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A Fresh Look at Older Data Yields a Surprise Near the Martian Equator
Jet Propulsion Laboratory
September 28, 2017

Scientists taking a new look at older data from NASA's longest-operating
Mars orbiter have discovered evidence of significant hydration near the Martian equator -- a mysterious signature in a region of the Red Planet
where planetary scientists figure ice shouldn't exist.

Jack Wilson, a post-doctoral researcher at the Johns Hopkins University Applied Physics Laboratory in Laurel, Maryland, led a team that reprocessed data collected from 2002 to 2009 by the neutron spectrometer instrument
on NASA's Mars Odyssey spacecraft. In bringing the lower-resolution compositional
data into sharper focus, the scientists spotted unexpectedly high amounts
of hydrogen -- which at high latitudes is a sign of buried water ice --
around sections of the Martian equator.

An accessible supply of water ice near the equator would be of interest
in planning astronaut exploration of Mars. The amount of delivered mass
needed for human exploration could be greatly reduced by using Martian
natural resources for a water supply and as raw material for producing hydrogen fuel.

By applying image-reconstruction techniques often used to reduce blurring
and remove "noise" from medical or spacecraft imaging data, Wilson's team improved the spatial resolution of the data from around 320 miles to 180
miles (520 kilometers to 290 kilometers). "It was as if we'd cut the spacecraft's
orbital altitude in half," Wilson said, "and it gave us a much better
view of what's happening on the surface."

The neutron spectrometer can't directly detect water, but by measuring neutrons, it can help scientists calculate the abundance of hydrogen --
and infer the presence of water or other hydrogen-bearing substances.
Mars Odyssey's first major discovery, in 2002, was abundant hydrogen just beneath the surface at high latitudes. In 2008, NASA's Phoenix Mars Lander confirmed that the hydrogen was in the form of water ice. But at lower latitudes on Mars, water ice is not thought to be thermodynamically stable
at any depth. The traces of excess hydrogen that Odyssey's original data showed at lower latitudes were initially explained as hydrated minerals,
which other spacecraft and instruments have since observed.

Wilson's team concentrated on those equatorial areas, particularly with
a 600-mile (1,000-kilometer) stretch of loose, easily erodible material between the northern lowlands and southern highlands along the Medusae
Fossae Formation. Radar-sounding scans of the area have suggested the
presence of low-density volcanic deposits or water ice below the surface,
"but if the detected hydrogen were buried ice within the top meter of
the surface, there would be more than would fit into pore space in soil," Wilson said. The radar data came from both the Shallow Radar on NASA's
Mars Reconnaissance Orbiter and the Mars Advanced Radar for Subsurface
and Ionospheric Sounding on the European Space Agency's Mars Express orbiter and would be consistent with no subsurface water ice near the equator.

How water ice could be preserved there is a mystery. A leading theory
suggests an ice and dust mixture from the polar areas could be cycled
through the atmosphere when Mars' axial tilt was larger than it is today.
But those conditions last occurred hundreds of thousands to millions of
years ago. Water ice isn't expected to be stable at any depth in that
area today, Wilson said, and any ice deposited there should be long gone. Additional protection might come from a cover of dust and a hardened "duricrust"
that traps the humidity below the surface, but this is unlikely to prevent
ice loss over timescales of the axial tilt cycles.

"Perhaps the signature could be explained in terms of extensive deposits
of hydrated salts, but how these hydrated salts came to be in the formation
is also difficult to explain," Wilson added. "So for now, the signature remains a mystery worthy of further study, and Mars continues to surprise
us."

Wilson led the research while at Durham University in the U.K. His team
- which includes members from NASA Ames Research Center, the Planetary
Science Institute and the Research Institute in Astrophysics and Planetology
- published its findings this summer in the journal Icarus.

News Media Contact
Guy Webster
Jet Propulsion Laboratory, Pasadena, Calif.
818-354-6278
guy.webster@jpl.nasa.gov

Michael Buckley
Johns Hopkins Applied Physics Laboratory, Laurel, Md.
240-228-7536
michael.buckley@jhuapl.edu

Laurie Cantillo / Dwayne Brown
NASA Headquarters, Washington
202-358-1077 / 202-358-1726
laura.l.cantillo@nasa.gov / dwayne.c.brown@nasa.gov

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