ESA - Cassini Mission to Saturn logo.
Sept. 6, 2017
The international Cassini-Huygens mission has explored Saturn and its rings and moons for 13 years, and will conclude by plunging into the planet’s atmosphere next week. This article highlights some of the mission’s exciting discoveries led by European teams.
Cassini Grand finale
Cassini is an international programme: a collaboration between NASA, ESA and Italy’s ASI space agency plus several separate European academic and industrial contributors. Nineteen nations contributed to building the spacecraft, and international science teams across the world have gained a better understanding of Saturn and its environment through the mission’s suite of 12 scientific instruments. Two of the instruments – the Cosmic Dust Analyser and the Magnetometer – are led by European principal investigator teams, but all teams are truly international. In total, 27 nations have participated in the mission.
Thousands of peer-reviewed academic publications have been generated, and about a third are led by a first author from an ESA Member/Cooperating State or ESA establishment – some of which are highlighted in this article. In addition, ESA provides support through its two sensitive, deep space tracking antennas at New Norcia, Western Australia, and Malargüe, Argentina, which played an important role during Cassini’s last months in orbit.
ESA’s Huygens probe
Cassini carried ESA’s Huygens probe to Saturn, where the probe detached and coasted for 20 days before descending to the planet’s largest moon Titan. Huygens touched down on Titan on 14 January 2005, becoming the first probe to land on a world in the outer Solar System.
It was equipped with six instruments, four led by European principal investigators and two US. The probe revealed the surprisingly Earth-like landscape below the moon’s dense and hazy nitrogen-rich atmosphere, its shorelines and river channels apparently carved by liquid methane, rather than water, given the –180ºC surface temperatures.
During its two-and-a-half-hour descent, Huygens profiled the moon’s atmosphere in terms of pressure, temperature and density, it measured super-rotating winds, and made in situ measurements of the chemical composition of haze particles. Huygens transmitted from the surface of Titan for another 72 minutes until Cassini disappeared over the horizon, but the data are still keeping scientists busy today.
Lakes and seas on Titan
Cassini at Titan
Cassini continued to make discoveries at Titan during its 127 targeted close flybys – it also made many more distant flybys – covering all aspects of the moon from its internal structure to its hydrocarbon-rich surface, hazy atmosphere and beyond to its interaction with the solar wind.
Using the radar and Radio Science System, which includes the ASI-built high-gain antenna, Cassini revealed that more than 1.6 million sq km of Titan – almost 2% – are covered in liquid, including several large seas and numerous small lakes.
One study, led by Alice Le Gall at the Laboratoire Atmosphères, Milieux in France, found that one of the largest seas, Ligeia Mare, is filled with pure methane. A team led by Marco Mastrogiuseppe at Università La Sapienza, Rome, Italy, used radio sounding to determine that the depth of the sea was up to 160 m in places – the first detection of the bottom of an extraterrestrial sea. By looking at thermal emission they also determined that the seabed is covered by a layer of organic-rich sludge. While fresh methane rainfall likely contributes to the replenishment of the sea, insoluble heavier molecules such as nitriles and benzene are thought to sink to the floor to create the sludge.
Meanwhile, Thomas Cornet and colleagues at the Université de Nantes, France, detected ephemeral lakes – large, shallow depressions that sometimes fill with liquid, similar to those seen on Earth. Ontario Lacus is the largest lake in the southern hemisphere of Titan and its changing characteristics are thought to be due to subsurface hydrocarbon fluids occasionally welling up and flooding the depression, before then partially drying out again. Sediments around Ontario Lacus also indicated that the liquid level has been higher in the past.
Radar has also been used to analyse the changing dunes of Titan, which cover about 13% of its surface, stretching over 10 million sq km. Titan’s dunes, made of solid hydrocarbons that precipitate out of the atmosphere, are gigantic by Earthly standards: they are on average 1–2 km wide, hundreds of kilometres long and around 100 m high.
