GROUND-BASED NEAR-INFRARED IMAGING OBSERVATIONS OF VENUS DURING THE GALILEO ENCOUNTER

被引：68

作者：

CRISP, D

MCMULDROCH, S

STEPHENS, SK

SINTON, WM

RAGENT, B

HODAPP, KW

PROBST, RG

DOYLE, LR

ALLEN, DA

ELIAS, J

机构：

[1] CALTECH,PALOMAR OBSERV,PASADENA,CA 91125

[2] CALTECH,DIV GEOL & PLANETARY SCI,PASADENA,CA 91125

[3] LAS CAMPANAS OBSERV,LA SERENE,CHILE

[4] UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822

[5] SAN JOSE STATE UNIV FDN,SAN JOSE,CA 95192

[6] UNIV HAWAII,MAUNA KEA OBSERV,MAUNA KEA,HI

[7] KITT PEAK NATL OBSERV,TUCSON,AZ 85719

[8] NASA,AMES RES CTR,MOFFETT FIELD,CA 94035

[9] ANGLO AUSTRALIAN OBSERV,EPPING,NSW 2121,AUSTRALIA

[10] CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE

来源：

SCIENCE | 1991年 / 253卷 / 5027期

关键词：

D O I：

10.1126/science.253.5027.1538

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Near-infrared images of Venus, obtained from a global network of ground-based observatories during January and February 1990, document the morphology and motions of the night-side near-infrared markings before, during, and after the Galileo Venus encounter. A dark cloud extended halfway around the planet at low latitudes (< +/- 40-degrees) and persisted throughout the observing program. It had a rotation period of 5.5 +/- 0.15 days. The remainder of this latitude band was characterized by small-scale (400 to 1000 kilometers) dark and bright markings with rotation periods of 7.4 +/- 1 days. The different rotation periods for the large dark cloud and the smaller markings suggests that they are produced at different altitudes. Mid-latitudes (+/- 40-degrees to 60-degrees) were usually occupied by bright east-west bands. The highest observable latitudes (+/- 60-degrees to 70-degrees) were always dark and featureless, indicating greater cloud opacity. Maps of the water vapor distribution show no evidence for large horizontal gradients in the lower atmosphere of Venus.

引用

页码：1538 / 1541

页数：4

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