New radiation belt discovered at Saturn

This image shows the proton radiation belts of Saturn. The radiation in the area between the planet and the D-ring can be seen enlarged in the inset and was first observed in the last mission phase of the Cassini mission. It is created by the incidence of galactic cosmic radiation on the planet’s rings. The protons generated in this way subsequently interact with the atmosphere of Saturn, its thin D-ring and its ringlets. Credit: MPS/JHUAPL

First results from Cassini’s final mission phase show protons of extreme energies between the planet and its dense rings 

Approximately one year ago a spectacular dive into Saturn ended NASA’s Cassini mission - and with it a unique, 13-year research expedition to the Saturnian system. In the mission’s last five months, the probe entered uncharted territory again: 22 times it plunged into the hitherto almost unexplored region between the planet Saturn and its innermost ring, the D-ring. On Friday, 5 October 2018, the journal Science released a total of six articles describing first results from this mission phase. In one of these papers a research team led by the Max Planck Institute for Solar System Research in Germany and the Applied Physics Laboratory of the Johns Hopkins University in the USA for the first time reports on the unique proton radiation belts formed in close proximity to the planet. Due to presence of the dense A-, B-, and C-rings, this area is almost completely decoupled from the main radiation belt and the rest of the magnetosphere, which extend farther outward. 

When the space probe Cassini swung into its first orbit around Saturn and its rings on July 1, 2004, the MIMI particle detector suite (Magnetospheric Imaging Instrument), including LEMMS (Low Energy Magnetospheric Measurement System), which had been developed and built under the leadership of MPS, caught a brief glimpse of the region between the planet and the innermost D ring. The measurements indicated that a population of charged particles may be present, but its exact composition and properties remained obscure. In the following years, MIMI-LEMMS investigated the particles that are trapped by Saturn’s strong magnetic field outside its rings, forming its main radiation belt that consists of high energy protons and electrons. The proton radiation belt extends more than 285,000 kilometers into space and is strongly influenced by Saturn’s numerous moons, which segment it into five sectors. "Only 13 years later, shortly before the end of the mission, we were given the opportunity to follow up on our very first measurements at Saturn and see if an additional radiation belt sector co-exists with the D-ring and the upper atmosphere of the planet", explains Elias Roussos, scientist at the Max Planck Institute for Solar Systems lead author of the current study. 

The 13-year-long test of patience has now paid off. In their current Science article, the scientists paint a comprehensive picture of the protons surrounding Saturn in close proximity. Two articles in the journal Geophysical Research Letters elaborate these findings. 

Similar to the main proton belt of Saturn, the protons that populate the region close to the planet are generated by incident galactic cosmic radiation. When cosmic radiation interacts with material in Saturn’s atmosphere or in its dense rings, it triggers a chain of reactions generating high-energy protons which get subsequently trapped by the planet’s magnetic field. 

Saturn’s magnetic field is more than ten times stronger near the planet than it is in the main radiation belts. That makes trapping so efficient that protons can remain for years in the same magnetic field line. That forces them to interact continuously with the D-ring and the Saturnian atmosphere and gradually lose their full energy. But with the densities of the tenuous D-ring unknown, it was unclear how fast this energy loss develops and whether all in all a radiation belt can be maintained. Theoretical modeling indicated that MIMI ending up measuring nothing but noise, was a viable scenario. 

That fortunately did not happen – at least for protons. LEMMS measurements revealed a stable accumulation of energetic protons that extends from the atmosphere of Saturn and all across the D-ring. The energy that many of these protons have is extreme: more than 10 times higher than what LEMMS was designed to measure. “We had to dig out old mechanical drawings of the instrument and construct new models of it to understand how it would measure in such an extreme environment”, Roussos adds. 

In its final mission phase, the Cassini probe entered the region between Saturn and the D-ring along the orange trajectory. The observed accumulation of protons extends across the D-ring. While the proton intensity is visibly reduced at ringlets D68 and D73, ringlet D72 hardly influences it. Although Cassini itself did not dive into the D-ring system, LEMMS obtained information about its structure as trapped particles move along magnetic field lines (e.g. marked in blue) and reach the spacecraft after they interact with ring material. Credit: MPS/JHUAPL

"Outward of the D ring, Saturn’s A, B and C rings, are significantly denser and dustier, forming an effective 62,000-kilometer barrier for the trapping of charged particles," Roussos continues. That meant that the outer edge of the D-ring was as far as this new proton belt could extend – and LEMMS measurements confirmed that. "This creates a radiation belt that is completely isolated from the rest of the magnetosphere," says MPS scientist Dr. Norbert Krupp, Principal Investigator of the MIMI-LEMMS team and co-author of the study in Science. 

Within the solar system this region is unique. It offers the possibility to examine a radiation belt 

in laboratory-like conditions, as its protons get created by a very stable process, guided and controlled by Saturn’s strong magnetic field. In Saturn’s main radiation belt and in the radiation belts of Earth and Jupiter these conditions are different - and much more complicated. At Earth, for example, a variable influx of high energy particles from the Sun can have a strong influence on the radiation belt structure. 

Equally valuable is the new information that LEMMS adds about the D-ring system, which is too faint to study by imaging alone. This ring contains a total of three narrow ringlets, all brighter than the rest of the ring and named as D68, D72 and D73. While the intensity of protons was reduced by ringlets D68 and D73, ringlet D72 lying between them does not appear to have an effect. "Even though the D72 and D68 ringlets are similarly bright, LEMMS measurements show us that they must actually be very different," says Roussos. 

MIMI measurements also revealed a secondary, lower energy proton radiation belt at an altitude below several thousand kilometers. This belt forms occasionally when fast neutral hydrogen atoms created in Saturn’s magnetosphere get trapped near the planet if they impact its atmosphere and become charged. “The presence of this lower altitude belt shows that some minimal information by Saturn’s variable, distant magnetosphere can be transmitted across the planet’s dense rings,” Krupp adds. 

In the 13 years the MIMI/LEMMS instrument spent at Saturn, it conducted one of the most comprehensive investigations of a planetary radiation belt other than that of the Earth and even helped to discover unknown rings. A summary of these and further discoveries can be found in the book “Saturn in the 21st Century”, which is published by Cambridge University Press this month. Dr. Norbert Krupp from the MPS is among its four editors. 

Source: Max Planck Society,