Alice Le Gall’s team found that their size and spacing vary across the surface, seemingly controlled by altitude and latitude. The main dune fields were found in lowland areas in equatorial regions, while those at higher elevations are narrower and more widely separated, indicating a thinner covering of sand.
In addition, the northern regions, home to the many lakes, likely has a greater soil moisture content, making sand particles less mobile. In general, the grains are shunted around by low-speed winds shifting over the moon’s surface in different directions throughout the year – which on Titan is equivalent to 30 Earth years – causing them to pile up in certain places over time.
Hints that Titan boasted a subsurface ocean already came from Huygens based on detections of electrical currents in the moon’s upper atmosphere. The unique pattern of radio signals suggested an ocean buried around 55-80 km depth, under an icy crust.
Using Cassini’s radio science system, Luciano Iess’ team at the Università La Sapienza in Rome studied the internal structure of Titan by the way in which the spacecraft was pulled off course by the moon as it flew by. The deviations in the velocity are detectable in the spacecraft’s radio signals received by ground stations, and provide a measurement of the gravity variations along the orbit. This can be translated into the distribution of mass inside the moon, and therefore provide constraints on its internal structure. Using this technique, the team also found tides on Titan that distort the surface by more than 10 m. The observation points to a liquid ocean – most likely water – swirling around below the surface. Models suggest that it may be up to 250 km deep beneath an ice shell some 50 km thick.
The presence of an ocean would also help to explain some aspects of Titan’s atmosphere, namely why it has so much methane, which given its naturally short lifetime must be replenished somehow. Since the reservoirs of methane in Titan’s surface hydrocarbon lakes are not enough to explain the large quantities in the atmosphere, an ocean could act as a deep reservoir. Understanding Titan’s hydrocarbon cycle, and how seasonal atmospheric processes are linked to the production of organic haze has provided a focus for many instrument teams.
Scientists using the Cassini’s plasma spectrometer, CAPS, which is led by principal investigator Hunter Waite at the US Southwest Research Institute and with numerous co-investigators in Europe, have gradually honed in on the building blocks of the organic haze particles in Titan’s atmosphere.
Co-investigator Andrew Coates and his team at University College London’s Mullard Space Science Laboratory in the UK, which provided the instrument’s electron spectrometer, made the surprising observation of large negatively charged molecules in Titan’s upper atmosphere. Atoms and molecules there are ionised by solar ultraviolet radiation and by impacts of energetic particles that originate mainly from Saturn’s magnetosphere, breaking apart the nitrogen and methane. An abundance of positively charged molecules was to be expected, but not negatively charged ones, which are highly reactive and should not last long in Titan’s atmosphere before combining with other materials.
Chemistry in Titan’s atmosphere
The initial discovery indicated that complex processes were involved in producing the haze particles, with the negative ions apparently playing a key role. Indeed, a recent study some 10 years after Cassini’s initial detection found linear carbon chain molecules around 1000 km above the moon’s surface that seed the larger organic molecules lower down.
Although no life has been detected on Titan, its atmosphere is thought to be similar to early Earth's before life developed, and thus can be seen as a planet-scale laboratory to understand the chemical reactions that may have led to life on Earth.
With Cassini’s Composite Infrared Spectrometer instrument, scientists led by Nick Teanby from the University of Bristol, UK, studied the rapid change in seasons on Saturn’s moon Titan, following equinox in August 2009, which saw the formation of a swirling vortex and a build up of exotic gases at unexpectedly high altitudes of about 400 km over the moon's south pole.
Vortex on Titan close up
The formation of the vortex indicates the effect of the changing seasons on the circulation pattern in Titan’s atmosphere, specifically with cooler air sinking down from warmer, high altitudes. The changes occurred over a surprisingly short period of time: around six months, quick for a world with over seven-year long seasons.
Scientists led by Remco de Kok of Leiden Observatory and SRON Netherlands Institute for Space Research used Cassini’s Visual and Infrared Mapping Spectrometer data to determine that this giant polar vortex contains frozen particles of the toxic compound hydrogen cyanide, HCN, showing that the atmosphere must be as cold as –148ºC, consistent with the rapidly cooling atmosphere as the seasons changed.
