Brown Dwarf Is Actually a Planetary Mass Object
Sometimes a brown dwarf is actually a planet — or planet-like anyway.
A team led by Carnegie’s Jonathan Gagné, and including researchers from the Institute for Research on Exoplanets (iREx) at Université de Montréal, the American Museum of Natural History, and University of California San Diego, discovered that what astronomers had previously thought was one of the closest brown dwarfs to our own Sun is in fact a planetary mass object.
Their results are published by The Astrophysical Journal Letters.
Smaller than stars, but bigger than giant planets, brown dwarfs are too small to sustain the hydrogen fusion process that fuels stars and allows them to remain hot and bright for a long time. So after formation, brown dwarfs slowly cool down and contract over time. The contraction usually ends after a few hundred million years, although the cooling is continuous.
“This means that the temperatures of brown dwarfs can range from as hot as stars to as cool as planets, depending on how old they are,” said the AMNH’s Jackie Faherty, a co-author on this discovery.
The team determined that a well-studied object known as SIMP J013656.5+093347, or SIMP0136 for short, is a planetary like member of a 200-million-year-old group of stars called Carina-Near.
Groups of similarly aged stars moving together through space are considered prime regions to search for free-floating planetary like objects, because they provide the only means of age-dating these cold and isolated worlds. Knowing the age, as well as the temperature, of a free-floating object like this is necessary to determine its mass.
Gagné and the research team were able to demonstrate that at about 13 times the mass of Jupiter, SIMP0136 is right at the boundary that separates brown dwarf-like properties, primarily the short-lived burning of deuterium in the object’s core, from planet-like properties.
Free-floating planetary mass objects are valuable because they are very similar to gas giant exoplanets that orbit around stars, like our own solar system’s Jupiter or Saturn, but it is comparatively much easier to study their atmospheres. Observing the atmospheres of exoplanets found within distant star systems is challenging, because dim light emitted by those orbiting exoplanets is overwhelmed by the brightness of their host stars, which blinds the instruments that astronomers use to characterize an exoplanet’s atmospheres.
“The implication that the well-known SIMP0136 is actually more planet-like than we previously thought will help us to better understand the atmospheres of giant planets and how they evolve,” Gagné said.
They may be easier to study in great detail, but these free-floating worlds are still extremely hard to discover unless scientists spend a lot of time observing them at the telescope, because they can be located anywhere in the sky and they are very hard to tell apart from brown dwarfs or very small stars. For this reason, researchers have confirmed only a handful of free-floating planetary like objects so far.
Étienne Artigau, co-author and leader of the original SIMP0136 discovery, added: “This newest addition to the very select club of free-floating planetary like objects is particularly remarkable, because we had already detected fast-evolving weather patterns on the surface of SIMP0136, back when we thought it was a brown dwarf.”
In a field where analyzing exoplanet atmospheres is of the utmost interest, having already seen evidence of weather patterns on an easier-to-observe free-floating object that exists away from the brightness of its host star is an exciting realization.
Reference: “SIMP J013656.5+093347 Is Likely a Planetary-Mass Object in the Carina-Near Moving Group,” Jonathan Gagné et al., 2017, to appear in Astrophysical Journal Letters [http://apjl.aas.org, preprint: https://arxiv.org/abs/1705.01625]. Other members of the research team were Adam Burgasser and Daniella Bardalez Gagliuffi of University of California San Diego and Sandie Bouchard, Loïc Albert, David LaFrenière, and René Doyon of iREx.
