Coarse clouds of hot sand blow in the powerful winds of these two failed stars.

An illustration of the powerful storms and clouds of silicate found in the atmosphere of the brown dwarfs.(Image credit: NASA/JPL–Caltech/University of Western Ontario/Stony Brook University/Tim Pyle)

The James Webb Space Telescope (JWST) has discovered stormy weather in the sky of two brown dwarfs in the most detailed weather report yet from such "failed stars." 

The two brown dwarfs form a binary pair called WISE 1049AB that was discovered by NASA's Wide-field Infrared Survey Explorer (WISE) in 2013; the duo sits just 6.5 light-years away from us. They are the closest brown dwarfs to our sun, and thus make an excellent target for the James Webb Space Telescope's powerful infrared instruments.

A brown dwarf is an object that isn't quite massive enough to ignite the nuclear fusion of hydrogen to helium in its core and become a fully fledged star — yet is also considered too massive to be a planet and thought to form like stars do (via the gravitational collapse of a cloud of molecular gas). As such, brown dwarfs are thought of as a missing link between gas giant planets like Jupiter, and the lowest mass stars, M-dwarfs.

Previous observations have probed the atmosphere of various brown dwarfs, but they have always been limited to time-averaged snapshots, meaning we could not see things in the brown-dwarf atmosphere changing with time. However, brown dwarfs are fast rotators — WISE 1049A spins on its axis once every 7 hours, and B once every 5 hours — and the conditions in their atmospheres can alter over time, meaning that previous observations that didn't factor in the objects' evolutions could have missed lots of variability.

The JWST, however, does have the ability to detect these changes over time. A team led by Beth Biller of the University of Edinburgh observed WISE 1049AB for 8 hours with the JWST's Mid-Infrared Instrument (MIRI), and then immediately afterward for another 7 hours with its Near-Infrared Spectrometer (NIRSpec).

The researchers found that both brown dwarfs are covered in tumultuous clouds, probably composed of silicate grains, sweltering in temperatures between 875 degrees Celsius (1,610 degrees F) and 1,026 degrees Celsius (1880 degrees F). In other words, hot sand is being blown in the winds of the brown dwarfs. The absorption signatures of carbon monoxide, methane and water vapor were also identified.

Intriguingly, the light curve for each brown dwarf (a graph of each brown dwarf's brightness over time) displays considerable variability. This has been interpreted as stormy conditions blowing clouds at various altitudes, and gaps appearing between those clouds that allows for views into deeper layers of the atmosphere. The light curves also show peaks at specific wavelengths — carbon monoxide at 2.3 microns and 4.2 microns (millionths of a meter), methane at 3.3 microns, and silicate grains tentatively at 8.3 microns to 8.5 microns.

Biller's team interpret the peaks at these wavelengths as indicating three different layers where there is a significant change in atmospheric pressure on each brown dwarf. There's a deep layer producing signals greater than 2.3 microns but less than 8.5 microns, an intermediate altitude layer absorbing light at between 2.3 and 4.2 microns, and a high altitude layer with exhibiting signals between 4.2 and 8.5 microns.

The findings indicate the power of the JWST to be able to probe, for the first time, the vertical profile (i.e. the conditions at different depths) of the atmosphere of a brown dwarf, and, in fact, there's no reason the JWST has to stop there. As the research paper describing the findings concludes: "This is the first such study, but will not be the last — in the next few observing cycles, JWST will transform our understanding of both brown dwarf and young, giant exoplanet atmospheres."

"Our findings show that we are on the cusp of transforming our understanding of worlds far beyond our own," said Biller in a statement. "Insights such as these can help us understand the conditions not just on celestial objects like brown dwarfs, but also on giant exoplanets beyond our solar system. Eventually, the techniques we are refining here may enable the first detections of weather on habitable planets like our own, which orbit other stars."

The findings were published on July 15 in the Monthly Notices of the Royal Astronomical Society. 

Quelle: SC

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Update: 25.07.2024

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Webb images nearest super-Jupiter, opening a new window to exoplanet research

The coldest and oldest exoplanet ever imaged agrees with models of planet evolution to solar system ages

Using the James Webb Space Telescope (JWST), an MPIA-led team of astronomers imaged a new exoplanet that orbits a star in the nearby triple system Epsilon Indi. The planet is a cold super-Jupiter exhibiting a temperature of around 0 degrees Celsius and a wide orbit comparable to that of Neptune around the Sun. This measurement was only possible thanks to JWST’s unprecedented imaging capabilities in the thermal infrared. It exemplifies the potential of finding many more such planets similar to Jupiter in mass, temperature, and orbit. Studying them will improve our knowledge of how gas giants form and evolve in time.

 

“We were excited when we realised we had imaged this new planet”, said Elisabeth Matthews, a researcher at the Max Planck Institute for Astronomy in Heidelberg, Germany. She is the main author of the underlying research article published in the journal Nature. “To our surprise, the bright spot that appeared in our MIRI images did not match the position we were expecting for the planet”, Matthews points out. “Previous studies had correctly identified a planet in this system but underestimated this super-Jupiter gas giant’s mass and orbital separation”. With the help of JWST, the team was able to set the record straight.

This detection is quite unusual in several aspects. It shows the first exoplanet imaged with JWST that had not already been imaged from the ground and is much colder than the gas planets JWST has studied so far. An ‘image’ means that the planet appears as a bright dot on the images and thus represents direct evidence. The transit and radial velocity methods are indirect evidence, as the planet only reveals itself through its mediated effect.

