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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.
“Sometimes, people zombie out of boredom: they have lost interest in someone, found interest in someone else, and then maybe things didn’t work out with that person so they’re looking to ...
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 ...
Serena Williams and her daughter Adira River Ohanian had a fun beach day. "My mini mini @adiraohanian wanted to take a dip in the ocean," Williams captioned the post. In one photo, Adira dips her ...
Brian Cox defended Kevin Spacey in a new interview with U.K. publication The i Paper, calling the Oscar winner “an old friend of mine” and asking the public: “How dare you cancel anybody?”
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