Global structure of thermal tides in the upper cloud layer of Venus revealed by the LIR onboard Akatsuki. (arXiv:1905.08947v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kouyama_T/0/1/0/all/0/1">T. Kouyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taguchi_M/0/1/0/all/0/1">M. Taguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukuhara_T/0/1/0/all/0/1">T. Fukuhara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imamura_T/0/1/0/all/0/1">T. Imamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horinouchi_T/0/1/0/all/0/1">T. Horinouchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sato_T/0/1/0/all/0/1">T. M. Sato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murakami_S/0/1/0/all/0/1">S. Murakami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hashimoto_G/0/1/0/all/0/1">G. L. Hashimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Y. J. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Futaguchi_M/0/1/0/all/0/1">M. Futaguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamada_T/0/1/0/all/0/1">T. Yamada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akiba_M/0/1/0/all/0/1">M. Akiba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Satoh_T/0/1/0/all/0/1">T. Satoh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakamura_M/0/1/0/all/0/1">M. Nakamura</a>
Longwave Infrared Camera (LIR) onboard Akatsuki first revealed the global
structure of the thermal tides in the upper cloud layer of Venus, where the
data coverage was from the equator to the mid-latitudes in both hemispheres and
over the whole local time, based on Akatsuki’s long-term observation. The
vertical structure was also indicated by comparing the results at two different
emission angles. From the long-term data, dynamical wave modes consisting of
tides were identified; the diurnal tide consists mainly of a Rossby-wave mode
and a gravity-wave mode, while the semidiurnal tide predominantly consists of a
gravity-wave mode. The suggested vertical structures are roughly consistent
with the wave modes, but some discrepancy remains if the waves are supposed to
be monochromatic. In turn, this discrepancy indicates that a future study
should constrain the heating profile that excites the tidal waves, which would
greatly advance the understanding of the Venusian atmosphere.
Longwave Infrared Camera (LIR) onboard Akatsuki first revealed the global
structure of the thermal tides in the upper cloud layer of Venus, where the
data coverage was from the equator to the mid-latitudes in both hemispheres and
over the whole local time, based on Akatsuki’s long-term observation. The
vertical structure was also indicated by comparing the results at two different
emission angles. From the long-term data, dynamical wave modes consisting of
tides were identified; the diurnal tide consists mainly of a Rossby-wave mode
and a gravity-wave mode, while the semidiurnal tide predominantly consists of a
gravity-wave mode. The suggested vertical structures are roughly consistent
with the wave modes, but some discrepancy remains if the waves are supposed to
be monochromatic. In turn, this discrepancy indicates that a future study
should constrain the heating profile that excites the tidal waves, which would
greatly advance the understanding of the Venusian atmosphere.
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