Astronomical objects of planetary size that did not form in orbit around a star
Comparison: theSun (yellow), a young sub-brown dwarf (red), andJupiter (multi-colored). As the sub-brown dwarf ages, it will gradually cool and shrink.
Sub-brown dwarfs are formed in the manner ofstars, through the collapse of agas cloud (perhaps with the help ofphoto-erosion) but there is no consensus amongst astronomers on whether the formation process should be taken into account when classifying an object as a planet.[4] Free-floating sub-brown dwarfs can be observationally indistinguishable from rogue planets, which originally formed around a star and were ejected from orbit. Similarly, a sub-brown dwarf formed free-floating in a star cluster may be captured into orbit around a star, making distinguishing sub-brown dwarfs and large planets also difficult. A definition for the term "sub-brown dwarf" was put forward by theIAU Working Group on Extra-Solar Planets (WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.[5]
The smallest mass of gas cloud that could collapse to form a sub-brown dwarf is about 1Jupiter mass (MJ).[6] This is because to collapse bygravitational contraction requires radiating away energy as heat and this is limited by the opacity of the gas.[7] A 3 MJ candidate is described in a 2007 paper.[8]
There is no consensus whether these companions of stars should be considered sub-brown dwarfs or planets. Some authors agree these objects should be considered sub-brown dwarfs, since they likely formed on their own, like a "failed star".[9]
Nonetheless, theIAU working definition of an exoplanet ignored formation mechanism as a criterion, and based on it these objects would be considered planets.[10]
At around 2022 the IAU working definition of an exoplanet excludes these objects as planets.[10] The only fitting label would be as sub-brown dwarfs, but they are more often referred asplanetary mass objects. Other definitions, like from theNASA Exoplanet Archive[11] would include these as exoplanets. There is no consensus whether these companions of brown dwarfs should be considered sub-brown dwarfs or planets.
WISE J0336−0143B, orbits a brown dwarf or sub-brown dwarf. The primary has a mass of 8.5 to 18MJ and secondary has a mass of 5-11.5MJ. This object does not fit the IAU working definition of anexoplanet.[10] This definition requires a mass ratio of about q<0.04, but the mass ratio of WISE J0336−0143AB is q=0.61±0.05.[12] It also does not fit the definition of arogue planet, because it is gravitationally bound to a brown dwarf (or possibly sub-brown dwarf). It could be considered a planet according to alternative definitions, but according to the IAU it only fits the definition of sub-brown dwarf.
2M1207b orbits around a young brown dwarf with a circumstellar disk and itself is likely surrounded by a circumstellar disk. The mass ratio is well above the upper limit of q=0.04 for exoplanets according to the IAU.[13]
