The relationship between frontal activity and the micropopulation of the atmosphere at altitude is described. It is shown that certain of the meteorological events associated with frontal activity quantitatively modify the micropopulation of the atmosphere. Precipitation associated with frontal passage reduces the micropopulation at altitude, whereas frontal activity with high levels of associa...

Author(s) Tsuda, Toshitaka; Sato, Natsuo; Fujii, Ryoichi; Ono, Takayuki; Yumoto, Kiyohumi; Iyemori, Toshihiko; Shibata, Kazunari; Hayashi, Hiroo; Hori, Tomoaki; Tanaka, Yoshimasa; Koyama, Yukinobu; Abe, Shuji; Shinbori, Atsuki; Umemura, Norio; Yoneda, Mizuki; Ueno, Satoru; Kaneda, Naoki; IUGONET project team Citation (2012) Issue Date 2012-05-23 URL http://hdl.handle.net/2433/156791 Right Type ...

Past observations and modeling of Jupiter's thermosphere have, due to their limited resolution, suggested that heat generated by the aurora near the poles results in a smooth thermal gradient away from these aurorae, indicating a quiescent and diffuse flow of energy within the subauroral thermosphere. Here we discuss Very Large Telescope-Cryogenic High-Resolution IR Echelle Spectrometer observa...

The large abundance of NH3 in Titan's upper atmosphere is a consequence of coupled ion and neutral chemistry. The density of NH3 is inferred from the measured abundance of NH4+. NH3 is produced primarily through reaction of NH2 with H2CN, a process neglected in previous models. NH2 is produced by several reactions including electron recombination of CH2NH2+. The density of CH2NH2+ is closely li...

In this paper we investigate the validity of the optically thin assumption in the transition region of the late–type star AU Mic. We use Far–Ultraviolet Spectroscopic Explorer (FUSE) observations of the C  multiplet and O  resonance lines, hence yielding information at two different levels within the atmosphere. Significant deviations from the optically thin fluxes are found for C  in b...

We have analyzed three stellar occultation observations of Saturn's upper atmosphere during the years 1989 to 1995. These occultations probed the stratosphere at pressure levels about 0.5 to 20 pbars, intermediate to those probed by the Pioneer 11, Voyager I and II radio and ultraviolet occultations. The time span of the earlier occultations and the observation of a higher latitude occultation ...

Department of Physics, Imperial College, London SW7 2AZ, UK b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, USA c School of Astronomy and Space Sciences, Nanjing University, Nanjing 210008, China National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China e Swedish Institute of Space Physics, Uppsala, Sweden Groupe de Spectrométrie Mol...

Emission features from ionized carbon dioxide and carbon monoxide were measured in the 1900- to 4300-angstrom spectral region. The Lyman alpha 1216-angstrom line of atomic hydrogen and the 1304-, 1356-, and 2972-angstrom lines of atomic oxygen were observed.

Since the first in situ observations of the Martian atmosphere were made by the twin Viking landers, we have learned considerably more about its composition, dynamics and variability. Not only did the new data on global atmospheric densities generate opportunities to understand the atmospheric composition of early Mars and supply constraints at the upper limit of General Circulation Models, it ...

Surfur-bearing molecules have been found at the surface of Mars by the Viking lander, the Spirit and Opportunity rovers, and the OMEGA infrared spectrometer aboard Mars Express. However, no gaseous sulfur-bearing species have ever been detected in the Martian atmosphere. We search for SO2 signatures in the thermal spectrum of Mars at 7.4 μm using the Texas Echelon Cross Echelle Spectrograph (TE...