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<\/p>\nTitan, the atmosphere-shrouded moon of Saturn, has captivated scientists\u2019 attention since its formal discovery on 25 March 1655. <\/b>While in-situ observations of the moon ended in September 2017 when the Cassini spacecraft was purposely plunged into Saturn\u2019s atmosphere at the end of its mission, data from the 13 year scientific voyage continues to reveal information not just about Titan\u2019s past but about its future potential to harbor life as well.<\/p>\n
While well known for its atmosphere, Titan\u2019s surface is an equal scientific prize due to its complex geology, weather patterns, surface erosion properties, and subterranean ocean.<\/p>\n<\/p>\n
Missions from Pioneer 11, to the two Voyager probes, to the joint NASA\/ESA Cassini-Huygens mission \u2014 which saw Huygens successfully enter Titan\u2019s atmosphere and land on its surface \u2014 have all studied the moon with intense interest.<\/p>\n
Like any other terrestrial world in the solar system, Titan has various impact craters across its surface, though not as many as would be expected given the moon\u2019s size and age. This lack of visible craters \u2014 as seen on Earth \u2014 has largely been attributed to erosion events caused by raining methane.<\/p>\n
A new examination, using Cassini and Huygens data, of nine Titan impact craters at various locations in the equatorial and mid-latitude regions has provided new information on the evolution of the craters, how they are related to Titan\u2019s weather systems, and a unique look at the subsurface composition of the moon exposed due to the impact.<\/p>\n
\u201cImpact craters are one of the few geologic features that expose material from the interior, providing a rare opportunity to understand the subsurface composition of Titan,\u201d said Anezina Solomonidou, lead author on the study published in the journal Astronomy & Astrophysics<\/i>.<\/p>\n
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The nine impact craters and their respective locations on Titan\u2019s surface. (Credit: Solomonidou et al. (2020) & Le Mou\u00e9lic et al. (2019))<\/p>\n
\u201cWhen we study the astrobiological potential of an ocean-bearing world like Titan, it is vital to look for pathways for organic material, for example mixtures that contain important elements, like carbon. These can be recognizable at the surface and in the atmosphere after being transported from the subsurface ocean, which is the most likely habitable environment, and vice versa.\u201d<\/p>\n
Space Shuttle models (adsbygoogle = window.adsbygoogle || []).push({});<\/p>\n Using data from Cassini\u2019s Visual and Infrared Mapping Spectrometer (VIMS) as well as its RADAR instrument, Solomonidou et al. were able to employ a three-pronged approach.<\/p>\n First, they looked tens of centimeters below the impact crater\u2019s surface using microwave emissivity data from the RADAR instrument to understand if the craters\u2019 sub-surfaces were composed mostly of water-ice or organics.<\/p>\n This was done by measuring the effectiveness of each crater\u2019s ability to emit energy, with lower emissivity indicating water-ice and high emissivity areas indicating organics.<\/p>\n Next, they studied the layer of material that has settled over the impact crater\u2019s surface with VIMS. However, in order for this instrument to study Titan\u2019s surface, the methane absorption properties and haze of the moon\u2019s atmosphere had to be properly understood.<\/p>\n<\/p>\n