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ROXs 42Bb is a directly imaged planetary-mass companion [1] to the binary M star ROXs 42B, [4] a likely member of the Rho Ophiuchi cloud complex. The companion was announced/discovered on October 17, 2013, by University of Toronto astronomer Thayne Currie .
The planet is calculated to have an accretion rate up to 10 −8 M ☉ per year assuming a planetary mass of 15 M Jup, which would correspond to a planetary radius of 0.13 R ☉ based on evolutionary tracks. [18] Thus, HD 100546 c is either in a relatively quiescent stage or its growth from accretion is at a low level or has already ceased. [18]
The sizes are listed in units of Jupiter radii (R J, 71 492 km).This list is designed to include all planets that are larger than 1.6 times the size of Jupiter.Some well-known planets that are smaller than 1.6 R J (17.93 R 🜨 or 114 387.2 km) have been included for the sake of comparison.
Exoplanets have been discovered using several different methods for collecting or combining direct images to isolate planets from the background light of their star. Non-Redundant Aperture Masking Interferometry is a method of combining the views of multiple telescopes into a single image, while the other methods are algorithms for combining ...
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Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively; hence the planet c is 1.11 times further from star than b. There have been unconfirmed detections of co-orbital pairs of exoplanet, each of which has a semi-major axis ratio of almost 1. Largest semi-major axis ratio between consecutive planets HD 83443 b and HD 83443 c
Thus ROXs 42 Bb, GQ Lupi b and HD 100546 b might actually be brown dwarfs. Thus it would be improper to say that they are the biggest planets, and CT Cha b (316 000 km) will get the record for now. --Joey P. - THE OFFICIAL 03:35, 14 July 2017 (UTC) No. HD 100546 b, ROXs 42Bb and GQ Lupi b are planets because they are not massive enough.
PSO J318.5−22 is an extrasolar object of planetary mass that does not orbit a parent star, it is an analog to directly imaged young gas giants. [6] There is no consensus yet among astronomers whether the object should be referred to as a rogue planet , [ 7 ] [ 8 ] as a young brown dwarf , [ 9 ] [ 10 ] or as a sub-brown dwarf .