Martian methane lasts less than a year
Methane in the atmosphere of Mars lasts less than a year, according to a study by Italian scientists. Sergio Fonti (Università del Salento) and Giuseppe Marzo (NASA Ames) have used observations from NASA’s Mars Global Surveyor spacecraft to track the evolution of the gas over three martian years. They will be presenting their results at the European Planetary Science Congress in Rome on Tuesday 21st September.
“Only small amounts of methane are present in the martian atmosphere, coming from very localised sources. We’ve looked at changes in concentrations of the gas and found that there are seasonal and also annual variations. The source of the methane could be geological activity or it could be biological – we can’t tell at this point. However, it appears that the upper limit for methane lifetime is less than a year in the martian atmosphere,” said Fonti.
Levels of methane are highest in autumn in the northern hemisphere, with localised peaks of 70 parts per billion, although methane can be detected across most of the planet at this time of year. There is a sharp decrease in winter, with only a faint band between 40-50 degrees north. Concentrations start to build again in spring and rise more rapidly in summer, spreading across the planet.
“One of the interesting things that we’ve found is that in summer, although the general distribution pattern is much the same as in autumn, there are actually higher levels of methane in the southern hemisphere. This could be because of the natural circulation occurring in the atmosphere, but has to be confirmed by appropriate computer simulations,” said Fonti.
There are three regions in the northern hemisphere where methane concentrations are systematically higher: Tharsis and Elysium, the two main volcano provinces, and Arabia Terrae, which has high levels of underground water ice. Levels are highest over Tharsis, where geological processes, including magmatism, hydrothermal and geothermal activity could be ongoing.
“It’s evident that the highest concentrations are associated with the warmest seasons and locations where there are favourable geological - and hence biological - conditions such as geothermal activity and strong hydration. The higher energy available in summer could trigger the release of gases from geological processes or outbreaks of biological activity,” said Fonti.
The mechanisms for removing methane from the atmosphere are also not clear. Photochemical processes would not break down the gas quickly enough to match observations. However, wind driven processes can add strong oxidisers to the atmosphere, such as the highly reactive salt perchlorate, which could soak up methane much more rapidly.
Martian years are nearly twice as long as Earth years. The team used observations from the Thermal Emission Spectrometer (TES) on Mars Global Surveyor between July 1999 and October 2004, which corresponds to three martian years. The team studied one of the characteristic spectral features of methane in nearly 3 million TES observations, averaging data together to eliminate noise.
“Our study is the first time that data from an orbiting spectrometer has been used to monitor methane over an extended period. The huge TES dataset has allowed us to follow the methane cycle in the martian atmosphere with unprecedented accuracy and completeness. Our observations will be very useful in constraining the origins and significance of martian methane,” said Fonti.
Methane was first detected in the martian atmosphere by ground based telescopes in 2003 and confirmed a year later by ESA’s Mars Express spacecraft. Last year, observations using ground based telescopes showed the first evidence of a seasonal cycle.
The atmosphere on Mars consists of 95% carbon dioxide, 3% nitrogen, 1.6% argon, and contains traces of oxygen and water, as well as methane.
MARS GLOBAL SURVEYOR
Mars Global Surveyor arrived at Mars in September 1997 and last communicated with Earth in November 2006. Findings from the mission included signs of past, persistent water such as an ancient delta and currently active water features in the gullies of canyon walls.
For more information, see: http://mars.jpl.nasa.gov/mgs/
EUROPEAN PLANETARY SCIENCE CONGRESS (EPSC) 2010
EPSC 2010 is organised by Europlanet, a Research Infrastructure funded under the European Commission’s Framework 7 Programme, in association with the European Geosciences Union, with the support of the Italian National Institute for Astrophysics (INAF) and the INAF Institute of Physics of Interplanetary Space (IFSI) in Rome. EPSC is the major meeting in Europe for planetary scientists. The 2010 programme comprises 48 sessions and workshops covering a wide range of planetary topics.
EPSC 2010 is taking place at the Angelicum Centre – Pontifical University of Saint Thomas Aquinas, Rome, Italy from Sunday 19 September to Friday 24 September 2010.
For further details, see the meeting website:
EUROPLANET RESEARCH INFRASTRUCTURE (RI)
Europlanet Research RI is a major (€6 million) programme co-funded by the European Union under the Seventh Framework Programme of the European Commission.
Europlanet RI brings together the European planetary science community through a range of Networking Activities, aimed at fostering a culture of cooperation in the field of planetary sciences, Transnational Access Activities, providing European researchers with access to a range of laboratory and field site facilities tailored to the needs of planetary research, as well as on-line access to the available planetary science data, information and software tools, through the Integrated and Distributed Information Service. These programmes are underpinned by Joint Research Activities, which are developing and improving the facilities, models, software tools and services offered by Europlanet
Department of Physics
Università del Salento
NASA Ames Research Center
Now at ENEA, UTFISST-RADSITO