Beyond Titan’s atmosphere
Using CAPS, and also Cassini's Langmuir Probe, which was provided by the Swedish Institute of Space Physics and is part of the US-led Cassini Radio and Plasma Wave Science (or RPWS) package, scientists could study Titan’s uppermost, ionised, atmospheric layers: its ionosphere. The ionisation of molecules by solar ultraviolet light and impacts of energetic particles from Saturn’s magnetosphere not only lead to the production of the complex organic chemistry, but also create a loss of atmospheric constituents.
From the first flybys, the Langmuir probe could see that conditions in Saturn’s magnetosphere affect the structure and dynamics of Titan's ionosphere. Saturn and its magnetosphere rotate together with a period of nearly 11 hours, as inferred from radio measurements. At the distance of Titan, some 20 Saturn radii, the moon spends about 95% of its time inside the magnetosphere, a situation that causes a plasma flow that sweeps by Titan, eroding the upper layers of its atmosphere. About seven tonnes per day of Titan’s atmosphere were found to be escaping on average dominated by heavy ions – a significant loss over billions of years.
The Cassini magnetometer, led by principal investigator Michele Dougherty at Imperial College London, determined that Titan does not have its own intrinsic magnetic field, and also contributed to studies of Titan’s interaction with the outer fringes of Saturn’s magnetosphere.
Combined analysis of the magnetometer data with those from the Cassini Plasma Spectrometer and the Radio and Plasma Wave Spectrometer showed that when Titan is temporarily outside of Saturn’s magnetosphere, its atmosphere retains a memory of the magnetic field of the plasma that surrounds Saturn. When Titan was directly exposed to the solar wind the magnetometer team found that Titan behaves much like other unmagnetised bodies, such as Venus or Mars, with the solar wind draped around the moon’s atmosphere. Studying this effect helps us to understand processes associated with atmospheric loss over time.
The magnetometer also made important discoveries at Saturn’s icy moons, including a first hint at one of the greatest finds of the entire mission: that Enceladus was hiding a liquid water ocean below the frozen surface of its icy crust.
During the first flyby of Enceladus, the magnetometer saw Saturn’s magnetic field bending around the south pole of Enceladus in a shape that wasn’t symmetrical. This turned out to be the first detection of the plume that sprays from the moon's internal ocean, with other instruments later confirming with spectacular images and with the composition of the grains being ejected in the plume.
The Cosmic Dust Analyser (CDA), led by Ralf Srama of the University of Stuttgart in Germany, directly sampled the particles ejected by Enceladus. Particles in Saturn’s E-ring, which is fed by Enceladus, were found to show a high abundance of salts and minerals that could originate from a reservoir of liquid water.
Luciano Iess’ radio science investigations indeed confirmed the presence of an underground sea, with the ice shell thought to overly liquid water at a depth of around 30–40 km in the southern hemisphere. While the gravity data could not rule out a global ocean, a regional sea extending from the south pole to 50ºS latitude appeared most consistent with the moon’s topography and high local temperatures observed around the fractures (called “tiger stripes”), from which the plumes are seen to originate.
Hydrothermal activity on Enceladus
Furthermore, in situ measurements of the plumes, and detections of tiny silicate-rich particles, showed that there was likely hydrothermal activity occurring on the sea floor. The silicate-rich particles are believed to originate where hot water dissolves minerals from the moon’s rocky interior, which could take place at hydrothermal vents.
More recent analysis of data collected with Cassini's Ion Neutral Mass Spectrometer revealed hydrogen gas in the plume, again pointing to the reaction of rocks with hot water, continuing to build the case for the potential habitability of Enceladus’ underground ocean.
