJ, 541, 270.Google Scholar
Bennett, D.P., & Rhie, S.H. 1996, ApJ, 472, 660.Google Scholar
Bennett, D.P. et al. 1997, ASP Conf. Prof. 119, 95 (astro-ph/9612208).Google Scholar
Bennett, D.P. et al. 1999, Nature, 402, 57.Google Scholar
Di Stefano, R., & Scalzo, 1999, ApJ, 512, 579.Google Scholar
Dominik, M., 1999, A&A, 349, 108.Google Scholar
Dominik, M., & Sahu, K. 2000, ApJ, 534, 213.CrossRefGoogle Scholar
Gaudi, B.S. 2000, , The Ohio State University.Google Scholar
Gaudi, B.S., Naber, , & Sackett, P. 1998, ApJ, 502L, 33.Google Scholar
Gaudi, B.S., & Sackett, P.D. 2000, ApJ, 528, 56.Google Scholar
Gould, A., & Han, C. 2000, ApJ, 538, 653.Google Scholar
Gould, A., & Loeb, A. 1992, ApJ, 396, 104.Google Scholar
Griest, K., & Safizadeh, N. 1998, ApJ, 500, 37.CrossRefGoogle Scholar
Han, C., 2000, in A New Era of Microlensing Astrophysics, ASP Conf. Series, eds. Menzies, & Sackett, , in press (astro-ph/0003369).Google Scholar
Marcy, G., Cochran, W.D., & Mayor, M. 2000, in Protostars and Planets IV, eds. Mannings, , Boss, & Russell, (U. of Arizona Press: Tucson) p. 1285.Google Scholar
Mayor, M., & Queloz, D. 1995, Nature, 378, 355.Google Scholar
Mao, S., & Paczynśki, B. 1991, ApJ, 374, 37.Google Scholar
Mao, S., Reetz, J., & Lennon, D.J. 1998, A&A, 338, 56.Google Scholar
Peale, S. 1997, Icarus, 127, 269.Google Scholar
Rhie, S.H. et al. 2000, ApJ, 533, 378.Google Scholar
Sackett, P.D. 1997, ESO Document: SPG-VLTI-97/002 (astro-ph/9709269).Google Scholar
Safizadeh, N., Dalai, N., & Griest, K. 1999, ApJ, 522, 512.Google Scholar
Udalski, A., & Szymanski, M. 2000, http://www.astrouw.edu.pi/ftp/ogle/ogle2/ews/ews.html.Google Scholar