http://www-personal.umich.edu/~atreya/Articles/2006_Venus_Baines.pdf

To the depths of Venus: Exploring the deep atmosphere and surface of our sister world with Venus Express

Near ultraviolet and infrared continuative high resolution images of Venus with amateur equipment can contribute actively to understand the dynamics of atmosphere and surface In this paper images taken with a commercial 023 m Schmidt-Cassegrain telescope and CCD devices during 2007-2009 and 2010 elongations are discussed Near ultraviolet and infrared sub-arcsecond resolution images of the clouds layers on the dayside have been analyzed, measuring the wind flow and showing change over time The thermal emission of the nightside has been investigated at 965 nm and a topographic map of Phoebe and Beta regio built, with spatial resolution of 26" and temperature resolution of 5 K, then compared with Magellan radar altimetric data Contrast and brightness variation caused by low clouds differential adsorbtion over the days have been observed

http://meetingorganizer.copernicus.org/EPSC2010/EPSC2010-167-1.pdf

The study of Venus with amateur telescopes

Atomic oxygen distributions in the Venus thermosphere: Comparisons between Venus Express observations and global model simulations

http://www-personal.umich.edu/~atreya/Articles/2006_VEX=PFS_Formisano.pdf

The planetary fourier spectrometer (PFS) onboard the European Venus Express mission

We present images of the nightside of Venus taken in the near-infrared windows at 1.0, 1.1, 1.18, 1.28, 1.31, and 2.3 microns with the new infrared camera/spectrometer IRIS on the Anglo-Australian Telescope. These data were taken in spectral-mapping mode. This technique involves scanning the telescope perpendicular to the slit, while collecting spectra at successive slit positions across the planet. We produce data cubes with one spectral and two spatial dimensions. Images can be extracted over any wavelength regions. Each image has square pixels of 0.8 inch resolution. We reduced the scattered light from the sunlit crescent in images extracted from each window by subtracting images taken on either side of the window, where the Venus atmosphere is opaque. Unlike the short wavelength windows, which reveal thermal contrasts that originate primarily from the surface and deep atmosphere, the emission in the 2.3 microns window is produced at much higher altitudes (30-40 km). Emission contrasts seen near 2.3 microns are associated with horizontal variations in the cloud optical depths, and have rotation periods of about six days. We detect large contrasts in infrared emission (20-40 percent) across the disc of Venus in the 1.0-, 1.1-, 1.18-, 1.28-, and 1.31-micron images. Contrasts at these wavelengths may be due to a combination of variations in the optical depths of the overlying sulfuric acid clouds and differences in surface emission. Comparison with the 2.3-micron images show that the patterns seen in the 1.28- and 1.31-micron windows are consistent with cloud optical depth variations alone and require no contribution from the surface. However, images at 1.0, 1.1, and 1.8 microns from July 1991 show a dark feature having a contrast that increases with decreasing wavelength. This behavior is contrary to that expected of cloud absorption. Images taken on three successive days in October show another dark feature that is stationary with respect to the surface. These regions of lower emission correspond closely to the high-altitude surface regions of Beta Regio and Aphrodite Terra. The images can potentially reveal the near-infrared emissiveity of the surface of Venus, thereby complementing Magellan radar reflectivity and ground based radio emissivity measurements. The contrast ratio between highlands and plains is much smaller than would be expected for blackbody radiation from the surface along. Unlike at radio wavelengths, where the atmosphere is essentially transparent, at near-infrared wavelengths the atmosphere emits, absorbs, and scatters radiation, and can modify the observed topographically induced contrasts. The additional radiation from the atmosphere reduces the contrast, and further modification would be expected if terrain at different altitudes has different emissivities. A fit to our data therefore requires, and may constrain, a model of the lowest scale height of the atmosphere.

/pdf/groundbased-near-ir-observations-of-the-surface-of-venus-2f5fvy6quk.pdf

Groundbased Near-IR Observations of the Surface of Venus

Groundbased imaging and spectroscopic observations of Venus reveal intense near-infrared oxygen airglow emission from the upper atmosphere and provide new constraints on the oxygen photochemistry and dynamics near the mesopause (approximately 100 km). Atomic oxygen is produced by the Photolysis of CO2 on the dayside of Venus. These atoms are transported by the general circulation, and eventually recombine to form molecular oxygen. Because this recombination reaction is exothermic, many of these molecules are created in an excited state known as O2(delta-1). The airglow is produced as these molecules emit a photon and return to their ground state. New imaging and spectroscopic observations acquired during the summer and fall of 1991 show unexpected spatial and temporal variations in the O2(delta-1) airglow. The implications of these observations for the composition and general circulation of the upper venusian atmosphere are not yet understood but they provide important new constraints on comprehensive dynamical and chemical models of the upper mesosphere and lower thermosphere of Venus.

/pdf/near-infrared-oxygen-airglow-from-the-venus-nightside-4woc0w7e8r.pdf

Near-infrared oxygen airglow from the Venus nightside

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Groundbased Near-IR Observations of the Surface of Venus

Near-infrared oxygen airglow from the Venus nightside