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J1407b is a substellar object, either a free-floating planet or brown dwarf, with a massive circumplanetary disk or ring system.It was first detected by automated telescopes in 2007 when its disk eclipsed the star V1400 Centauri, causing a series of dimming events for 56 days.
V1400 Centauri, also known as 1SWASP J140747.93−394542.6 or simply J1407, is a young, pre-main-sequence star that was eclipsed by the likely free-floating substellar object J1407b in April–June 2007.
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]
J1407b is a substellar object, possibly a free-floating planet, with a massive ring system or circumplanetary disk. It was first detected in 2007 when its rings eclipsed the star V1400 Centauri , causing a series of dimming events for 56 days.
J1407b.ogv (Ogg multiplexed audio/video file, Theora/Vorbis, length 27 s, 640 × 480 pixels, 3.24 Mbps overall, file size: 10.55 MB) This is a file from the Wikimedia Commons . Information from its description page there is shown below.
Comment: The J1407b article was converted from redirect into article as a result of a split from the V1400 Centauri article. I began slowly expanding V1400 Centauri on 8 July 2024, but I did not add much to the J1407b section until 24 July 2024. As of today, it's been 5 days since I significantly expanded the J1407b section.
This video shows an artist's impression of the free-floating planet CFBDSIR J214947.2-040308.9.. A rogue planet, also termed a free-floating planet (FFP) or an isolated planetary-mass object (iPMO), is an interstellar object of planetary mass which is not gravitationally bound to any star or brown dwarf.
HD 189733 b is an exoplanet in the constellation of Vulpecula approximately 64.5 light-years (19.8 parsecs) away [7] from the Solar System.Astronomers in France discovered the planet orbiting the star HD 189733 on October 5, 2005, by observing its transit across the star's face. [1]