Saturn and its rings and moons
Awe-inspiring images of Saturn’s rings have marveled many viewers at their beauty. For one team led by Carl Murray at the University of London, the F ring and its many perplexing features has been their focus. The narrow and contorted ring is intimately linked to moons Prometheus and Pandora, which weave towards and away from the ring, drawing out structures in the ring material. The team also discovered that some of the small, rogue fragments occasionally crash through the core of the F ring, dragging out ice particles with them to form long streamers.
Spying Saturn’s moonlets
The F ring is not the only ring controlled by a moon. Enceladus feeds Saturn’s wide, diffuse E ring with icy water particles, which stretches from the orbit of the moon Mimas to beyond that of Titan, according to Cosmic Dust Analyser data. Enceladus is also a major source of ionised material filling the huge magnetic bubble around Saturn – the magnetosphere. It ejects about 100 kg of water into space every second. One of the plasma spectrometer’s major discoveries was that most of the ions in the Saturn system come from water ejected by Saturn’s moon Enceladus. When exposed to the magnetosphere and ultraviolet sunlight in space, the ejected particles become ionised, meaning they acquire an electric charge. But where do all the water-ions go? Using the Cassini Plasma Spectrometer and the magnetometer, Chris Arridge and colleagues at Lancaster University, UK, found the first direct evidence for explosive releases of energy in the magnetosphere, such that this process of ‘magnetic reconnection’ allows plasma to escape. During the grand finale orbits, Cassini’s spectrometer will try to determine if some of this plasma is lost to Saturn’s upper atmosphere.
The plasma spectrometer’s electron sensor also revealed that Enceladus is linked to Saturn by powerful electric currents. The motion of Enceladus and its ionosphere through Saturn’s magnetosphere acts like a dynamo, setting up an electrical current, and creating an auroral footprint on Saturn. The same process had already been seen between Jupiter and three of its moons.
Meanwhile, small moons Methone and Anthe, both discovered in Cassini images between the orbits of Mimas and Enceladus, were found to be linked to two peculiar breaks in the near-constant rain of high-energy electrons that bombard Cassini when it is near Saturn. Using Cassini's Low Energy Magnetospheric Measurement System, a part of the Magnetospheric Imaging Instrument, Elias Roussos from the Max Planck Institute for Solar System Research in Germany reported that the gaping holes fell along the orbits of the then-newly discovered moons.
The moons’ dusty surfaces are not only thought to absorb a proportion of the high-energy particles, but their surfaces are also losing dust through micrometeorite impacts, building up significant arcs of material along their orbits, creating near-invisible partial rings.
Roussos and colleagues also discovered a transient radiation belt at Saturn with the same instrument, near the orbit of moons Dione and Tethys. It was observed as sudden increases in the intensity of high-energy charged particles in the inner part of Saturn’s magnetosphere, and likely was caused by a change in the intensities of cosmic rays at Saturn arising from solar storms reaching the planet. The belt was detected for only a few weeks after each of its appearances, suggesting that the charged particles were absorbed by the moons. At the same time, the inner radiation belts were clearly separated by a permanent radiation gap along the orbit of moon Tethys, which apparently shields these belts from solar wind influences. Instead, those radiation belts probably arise from the interaction of the planet’s main rings and atmosphere with galactic cosmic ray particles that, unlike the solar wind, have the very high energies needed to penetrate the innermost Saturnian magnetosphere.
Studying how Saturn’s vast magnetosphere interacts with the solar wind was an important aspect of Cassini’s studies. During a chance encounter with an unusually strong blast of solar wind arriving at Saturn, the Cassini Plasma Spectrometer and Magnetospheric Imaging Instrument detected particles being accelerated to ultra-high energies, and one of the strongest shocks ever encountered at Saturn. The scenario mimicked the kinds of accelerations that occur in supernova remnants, the death cries of dying stars, giving scientists the capability of studying the nature of a supernova shock in situ in our own Solar System and bridging the gap to distant high-energy astrophysical phenomena that are usually only studied remotely.
The Magnetospheric Imaging Instrument was also used to determine the shape of our Solar System’s heliosphere – the magnetic bubble created by the solar wind. It was previously thought to be comet-shaped, with a head pointed into the stream of the interstellar medium and a tail flowing downstream, but the Cassini data suggested it was more spherical, controlled by the interstellar magnetic field that it passes through.
