NASA’s James Webb Space Telescope Primed to Lift the Haze Surrounding Sub-Neptunes
Detailed atmospheric studies will provide key insights into some of the most common – and mysterious – planets known in the galaxy.
The Milky Way is chock-full of enigmatic planets larger than Earth but somewhat smaller than Neptune, racing around their stars faster and closer than Mercury orbits the Sun. Light-years away, obscured by haze or clouds, and with nothing comparable in our own solar system, the exact nature of these nearly ubiquitous sub-Neptune-sized planets remains a mystery. What are they made of? How did they form? And what can they tell us about planets and planetary evolution in general?
With its unparalleled ability to measure extremely subtle differences in the brightness and color of dim infrared light, NASA’s James Webb Space Telescope is primed to lift the haze surrounding the nature and origin of the most common type of planet observed in the Milky Way.
More than half of the Sun-like star systems surveyed in the Milky Way harbor a mysterious type of planet unlike any in our own solar system.
Larger than Earth, smaller than Neptune, and orbiting closer to their stars than Mercury orbits the Sun, these warm-to-hot sub-Neptunes are the most common type of planet observed in the galaxy. But although researchers have been able to measure basic properties – including size, mass, and orbit – of hundreds of these planets, their fundamental nature remains unclear.
Are they dense, Earth-like balls of rock and iron, blanketed in thick layers of hydrogen and helium gas? Or less dense mixtures of rock and ice, surrounded by steamy, water-rich atmospheres? With limited data and no planets of similar size and orbit in our own solar system to use for comparison, it has been difficult to answer these questions.
“What are these planets? How do they form? Why doesn’t our solar system have them? These are fundamental questions,” explains Jacob Bean, an astronomer at the University of Chicago who has led numerous observations of exoplanets.
The Haze Problem
The key to figuring out what sub-Neptunes are made of and how they formed is examining their atmospheres. But getting a clear view has not been easy.
The most effective method of analyzing exoplanet atmospheres is a technique known as transmission spectroscopy. When the planet is transiting its star, some wavelengths (colors) of starlight are filtered out by gases in the planet’s atmosphere. Because each type of gas has a unique “signature,” or set of wavelengths that it absorbs, it’s possible to figure out what an atmosphere is made of based on patterns in the transmission spectrum.
This technique has been successful for many exoplanets, but not for most sub-Neptunes. “There have been very few atmospheric observations of sub-Neptune planets,” explains Eliza Kempton of the University of Maryland–College Park, who specializes in theoretical modeling of exoplanet atmospheres. “And most of those have been dissatisfying in that the spectra have not revealed much in the way of spectral features that would allow us to identify the gases in the atmosphere.”
The issue seems to be aerosols, tiny particles, and droplets that make up clouds or haze. These particles scatter starlight, eroding the prominent spectral peaks into subtle undulations and rendering the spectrum virtually useless in terms of determining gas composition.
But with Webb, researchers are confident that a much clearer view of sub-Neptunes is on the horizon. Two observation programs co-led by Bean and Kempton and scheduled for the first year of Webb operations will use Webb’s uniquely powerful capabilities to probe two sub-Neptune-sized planets: GJ 1214 b, the archetype sub-Neptune; and TOI-421 b, a more recent discovery.
The Sub-Neptune Archetype: GJ 1214 b
GJ 1214 b, a warm sub-Neptune orbiting a nearby red dwarf star, has been the subject of dozens of investigations. Its short orbital period, large size relative to its star, and comparative proximity to Earth make it easy (as exoplanets go) to observe effectively, while its status as the benchmark sub-Neptune – and, according to Bean, “the most mysterious exoplanet that we know of” – make it a worthy target of investigation.
The team will use Webb’s Mid-Infrared Instrument (MIRI) to stare at the GJ 1214 system nearly continuously for nearly 50 hours as the planet completes a little more than one full orbit. They will then analyze the data in three different ways to narrow down the possible combinations of gases and aerosols that make up GJ 1214 b’s atmosphere.
Transmission Spectroscopy: If molecules like water, methane, or ammonia are abundant, they should be obvious in the transmission spectrum. Mid-infrared light should not be scattered by aerosols in the same way as visible and near-infrared light.
Thermal Emission Spectroscopy: Mid-infrared light emitted by the planet itself will provide information about the planet’s temperature and reflectivity, both of which are affected by the atmosphere. A planet surrounded by dark, sooty, light-absorbing haze, for example, will be warmer than one covered in bright, reflective clouds.
Phase Curve Temperature Mapping: Although Webb will not be able to observe GJ 1214 b directly (the planet is too close to its star), it is sensitive enough to measure very subtle changes in the total amount of light from the system as the planet orbits the star. Researchers will use GJ 1214 b’s phase curve, a graph of brightness versus phase (i.e., how much of the planet’s day side is facing the telescope) to map the average temperature of the planet with longitude. This will provide additional information about the circulation and make-up of the atmosphere.
Hot Sub-Neptune TOI-421 b
It’s not clear what the aerosols surrounding warm sub-Neptunes like GJ 1214 b are made of, but they could be similar to those that make up smog-like haze found on Saturn’s moon Titan. To test this hypothesis, the researchers decided to target TOI-421 b, a planet that is similar in size and density to GJ 1214 b, but is thought to be too hot for sooty haze to exist.
Webb will observe TOI-421 b twice as it transits its star, once using the Near-Infrared Imager and Slitless Spectrograph (NIRISS) and again with the Near-Infrared Spectrograph (NIRSpec), to produce a complete near-infrared transmission spectrum of the planet. If the hypothesis is correct and TOI-421 b’s skies are clear, the spectrum can be used to measure the abundance of molecules like water, methane, and carbon dioxide. If it turns out that TOI-421 b has an aerosol problem after all, the team will use the data to better understand what those aerosols are made of.
Kempton and Bean are confident that by probing elusive sub-Neptune atmospheres in a number of different ways with Webb, scientists will finally begin to understand not just these two specific objects, but an entire class of planets.
Both the MIRI observations of GJ 1214 b and the NIRISS and NIRSpec observations of TOI-421 b will be conducted as part of Webb’s Cycle 1 General Observers program. General Observers programs were competitively selected using a dual-anonymous review system, the same system used to allocate time on Hubble.
The James Webb Space Telescope will be the world’s premier space science observatory when it launches in 2021. Webb will solve mysteries in our solar system, look beyond to distant worlds around other stars, and probe the mysterious structures and origins of our universe and our place in it. Webb is an international program led by NASA with its partners, ESA (European Space Agency), and the Canadian Space Agency.
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