during and after probe entry
[1] We present adaptive optics data from the Keck telescope, taken while the Huygens probe descended through Titan’s atmosphere and on the days following touchdown. No probe entry signal was detected. Our observations span a solar phase angle range from 0.05 ° up to 0.8°, with the Sun in the west. C...
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ftciteseerx:oai:CiteSeerX.psu:10.1.1.71.6778 2023-05-15T18:22:06+02:00 during and after probe entry Imke De Pater Máte Ádámkovics Antonin H. Bouchez Michael E. Brown Seran G. Gibbard Franck Marchis Henry G. Roe Emily L. Schaller Eliot Young The Pennsylvania State University CiteSeerX Archives application/pdf http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.71.6778 http://www.gps.caltech.edu/~mbrown/papers/ps/imke.pdf en eng http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.71.6778 http://www.gps.caltech.edu/~mbrown/papers/ps/imke.pdf Metadata may be used without restrictions as long as the oai identifier remains attached to it. http://www.gps.caltech.edu/~mbrown/papers/ps/imke.pdf text ftciteseerx 2016-01-08T18:54:53Z [1] We present adaptive optics data from the Keck telescope, taken while the Huygens probe descended through Titan’s atmosphere and on the days following touchdown. No probe entry signal was detected. Our observations span a solar phase angle range from 0.05 ° up to 0.8°, with the Sun in the west. Contrary to expectations, the east side of Titan’s stratosphere was usually brightest. Compiling images obtained with Keck and Gemini over the past few years reveals that the east-west asymmetry can be explained by a combination of the solar phase angle effect and an enhancement in the haze density on Titan’s morning hemisphere. While stratospheric haze was prominent over the northern hemisphere, tropospheric haze dominated the south, from the south pole up to latitudes of 45°S. At 2.1 mm this haze forms a polar cap, while at 1.22 mm it appears in the form of a collar at 60°S. A few small clouds were usually present near the south pole, at altitudes of 30–40 km. Our narrowband J,H,K images of Titan’s surface compare extremely well with that obtained by Cassini ISS, down to the small-scale features. The surface contrast between dark and bright areas may be larger at 2 mm than at 1.6 and 1.3 mm, which would imply that the dark areas may be covered by a coarser-grained frost than the bright regions and/or that there is additional 2 mm absorption there. Text South pole Unknown Gemini ENVELOPE(-62.500,-62.500,-66.133,-66.133) South Pole |
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ftciteseerx |
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English |
description |
[1] We present adaptive optics data from the Keck telescope, taken while the Huygens probe descended through Titan’s atmosphere and on the days following touchdown. No probe entry signal was detected. Our observations span a solar phase angle range from 0.05 ° up to 0.8°, with the Sun in the west. Contrary to expectations, the east side of Titan’s stratosphere was usually brightest. Compiling images obtained with Keck and Gemini over the past few years reveals that the east-west asymmetry can be explained by a combination of the solar phase angle effect and an enhancement in the haze density on Titan’s morning hemisphere. While stratospheric haze was prominent over the northern hemisphere, tropospheric haze dominated the south, from the south pole up to latitudes of 45°S. At 2.1 mm this haze forms a polar cap, while at 1.22 mm it appears in the form of a collar at 60°S. A few small clouds were usually present near the south pole, at altitudes of 30–40 km. Our narrowband J,H,K images of Titan’s surface compare extremely well with that obtained by Cassini ISS, down to the small-scale features. The surface contrast between dark and bright areas may be larger at 2 mm than at 1.6 and 1.3 mm, which would imply that the dark areas may be covered by a coarser-grained frost than the bright regions and/or that there is additional 2 mm absorption there. |
author2 |
The Pennsylvania State University CiteSeerX Archives |
format |
Text |
author |
Imke De Pater Máte Ádámkovics Antonin H. Bouchez Michael E. Brown Seran G. Gibbard Franck Marchis Henry G. Roe Emily L. Schaller Eliot Young |
spellingShingle |
Imke De Pater Máte Ádámkovics Antonin H. Bouchez Michael E. Brown Seran G. Gibbard Franck Marchis Henry G. Roe Emily L. Schaller Eliot Young during and after probe entry |
author_facet |
Imke De Pater Máte Ádámkovics Antonin H. Bouchez Michael E. Brown Seran G. Gibbard Franck Marchis Henry G. Roe Emily L. Schaller Eliot Young |
author_sort |
Imke De Pater |
title |
during and after probe entry |
title_short |
during and after probe entry |
title_full |
during and after probe entry |
title_fullStr |
during and after probe entry |
title_full_unstemmed |
during and after probe entry |
title_sort |
during and after probe entry |
url |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.71.6778 http://www.gps.caltech.edu/~mbrown/papers/ps/imke.pdf |
long_lat |
ENVELOPE(-62.500,-62.500,-66.133,-66.133) |
geographic |
Gemini South Pole |
geographic_facet |
Gemini South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
http://www.gps.caltech.edu/~mbrown/papers/ps/imke.pdf |
op_relation |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.71.6778 http://www.gps.caltech.edu/~mbrown/papers/ps/imke.pdf |
op_rights |
Metadata may be used without restrictions as long as the oai identifier remains attached to it. |
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1766201450446192640 |