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Astronomers have located a planet-like star that’s barely warmer than a balmy summer day on Earth… it’s literally the coldest object ever directly imaged outside of our solar system!
WD 0806-661 B is a brown “Y dwarf” star that’s a member of a binary pair. Its companion is a much hotter white dwarf, the remains of a Sun-like star that has shed its outer layers. The pair is located about 63 light-years away, which is pretty close to us as stars go. The stars were identified by a team led by Penn State Associate Professor of Astronomy and Astrophysics Kevin Luhman using images from NASA’s Spitzer Space Telescope. Two infrared images taken in 2004 and 2009 were overlaid on top of each other and show the stars moving in tandem, indicating a shared orbit.
Of course, locating the stars wasn’t quite as easy as that. To find this stellar duo Luhman and his team searched through over six hundred images of stars located near our solar system taken years apart, looking for any shifting position as a pair.
The use of infrared imaging allowed the team to locate a dim brown dwarf star like WD 0806-661 B, which emits little visible light but shines brightly in infrared. (Even though brown dwarfs are extremely cool for stars they are still much warmer than the surrounding space. And, for the record, brown dwarfs are not actually brown.) Measurements estimate the temperature of WD 0806-661 B to be in the range of about 80 to 130 degrees Fahrenheit (26 to 54 degrees C, or 300 – 345 K)… literally body temperature!
“Essentially, what we have found is a very small star with an atmospheric temperature about cool as the Earth’s.”
– Kevin Luhman, Associate Professor of Astronomy and Astrophysics, Penn State
Six to nine times the mass of Jupiter, WD 0806-661 B is more like a planet than a star. It never accumulated enough mass to ignite thermonuclear reactions and thus more resembles a gas giant like Jupiter or Saturn. But its origins are most likely star-like, as its distance from its white dwarf companion – about 2,500 astronomical units – indicates that it developed on its own rather than forming from the other star’s disc.
There is a small chance, though, that it did form as a planet and gradually migrated out to its current distance. More research will help determine whether this may have been the case.
Brown dwarfs, first discovered in 1995, are valuable research targets because they are the next best thing to studying cool atmospheres on planets outside our solar system. Scientists keep trying to locate new record-holders for the coldest brown dwarfs, and with the discovery of WD 0806-661 B Luhman’s team has done just that!
A paper covering the team’s findings will be published in The Astrophysical Journal. Other authors of the paper include Ivo Labbé, Andrew J. Monson and Eric Persson of the Observatories of the Carnegie Institution for Science, Pasadena, Calif.; Didier Saumon of the Los Alamos National Laboratory, New Mexico; Mark S. Marley of the NASA Ames Research Center, Moffett Field, Calif.; and John J. Bochanski also of The Pennsylvania State University.
Read more on the Penn State science site here.
ok, I am a little confused here. I thought Brown Dwarfs were classified by their composition, not how they formed (collapse vs. accretion)
This object is far too small to have ever burned deuterium, so it’s not a brown dwarf by the standard mass threshold used in the past (i.e. >13 Jupiter masses).
Are we changing the definition to allow Jovian-sized objects that form from gas collapse to be called “brown dwarfs” now?
Why not just simply acknowledge that gas giants can occasionally form outside of a planetary disk of a parent star? After all, that’s exactly what this object is — a gas giant. Or, more accurately, a very large version of Neptune.
WD 0806-661 B is being issued as a candidate for a new brown dwarf, but it hasn’t been officially classified as such yet.
Maybe we’ll see a big knock-down drag out in the IAU over the definition of a “brown dwarf”.
We can rally up first-graders to petition astronomers, asking “why do you hate WD 0806-661 B?”
I think the classification is under debate because this is research into new objects, and because the astronomical community feels (there is a chance) that dwarfs are different from planets.
Unless dwarfs forms of themselves, they seem to form in pairs with stars or dwarfs (and may likely have planets), while planets can be numerous. And there is AFAIK still an ongoing uncertainty whether gas planets forms by accretion and/or collapse and whether they have a core or not.
There may be a continuity there, but since historically it wasn’t and it is still an open question these categories are kept separate as of yet. Or at least, that is my understanding, such as it is.
Likely an interesting system in that it’s very old. The BD probably started much closer and drifted away as the progenitor of the WD lost mass. Perhaps gaining some mass of it’s own in the process?
2500 AU eh? The period of the orbit not mentioned. The planetary nebula of the WD has totally dissipated. We will need flashlights if we go there.
AFAIC this is a just a massive gas giant. Sub-brown dwarf at best, though those are pretty much the same thing as a planet. Whether or not they have a rocky core (to me) would have more to do with the gas cloud/accretion disk, so maybe that’s where the definitions vary.
In other words, if it forms in an accretion disk, it’s a planet, and if it form from cloud collapse, it’s a brown dwarf. But then if a gas planet has little or no rocky-metallic core, or a brown dwarf is in orbit around a star, then that definition falls apart.
Honestly, if the end result is the same thing, then it shouldn’t really matter. We are simply obsessed with classifying things.