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Title Planet Star Data Notes Most massive The most massive planet is difficult to define due to the blurry line between planets and brown dwarfs.If the borderline is defined as the deuterium fusion threshold (roughly 13 M J at solar metallicity [30] [b]), the most massive planets are those with true mass closest to that cutoff; if planets and brown dwarfs are differentiated based on formation ...
Planet Discovery method Mass (M J) Radius (R J) Density (g/cm 3) Orbital period ()Semimajor axis ()Orbital eccentricity Year of confirmation Ref. Earth (for reference): 0.003 15
This method works best for young planets that emit infrared light and are far from the glare of the star. Currently, this list includes both directly imaged planets and imaged planetary-mass companions (objects that orbit a star but formed through a binary-star-formation process, not a planet-formation process).
On February 26, 2014, NASA announced the discovery of 715 newly verified exoplanets around 305 stars by the Kepler Space Telescope. The exoplanets were found using a statistical technique called "verification by multiplicity". 95% of the discovered exoplanets were smaller than Neptune and four, including Kepler-296f, were less than 2 1/2 the ...
The timeline of discovery of Solar System planets and their natural satellites charts the progress of the discovery of new bodies over history. Each object is listed in chronological order of its discovery (multiple dates occur when the moments of imaging, observation, and publication differ), identified through its various designations (including temporary and permanent schemes), and the ...
By RYAN GORMAN Scientists may have found Planet X -- the long-rumored object believed to be larger than Earth and further from the sun than Pluto. Planet X and another object dubbed "Planet Y ...
The planets were detected by observing small dips in the star's brightness when they crossed in front of it from our vantage point. The innermost planet takes about nine days to orbit the star ...
Tadmor: The radial velocity variations of the star Errai were announced in 1989, consistent with a planet in a 2.5-year orbit. [5] However, misclassification of the star as a giant combined with an underestimation of the orbit of the Gamma Cephei binary, which implied the planet's orbit would be unstable, led some astronomers to suspect the variations were merely due to stellar rotation.