JWST observations update previous measurements

The planet revolves around the main component of the nearby triple star system Epsilon Indi, or Eps Ind for short. Astronomical labelling conventions assign the label Eps Ind A to that primary star, a red dwarf star a little smaller and cooler than the sun. To construct the planet’s name, a “b” is appended, resulting in the designation Eps Ind Ab.

The new JWST data are consistent with a super-Jupiter having a mass six times that of Jupiter in the Solar System. Eps Ind Ab orbits its host star on an eccentric, elliptical orbit whose farthest separation from Eps Ind A should range between 20 and 40 astronomical units. One astronomical unit is the mean distance between Earth and the Sun, approximately 150 million kilometres. The new values differ considerably from earlier studies, which is why the team chose to call this a “new” planet.

Cool planets, hot science

Only a few cold gas-giant planets orbiting solar-age stars are known to date, and these have all been inferred indirectly from radial velocity measurements. By imaging and taking spectra of the planets, astronomers can study their atmospheres and trace the evolution of planetary systems compared to computational models. Studying planets in fully settled planetary systems helps tie up loose ends concerning the late stages of planetary evolution and refine our general understanding of planet formation and evolution.

The recent observations lead the way to finding many more of these cold gas-giant planets. These will allow astronomers to study a new class of exoplanets and compare them to the solar system gas giants.

How to detect cold gas planets

However, these planets are hard to find using the classical detection methods. Planets far from their host stars are typically very cold, unlike the hot Jupiters that circle their stars at separations of only a few stellar radii. Wide orbits are highly unlikely to be aligned along the line of sight to produce a transit signal. In addition, measuring their signals with the radial-velocity method is challenging when only a small section of the orbit can be monitored.

Earlier studies attempted to investigate a giant planet orbiting Eps Ind A using radial velocity measurements. However, extrapolating a small part of the orbit led to incorrect conclusions about the planet’s properties. After all, Eps Ind Ab needs around 200 years to orbit its star. Observations over a few years are insufficient to determine the orbit with high precision.

Therefore, the team around Matthews devised a different approach. They wanted to take a picture of the known planet using a method commonly known as direct imaging. Since exoplanet host stars are so bright, they outshine any other nearby object. Regular cameras would be overwhelmed by the blinding starlight.

For this reason, the team employed JWST’s MIRI (Mid-Infrared Instrument) camera equipped with a coronagraph. This light-blocking mask covers the star like an artificial eclipse. Another advantage is Eps Ind’s proximity to Earth, which is only 12 light-years. The smaller the distance to the star, the larger the separation between two objects appears in an image, providing a better chance of mitigating the host star’s interference. MIRI was the perfect choice because it observes in the thermal or mid-infrared, where cold objects shine brightly.

What do we know about Eps Ind Ab?

“We discovered a signal in our data that did not match the expected exoplanet,” says Matthews. The point of light in the image was not in the predicted location. “But the planet still appeared to be a giant planet,” adds Matthews. However, before being able to make such an assessment, the astronomers had to exclude the signal was coming from a background source unrelated to Eps Ind A.

“It is always hard to be certain, but from the data, it seemed quite unlikely the signal was coming from an extragalactic background source,” explains Leindert Boogaard, another MPIA scientist and a co-author of the research article. Indeed, while browsing astronomical databases for other observations of Eps Ind, the team came across imaging data from 2019 obtained with the VISIR infrared camera attached to the European Southern Observatory’s (ESO) Very Large Telescope (VLT). After re-analysing the images, the team found a faint object precisely at the position where it should be if the source imaged with JWST belonged to the star Eps Ind A.

The scientists also attempted to understand the exoplanet atmosphere based on the available images of the planet in three colours: two from JWST/MIRI and one from VLT/VISIR. Eps Ind Ab is fainter than expected at short wavelengths. This could indicate substantial amounts of heavy elements, particularly carbon, which builds molecules such as methane, carbon dioxide, and carbon monoxide, commonly found in gas-giant planets. Alternatively, it might indicate that the planet has a cloudy atmosphere. However, more work is needed to reach a final conclusion.

Plans and prospects

This work is only a first step towards characterising Eps Ind Ab. “Our next goal is to obtain spectra which provide us a detailed fingerprint of the planet’s climatology and chemical composition,” says Thomas Henning, Emeritus Director at MPIA, co-PI of the MIRI instrument, and a co-author of the underlying article.

“In the long run, we hope to also observe other nearby planetary systems to hunt for cold gas giants that may have escaped detection,” says Matthews. “Such a survey would serve as the basis for a better understanding of how gas planets form and evolve.”

Background information

The MPIA scientists involved in this study are Elisabeth Matthews, Leindert Boogaard, and Thomas Henning.

Other researchers include Aarynn Carter (Space Telescope Science Institute, Baltimore, USA), Caroline Morley (University of Texas at Austin, Austin, USA), and Prashant Pathak (Indian Institutes of Technology, Kanpur, India).

The MIRI consortium consists of the ESA member states Belgium, Denmark, France, Germany, Ireland, the Netherlands, Spain, Sweden, Switzerland, and the United Kingdom. The national science organisations fund the consortium’s work – in Germany, the Max Planck Society (MPG) and the German Aerospace Center (DLR). The participating German institutions are the Max Planck Institute for Astronomy in Heidelberg, the University of Cologne, and Hensoldt AG in Oberkochen, formerly Carl Zeiss Optronics.

JWST is the world’s premier space science observatory. It is an international program led by NASA jointly with its partners, ESA (European Space Agency) and CSA (Canadian Space Agency).

Quelle: Max-Planck-Gesellschaft