Not exact matches
On the exo - Mars, thermal
escape would increase only if the increase in UV radiation were to push
more hydrogen to the top of the atmosphere.
While lower - energy ultraviolet radiation breaks up water molecules — a process called photodissociation — ultraviolet rays with
more energy (XUV radiation) and X-rays heat the upper atmosphere of a planet, which allows the products of photodissociation,
hydrogen and oxygen, to
escape.
«Now that we know such large changes occur, we think of
hydrogen escape from Mars less as a slow and steady leak and
more as an episodic flow — rising and falling with season and perhaps punctuated by strong bursts,» said Michael Chaffin, a scientist at the University of Colorado at Boulder who is on the Imaging Ultraviolet Spectrograph (IUVS) team.
But he says the argument would be
more persuasive if it explained why the crust would have absorbed the excess oxygen produced by
hydrogen escape.
«Now that we know such large changes occur, we think of
hydrogen escape from Mars less as a slow and steady leak and
more as an episodic flow — rising and falling with season and perhaps punctuated by strong bursts,» said Michael Chaffin, a scientist at the University of Colorado Boulder's Laboratory for Atmospheric and Space Physics who is on the Imaging Ultraviolet Spectrograph (IUVS) team.
Since the lighter version
escapes more often, over time, the Martian atmosphere has less and less
hydrogen compared to the amount of deuterium remaining.
Accelerating a CO2 molecule to
escape velocity (15 km / s), even with 100 % efficiency, requires far energy
more than the energy released burning one carbon atom and even the associated
hydrogen atoms.