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‘Electric wind’ can strip Earth-like planets of oceans and atmospheres


Credit: Credit: NASA/Conceptual Image Lab.

WASHINGTON, DC — Venus has an "electric wind" strong enough to remove the components of water from its upper atmosphere, which may have played a significant role in stripping Earth's twin planet of its oceans, according to new results from the European Space Agency's Venus Express mission by NASA-funded researchers.

"It's amazing, shocking," said Glyn Collinson, a scientist at NASA's Goddard Space Flight Center, Greenbelt, Maryland. "We never dreamt an electric wind could be so powerful that it can suck oxygen right out of an atmosphere into space. This is something that has to be on the checklist when we go looking for habitable planets around other stars." Collinson is lead author of a paper about this research published today in Geophysical Research Letters, a journal of the American Geophysical Union.

Venus is in many ways the most like Earth in terms of its size and gravity, and there's evidence that it once had oceans worth of water in its distant past. However, with surface temperatures around 860 degrees Fahrenheit (460 Centigrade), any oceans would have long since boiled away to steam and Venus is uninhabitable today. Yet Venus' thick atmosphere, about 100 times the pressure of Earth's, has 10,000 to 100,000 times less water than Earth's atmosphere. Something had to remove all that steam, and the current thinking is that much of the early steam dissociated to hydrogen and oxygen: the light hydrogen escaped, while the oxygen oxidized rocks over billions of years. Also the solar wind – a million-mile-per-hour stream of electrically conducting gas blowing from the sun – could have slowly but surely eroded the remainder of an ocean's worth of oxygen and water from Venus' upper atmosphere.

"We found that the electric wind, which people thought was just one small cog in a big machine, is in fact this big monster that's capable of sucking the water from Venus by itself," Collinson said.

Just as every planet has a gravity field, it is believed that every planet with an atmosphere is also surrounded by a weak electric field. While the force of gravity is trying to hold the atmosphere on the planet, the electric force (the same force that sticks your laundry together in a dryer and pushes electricity through wires) can help to push the upper layers of the atmosphere off into space. At Venus, the much faster hydrogen escapes easily, but this electric field is so strong that it can accelerate even the heavier electrically charged component of water – oxygen ions – to speeds fast enough to escape the planet's gravity. When water molecules rise into the upper atmosphere, sunlight breaks the water into hydrogen and oxygen ions, which are then carried away by the electric field.

"If you were unfortunate enough to be an oxygen ion in the upper atmosphere of Venus then you have won a terrible, terrible lottery," Collinson said. "You and all your ion friends will be dragged off kicking and screaming into space by an invisible hand, and nothing can save you."

The team discovered Venus' electric field using the electron spectrometer, a component of the ASPERA-4 instrument, aboard the ESA Venus Express. They were monitoring electrons flowing out of the upper atmosphere when it was noticed that these electrons were not escaping at their expected speeds. The team realized that these electrons had been tugged on by Venus' potent electric field. By measuring the change in speed, the team was able to measure the strength of the field, finding it to be much stronger than anyone had expected, and at least five times more powerful than at Earth.

"We don't really know why it is so much stronger at Venus than Earth," Collinson said, "but, we think it might have something to do with Venus being closer to the sun, and the ultraviolet sunlight being twice as bright. It's a challenging thing to measure and even at Earth to date all we have are upper limits on how strong it might be."

Such information also helps us understand other worlds around the solar system.

"We've been studying the electrons flowing away from Titan and Mars as well as from Venus, and the ions they drag away to space," said Andrew Coates, leader of the electron spectrometer team at University College London in the UK and a co-author of the paper. "The new result here shows that the electric field powering this escape is surprisingly strong at Venus compared to the other objects. This will help us understand how this universal process works."

Another planet where the electric wind may play an important role is Mars. NASA's MAVEN mission is currently orbiting Mars to determine what caused the Red Planet to lose much of its atmosphere and water. "We are actively hunting for Mars' electric wind with MAVEN's full arsenal of scientific instruments," Collinson said. "MAVEN is a robotic detective on this four-billion-year-old mystery of where the atmosphere and oceans went, and the electric wind has long been a prime suspect."

Taking the electric wind into account will also help astronomers improve estimates of the size and location of habitable zones around other stars. These are areas where the temperature could allow liquid water to exist on the surface of alien worlds, making them places where life might be found. Some stars emit more ultraviolet light than the sun, so if this creates stronger electric winds in any planets orbiting them, the habitable zone around such stars may be farther away and narrower than thought. "Even a weak electric wind could still play a role in water and atmospheric loss at any planet," said Alex Glocer of NASA Goddard, a co-author on the paper. "It could act like a conveyor belt, moving ions higher in the ionosphere where other effects from the solar wind could carry them away."


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"The Electric Wind of Venus: A global and persistent "polar wind" like ambipolar electric field sufficient for the direct escape of heavy ionospheric ions"


Glyn A. Collinson: NASA Goddard Space Flight Center, Greenbelt, Maryland, U.S.A.; Mullard Space Science Laboratory, University College London, Surrey, U.K.; and Institute for Astrophysics and Computational Sciences, The Catholic University of America, Washington, District of Columbia, U.S.A.;

Rudy A. Frahm, John D. Winningham: Southwest Research Institute, San Antonio, Texas, U.S.A.;

Alex Glocer, Joseph M. Grebowsky, Shawn D. Domagal-Goldman, George Khazanov, Thomas E. Moore: NASA Goddard Space Flight Center, Greenbelt, Maryland, U.S.A.;

Andrew J. Coates, Lin K. Gilbert: Mullard Space Science Laboratory, University College London, Surrey, U.K.;

Stas Barabash, Yoshifumi Futaana: Swedish Institute of Space Physics, Kiruna, Sweden;

Andrei Fedorov: CNRS, L'Institut de Recherche en Astrophysique et Planétologie, and University Paul Sabatier, Toulouse, France;

Thomas A. Nordheim: Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, U.S.A., and Mullard Space Science Laboratory, University College London, Surrey, U.K.;

David Mitchell: Space Sciences Laboratory, University of California, Berkeley, U.S.A.;

William K. Peterson: Laboratory for Atmospheric and Space Physics, Boulder, Colorado, U.S.A.;

Tielong L. Zhang: Space Research Institute, Austrian Academy of Sciences, Graz, Austria.

Contact Information for the Authors:

Glyn A. Collinson: +1 (301) 286-2511, [email protected]

AGU Contact:

Lauren Lipuma
+1 (202) 777-7396
[email protected]

NASA Contact:

Karen Fox
+1 (301) 286-6284
[email protected]

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