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The Changing Face of the Extrasolar Giant Planet HD 209458b

James Y-K. Cho et al 2003 ApJ 587 L117-L120   doi: 10.1086/375016  Help

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James Y-K. Cho1,2, Kristen Menou3,4,5, Bradley M. S. Hansen3,6,7 and Sara Seager2,8
1 Spectral Sciences, Inc., 99 South Bedford Street, No. 7, Burlington, MA 01803
2 Current address: Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW, Washington, DC 20015
3 Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08540
4 Chandra Fellow
5 Current address: Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903
6 Division of Astronomy, University of California at Los Angeles, 8971 Math Sciences, Los Angeles, CA 90095
7 Hubble Fellow
8 School of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540

ABSTRACT. High-resolution atmospheric flow simulations of the tidally locked extrasolar giant planet HD 209458b show large-scale spatio-temporal variability. This is in contrast to the simple, permanent day/night (i.e., hot/cold) picture. The planet's global circulation is characterized by a polar vortex in motion around each pole and a banded structure corresponding to approximately three broad zonal (east-west) jets. For very strong jets, the circulation-induced temperature difference between moving hot and cold regions can reach up to ~1000 K, suggesting that atmospheric variability could be observed in the planet's spectral and photometric signatures.

Subject headings: planetary systems; planets and satellites: general; stars: atmospheres; turbulence

Print publication: Issue 2 (2003 April 20)
Received 2002 September 11, accepted for publication 2003 February 28
Published 2003 March 20

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