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A new spin to solving mystery of stellar companions

Researchers measure the spin rates of bodies thought to be either planets or tiny 'failed' stars

W. M. Keck Observatory

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IMAGE: Planetary-mass companions are more massive than Jupiter. view more 

Credit: NASA/JPL-CALTECH

Maunakea, Hawaii - Taking a picture of an exoplanet--a planet in a solar system beyond our sun -- is no easy task. The light of a planet's parent star far outshines the light from the planet itself, making the planet difficult to see.

While taking a picture of a small rocky planet like Earth is still not feasible, researchers have made strides by snapping images of about 20 giant planet-like bodies.

These objects, known as planetary-mass companions, are more massive than Jupiter, orbit far from the glare of their stars, and are young enough to still glow with heat from their formation -- all traits that make them easier to photograph.

But one big question remains: Are these planetary-mass companions actually planets, or are they instead small "failed" stars called brown dwarfs?

Brown dwarfs form like stars do--out of collapsing clouds of gas -- but they lack the mass to ignite and shine with starlight. They can be found floating on the their own in space, or they can be found orbiting with other brown dwarfs or stars. The smallest brown dwarfs are similar in size to Jupiter and would look just like a planet when orbiting a star.

Using the W. M. Keck Observatory on Maunakea, Hawaii, researchers at Caltech have taken a new approach to the mystery: they have measured the spin rates of three of the photographed planetary-mass companions and compared them to spin rates for small brown dwarfs. The results offer a new set of clues that hint at how the companions may have formed.

"These companions with their high masses and wide separations could have formed either as planets or brown dwarfs," says graduate student Marta Bryan (MS '14), lead author of a new study describing the findings in the journal Nature Astronomy. "In this study, we wanted to shed light on their origins."

"These new spin measurements suggest that if these bodies are massive planets located far away from their stars, they have properties that are very similar to those of the smallest brown dwarfs," says Heather Knutson, professor of planetary science at Caltech and a co-author of the paper.

The astronomers measured the spin rate, or the length of a day, of three planetary-mass companions known as ROXs 42B b, GSC 6214-210 b, and VHS 1256-1257 b. They used an instrument at Keck Observatory called the Near Infrared Spectrograph (NIRSpec) to dissect the light coming from the companions.

As the objects spin on their axes, light from the side that is turning toward us shifts to shorter, bluer wavelengths, while light from the receding side shifts to longer, redder wavelengths. The degree of this shifting indicates the speed of a rotating body.

The results showed that the three companions' spin rates ranged between six to 14 kilometers per second, similar to rotation rates of our solar system's gas giant planets Saturn and Jupiter.

For the study, the researchers also included the two planetary-mass companions for which spin rates had already been measured. One, β Pictoris b, has a rotation rate of 25 kilometers per second--the fastest rotation rate of any planetary-mass body measured so far.

The researchers compared the spin rates for the five companions to those measured previously for small free-floating brown dwarfs. The ranges of rotation rates for the two populations were indistinguishable. In other words, the companions are whirling about their own axes at about the same speeds as their free-floating brown-dwarf counterparts.

The results suggest two possibilities. One is that the planetary-mass companions are actually brown dwarfs. The second possibility is that the companions looked at in this study are planets that formed, just as planets do, out of disks of material swirling around their stars, but for reasons not yet understood, the objects ended up with spin rates similar to those of brown dwarfs.

Some researchers think that both newly forming planets and brown dwarfs are encircled by miniature gas disks that might be helping to slow their spin rates. In other words, similar physical processes may leave planets and brown dwarfs with similar spin rates.

"It's a question of nature versus nurture," says Knutson. "Were the planetary companions born like brown dwarfs, or did they just end up behaving like them with similar spins?"

The team also says that the companions are spinning more slowly than expected. Growing planets tend to be spun up by the material they pull in from a surrounding gas disk, in the same way that spinning ice skaters increase their speed, or angular momentum, when they pull their arms in. The relatively slow rotation rates observed for these objects indicate that they were able to effectively put the brakes on this spin-up process, perhaps by transferring some of this angular momentum back to encircling gas disks. The researchers are planning future studies of spin rates to further investigate the matter.

"Spin rates of planetary-mass bodies outside our solar system have not been fully explored," says Bryan. "We are just now beginning to use this as a tool for understanding formation histories of planetary-mass objects."

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The study, titled, "Constraints on the Spin Evolution of Young Planetary-MassCompanions," was funded by NASA and the Sloan Research Fellowship Program. Other authors include Caltech's Konstantin Batygin (MS '10, PhD '12), assistant professor of planetary science and Van Nuys Page Scholar; Björn Benneke, formerly of Caltech and now of the University of Montreal; and Brendan Bowler of the University of Texas at Austin.

ABOUT W. M. KECK OBSERVATORY

The W. M. Keck Observatory telescopes are among the most scientifically productive on Earth. The two, 10-meter optical/infrared telescopes on the summit of Maunakea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometers, and world-leading laser guide star adaptive optics systems.

The data presented herein were obtained at Keck Observatory, which is a private 501(c) 3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

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