A team led by ESA’s Cassini project scientist Nicolas Altobelli used the Cosmic Dust Analyser (CDA) to sample interstellar dust grains originating from outside of our Solar System. While most of the particles collected by the CDA originated from Enceladus, a handful stood out in their high speed and direction of impact. They could be traced back to the local interstellar cloud: an almost empty bubble of gas and dust our Solar System is travelling through with a distinct direction and speed.
The CDA also measured fast silicate-rich particles escaping Saturn’s environment. A stream of nanometer-sized silicate particles, originating from Saturn and travelling at very high speed (hundreds of km/s) was discovered as Cassini was arriving at Saturn. This particle population and the acceleration mechanism, linked to the rotating magnetic field of the planet, were known to exist at Jupiter – Cassini showed that the same physics are at play at Saturn.
Science until the end
Cassini's science instruments will continue returning unique data until the very end. Since 22 April 2017, Cassini has been making weekly dives between Saturn’s upper atmosphere and its innermost rings, collecting unprecedented data in this previously unexplored region, including the first in situ measurements in this environment.
While crossing the ring plane, the CDA has been directly sampling the composition of dust particles from different parts of the ring system. With its radio science investigation, Cassini can measure Saturn’s gravitational field as close as 3000 km from the upper cloud layers, greatly improving the current models of the planet’s internal structure, its rotation, and winds in its atmosphere.
Internal structure of Saturn
Scientists expect the new data will also allow them to disentangle the gravity of the planet from the tiny pull exerted on the spacecraft by the rings, estimating the total mass of the rings to unprecedented accuracy. ESA ground stations in Argentina and Australia helped to receive Cassini's radio science data, providing a series of 22 tracking passes during the grand finale.
The grand finale orbits are also probing the planet’s magnetic field at close distances. Previous observations have shown that the magnetic field is weaker than expected, with the magnetic axis surprisingly well aligned with the planet’s rotation. New data to be collected by the Cassini magnetometer will provide insights to understand why this is so and where the sources of magnetic field are located, or whether something in Saturn’s atmosphere has been obscuring the true magnetic field from Cassini until now.
Over the last five weeks, Cassini’s orbits have dipped it into the upper atmosphere of the planet. One last distant flyby of Titan on 11 September will set the spacecraft on its final trajectory, adjusting its orbit to send it plunging into the planet’s atmosphere. Eight instruments (CDA, CIRS, INMS, MAG, MIMI, RPWS, RSS and UVIS) will collect data during the final plunge, transmitting it back to Earth in near-real time. Cassini will no doubt surprise scientists with more of Saturn’s hidden secrets right up until the very end of its pioneering mission.
For more about the grand finale, see: https://saturn.jpl.nasa.gov/grandfinale
Huygens touched down on Titan: http://www.esa.int/spaceinimages/Images/2005/01/First_colour_view_of_Titan_s_surface
International science teams: https://saturn-archive.jpl.nasa.gov/mission/team/
ESA Member/Cooperating State: http://www.esa.int/About_Us/Welcome_to_ESA/New_Member_States
US Southwest Research Institute: http://caps.space.swri.edu/caps/teamMembers/teamMembers.shtml
Eight instruments (CDA, CIRS, INMS, MAG, MIMI, RPWS, RSS and UVIS): http://www.esa.int/ESA_Multimedia/Images/2017/09/Science_during_Cassini_s_descent
At Saturn and Titan: http://www.esa.int/Our_Activities/Space_Science/Cassini-Huygens
NASA JPL Cassini site: http://saturn.jpl.nasa.gov/
Italian Space Agency: http://www.asi.it/en
Animation, Images, Text, Credits: NASA/JPL-Caltech/ASI/USGS; left and right: NASA/ESA. Acknowledgement: T. Cornet, ESA/Angelo Tavani/Space Science Institute.
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