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Volumn 318, Issue 5848, 2007, Pages 226-229

Polar lightning and decadal-scale cloud variability on Jupiter

(19)  Baines, Kevin H a   Simon Miller, Amy A b   Orton, Glenn S a   Weaver, Harold A c   Lunsford, Allen b   Momary, Thomas W a   Spencer, John d   Cheng, Andrew F c   Reuter, Dennis C b   Jennings, Donald E b   Gladstone, G R e   Moore, Jeffrey f   Alan Stern, S g   Young, Leslie A d   Throop, Henry d   Yanamandra Fisher, Padma a   Fisher, Brendan M a   Hora, Joseph h   Ressler, Michael E a  


Author keywords

[No Author keywords available]

Indexed keywords

CLOUD; CONVECTION; DECADAL VARIATION; INFRARED IMAGERY; JUPITER; LIGHTNING; OPTICAL PROPERTY;

EID: 35348839598     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1147912     Document Type: Article
Times cited : (57)

References (34)
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    • Lightning strikes could be distinguished from cosmic ray hits and auroral features by their distinctive shapes. Because of slight spacecraft nodding motions, constant-brightness point sources such as stars produce curlicue features in our 5-s exposures, unlike our short-lived lightning strikes. Lightning flashes produce a bright central flash surrounded by a halo of light due to diffuse scattering by the overlying atmosphere. Lightning energies were calculated using the spectral irradiance of jovian lightning determined by Borucki et al, 31, The latitudes and longitudes of lightning flashes are determined by a limb/terminator fitting program that generates the planetary ellipse based on the range, camera focal length, and pixel scale. With sufficient contrast between the sky and the planet, the ellipse center is located with an iterative least-squares fit, typically with a precision of 0.1 pixel or better. For low-contrast images, the ellipse is placed manually with an uncerta
    • Lightning strikes could be distinguished from cosmic ray hits and auroral features by their distinctive shapes. Because of slight spacecraft nodding motions, constant-brightness point sources such as stars produce curlicue features in our 5-s exposures, unlike our short-lived lightning strikes. Lightning flashes produce a bright central flash surrounded by a halo of light due to diffuse scattering by the overlying atmosphere. Lightning energies were calculated using the spectral irradiance of jovian lightning determined by Borucki et al. (31). The latitudes and longitudes of lightning flashes are determined by a limb/terminator fitting program that generates the planetary ellipse based on the range, camera focal length, and pixel scale. With sufficient contrast between the sky and the planet, the ellipse center is located with an iterative least-squares fit, typically with a precision of 0.1 pixel or better. For low-contrast images, the ellipse is placed manually with an uncertainty of a few pixels.
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    • Galileo NIMS global maps were acquired on 5 September 1996 from a distance of 1.98 × 106 km, a phase angle of 64.3°, a subsolar latitude near 2°S, and a subspacecraft latitude near 0°. A Cassini Imaging Science Subsystem global image was acquired on 29 December 2000 from a distance of approximately 1.0 × 10+ km, a phase angle near 90°, a subsolar latitude near 2.9°N, and a subspacecraft latitude near 3.5°N. A New Horizons LEISA global map was acquired on 28 February 2007 in three north/south scans over a 47-min period beginning at 01:40 universal time (UT) on 28 February from an altitude of 2.32 × 106 km, a phase angle of 76°, a subsolar latitude near 2.9°S, and a subspacecraft latitude of 8.4°S. The three-color image (middle right of Fig. 2, is composed of a 1.59-μm continuum wavelength image (red, a 1.90-μm wavelength image of moderate atmospheric gas absorption green, and a 1.85-μm wa
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    • We thank the New Horizons mission and science teams. New Horizons is funded by NASA. G.S.O, P.Y.F, and B.M.F. were visiting astronomers at the IRTF, which is operated by the University of Hawaii under Cooperative Agreement no. NCC-538 with NASA, Science Mission Directorate, Planetary Astronomy Program. Thanks to E. Tollestrup and M. Connelley for IRTF instrument orientation and J. Kemerer, and J. Yang for assistance in reducing the observations. Much of the work described in this paper was carried out at the Jet Propulsion Laboratory, Pasadena, CA, under contract with NASA
    • We thank the New Horizons mission and science teams. New Horizons is funded by NASA. G.S.O., P.Y.F., and B.M.F. were visiting astronomers at the IRTF, which is operated by the University of Hawaii under Cooperative Agreement no. NCC-538 with NASA, Science Mission Directorate, Planetary Astronomy Program. Thanks to E. Tollestrup and M. Connelley for IRTF instrument orientation and J. Kemerer, and J. Yang for assistance in reducing the observations. Much of the work described in this paper was carried out at the Jet Propulsion Laboratory, Pasadena, CA, under contract with NASA.


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