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The eclipse by J1407b was not discovered until 2010, by Mark Pecaut and Eric Mamajek, and was announced in 2012. J1407b's disk spans a radius of about 90 million kilometers (56 million miles) and consists of many rings and gaps which may indicate moons are forming in orbit around the object. It was initially thought to be orbiting V1400 ...
J1407) in 2007, may have a few moons based on gaps observed in its circumstellar disk or ring system. [1] Later studies have since found that J1407b is most likely a free-floating sub-brown dwarf or rogue planet, possibly less than 6 Jupiter masses. [2] 2012 — The confirmed hot Jupiter planet WASP-12b may also possess a moon. [3]
The most recent parallax measurements by the Gaia spacecraft indicate V1400 Centauri is located 450.8 ± 0.9 light-years (138.2 ± 0.3 parsecs) from the Sun. [1] Observations of V1400 Centauri's position over time have shown that it has a southwestward [b] proper motion consistent with that of the Scorpius–Centaurus association, an OB ...
J1407b's rings span a radius of about 90 million kilometers (56 million miles) and may eventually form moons over time. Although initially thought to be orbiting V1400 Centauri, later studies suggest J1407b is likely an unbound object passing in front of the star. This is stripped down to what I think is the bare minimum.
[2] Exomoons are difficult to detect and confirm using current techniques, [3] and to date there have been no confirmed exomoon detections. [4] However, observations from missions such as Kepler have observed a number of candidates. [5] [6] Two potential exomoons that may orbit rogue planets have also been detected by microlensing.
The companion's mass is roughly 13 times the mass of Jupiter. [2] As early history on Kappa And b is filled with debate over whether it is an exoplanet or a brown dwarf, some scientists have broadly described it as a "super-Jupiter" object.
Many TNOs are often just assumed to have Pluto's density of 2.0 g/cm 3, but it is just as likely that they have a comet-like density of only 0.5 g/cm 3. [ 4 ] For example, if a TNO is incorrectly assumed to have a mass of 3.59 × 10 20 kg based on a radius of 350 km with a density of 2 g/cm 3 but is later discovered to have a radius of only 175 ...
There are three ways that thicker planetary rings have been proposed to have formed: from material originating from the protoplanetary disk that was within the Roche limit of the planet and thus could not coalesce to form moons, from the debris of a moon that was disrupted by a large impact, or from the debris of a moon that was disrupted by tidal stresses when it passed within the planet's ...