A false-color image of Venus’s atmosphere
New research offers a new look at Venus’s atmosphere by measuring the bend and scatter of radio waves as they pass through the planet’s atmosphere. This false-color image taken by Japan’s Venus probe Akatsuki shows atmospheric fine structures. Credit: JAXA
Source: Journal of Geophysical Research: Planets

Venus is Earth’s closest planetary neighbor and the nearest in size to our “Blue Marble,” yet many questions remain about its atmosphere, in part because of challenges in generating fine-scale analyses. Research on the atmosphere of Venus typically results in a vertical resolution between 0.4 and 0.7 kilometers, which is too coarse to observe small-scale atmospheric features. Phenomena like the Venusian “cold collar,” a distinct temperature minimum about 60 kilometers above the surface at high latitudes, remain poorly understood because remote sensing algorithms cannot clearly delineate them.

Remotely sensed data captured by the European Space Agency’s Venus Express Radio Science Experiment (VeRa) and the Japan Aerospace Exploration Agency’s Akatsuki Radio Science mission underlie many analyses of the Venusian atmosphere. These data are collected through radio occultation, which detects bends in radio waves caused by Venus’s atmosphere when the planet passes between the spacecraft and Earth. The data are commonly evaluated using the geometrical optics (GO) method; however, GO often blurs radio rays and cannot decipher rays spreading along multiple pathways. The inability to capture ray propagation plays a significant role in limiting the vertical resolution in research outputs.

In a new study, Imamura et al. addressed the resolution problem by applying an analytical twist to the standard data. The researchers evaluated the radio occultation data using a radio holographic method known as full spectrum inversion (FSI); this is the first time the technique has been applied to Venusian atmospheric data. Among the differences in the two approaches, FSI calculates the arrival time of the radio signal to Earth as a function of the wave frequency; in comparison, GO obtains the radio wave frequency as a function of time.

By using FSI, the researchers obtained an unprecedented vertical resolution (less than 100 meters) in the remotely sensed data. The finer resolution revealed small temperature structures in the atmosphere that the authors suggest are manifestations of atmospheric gravity waves and thin turbulent layers. Atmospheric gravity waves and turbulent layers generated by those waves play crucial roles in Earth’s middle atmosphere but have not previously been well studied on Venus, partly because of the coarse-scale analysis.

The findings also clearly delineate the cold collar temperature minimum hovering around the tops of clouds in the atmosphere. The authors suggest that the sharp gradient was created by adiabatic cooling. Such inference was not possible using the GO method.

The study’s conclusions yield a more precise view of Venus’s atmospheric temperature profile than has previously been published, and both results offer new insights into the atmospheric dynamics on Venus. The radio holographic analysis also provides many possibilities for observing narrow vertical structures in the atmospheres of other far-flung planets. (Journal of Geophysical Research: Planets, https://doi.org/10.1029/2018JE005627, 2018)

—Aaron Sidder, Freelance Writer


Sidder, A. (2019), New analysis provides a fresh view of the atmosphere on Venus, Eos, 100, https://doi.org/10.1029/2019EO113675. Published on 17 January 2019.

Text © 2019. The authors. CC BY-NC-ND 3.0
Except where otherwise noted, images are subject to copyright. Any reuse without express permission from the copyright owner is prohibited.