A type of Martian aurora firstÂ identified by NASAâs MAVEN spacecraft in 2016Â is actually the most common form of aurora occurring on the Red Planet, according to new results from the mission. The aurora is known as a proton aurora and can help scientists track water loss from Marsâ atmosphere.
On Earth, aurora are commonly seen as colorful displays of light in the night sky near the polar regions, where they are also known as the northern and southern lights. However, the proton aurora on Mars happens during the day and gives off ultraviolet light, so it is invisible to the human eye but detectable to the Imaging UltraViolet Spectrograph (IUVS) instrument on the MAVEN (Mars Atmosphere and Volatile EvolutioN) spacecraft.
MAVENâs missionÂ is to investigate how the Red Planet lost much of its atmosphere and water, transforming its climate from one that might have supported life to one that is cold, dry, and inhospitable.
Since the proton aurora is generated indirectly by hydrogen derived from Martian water thatâs in the process of being lost to space, this aurora could be used to help track ongoing Martian water loss.Â AndrÃ©a Hughes of Embry-Riddle Aeronautical University in Daytona Beach, Florida, and lead author of the paper published in the Journal of Geophysical Research, Space Physics,Â said:
âIn this new study using MAVEN/IUVS data from multiple Mars years, the team has found that periods of increased atmospheric escape correspond with increases in proton aurora occurrence and intensity.
âPerhaps one day, when interplanetary travel becomes commonplace, travelers arriving at Mars during southern summer will have front-row seats to observe Martian proton aurora majestically dancing across the dayside of the planet (while wearing ultraviolet-sensitive goggles, of course).
“These travelers will witness firsthand the final stages of Mars losing the remainder of its water to space.â
Different phenomena produce different kinds of aurora. However, all aurora on Earth and Mars are powered by solar activity, whether it be explosions of high-speed particles known as solar storms, eruptions of gas and magnetic fields known as coronal mass ejections, or gusts in the solar wind, a stream of electrically conducting gas that blows continuously into space at around a million miles per hour.
For example, the northern and southern lights on Earth happen when violent solar activity disturbs Earthâs magnetosphere, causing high velocity electrons to slam into gas particles in Earthâs nightside upper atmosphere and make them glow. Similar processes generate Marsâ discrete and diffuse aurora â two types of aurora that were previously observed on the Martian nightside.
Proton aurora form when solar wind protons (which are hydrogen atoms stripped of their lone electrons by intense heat) interact with the upper atmosphere on the dayside of Mars.
As they approach Mars, the protons coming in with the solar wind transform into neutral atoms by stealing electrons from hydrogen atoms in theÂ outer edge of the Martian hydrogen corona, a huge cloud of hydrogen surrounding the planet. When those high-speed incoming atoms hit the atmosphere, some of their energy is emitted as ultraviolet light.
When the MAVEN team first observed the proton aurora, they thought it was a relatively unusual occurrence.Â Mike Chaffin, research scientist at the University of Colorado Boulderâs Laboratory for Atmospheric and Space Physics (LASP) and second author of the study, said:
âAt first, we believed that these events were rather rare because we werenât looking at the right times and places.
âBut after a closer look, we found that proton aurora are occurring far more often in day side southern summer observations than we initially expected.â
The team has found proton aurora in about 14 percent of their day side observations, which increases to more than 80 percent of the time when only day side southern summer observations are considered.Â Nick Schneider, coauthor and lead of the IUVS team at LASP, said:
âBy comparison, IUVS has detected diffuse aurora on Mars in a few percent of orbits with favorable geometry, and discrete aurora detections are rarer still in the dataset.â
The correlation with the southern summer gave a clue as to why proton aurora are so common and how they could be used to track water loss. During the southern summer on Mars, the planet is also near its closest distance to the Sun in its orbit and huge dust storms can occur. Summer warming and dust activity appear to cause proton auroras by forcing water vapor high into the atmosphere.
Solar extreme ultraviolet light breaks the water into its componentsÂ â hydrogen and oxygen. The light hydrogen is weakly bound by Marsâ gravity and enhances the hydrogen corona surrounding Mars, increasing hydrogen loss to space. More hydrogen in the corona makes interactions with solar-wind protons more common, making proton aurora more frequent and brighter. Hughes concluded:
âAll the conditions necessary to create Martian proton aurora (e.g.,Â solar wind protons, an extended hydrogen atmosphere, and the absence of a global dipole magnetic field) are more commonly available at Mars than those needed to create other types of aurora.
âAlso, the connection between MAVENâs observations of increased atmospheric escape and increases in proton aurora frequency and intensity means that proton aurora can actually be used as a proxy for whatâs happening in the hydrogen corona surrounding Mars, and therefore, a proxy for times of increased atmospheric escape and water loss.â
Provided by: Bill Steigerwald / Nancy Jones,Â NASAÂ [Note: Materials may be edited for content and length.]