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Exoplanetary Scratchpad

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Young massive star with the first discovered circumstellar disk and the source of most interstellar meteorites in the Solar System. Comet crystals were found to be similar composition as those in Solar System. The first exo-comet was discovered in this system in 1983 and is the only star known with a detected comet known to also have a planet. Hundreds of comets detected by transit, of which on average of 6 transits occur in a 30 minute spetra, have been placed into two groups. One family (Population D for "deep" absorption lines) were older comets depleted of their volatiles and trapped in mean motion resonance with planet b or another undiscovered one. The other is fresher (Population S for "shallow"), emit more dust, follow similar orbits, and may have been formed after the breakup of a larger object. Contains the youngest known exo-planet, which shows that Jupiter-like planets can form much quicker than previously believed. It is the closest-in exoplanet photographed and is at 8 AU and 7-11 Jupiter Masses and orbits in 20 years. This planet was first hinted at by studying dust disks in 2003 and first photographed in 2003, but it was not confirmed and was lost. It was imaged again in 2008, and became the first imaged exoplanet confirmed to move around its star in 2010. It has an effective temperature of 1,100 to 1,700C, showing that it is still warm and has retained much of its heat from its formation. Evidence of a planetary transit in 1981 was found in record. It was originally thought that a second planet must have caused a tilt in one of the disks, but now it known that the first planet is. Models show that it could create waves and spirals in the disk. Some data suggests the planet is unusually wide, perhaps evidence of a ring system around it. The planet is traveling through a relatively dust-free gap in the debris disk, and thought to be clearing it. The planet is losing momentum as it travels through the debris disk. A large belt of carbon monoxide 50-160 AU concentrated at 85 AU has been observed, possibly caused by collision of comets. A Saturn sized planet interior to the belt that is not currently detectable due to being edge on in the disk could be shepherding it. It is possible that diamond-planets are forming in the disk. A cubesat could target this star in search of a second planet using the transit method since the system is edge-on. Principle member of the Beta Pictoris Moving Group.

Beta Pictoris System Web Pages[]

Beta Pictoris System In the News[]

First Exo-Comet Discovered (1983)[]

Articles recalling this past discovery (2013):

First Planetary Dust Disk Detected (1984)[]

Comet Absorption in Circumstellar Disk Theorized (1990)[]

Source of Most of Solar System's Interstellar Dust (2000)[]

Found to be a Delta Scuti Variable Star (2003)[]

Inner Ring Found, Suggests Planetary System (2003)[]

Planet b Imaged, but unconfirmed and then lost (2003)[]

Silicate Ring Discovered (Oct 2004)[]

Japanese astronomers discover a third ring around Beta Pictoris, hinting at the existance of a planet.

Formation of Carbon Planets Speculated (2006)[]

Second Dust Disk Discovered (2006)[]

3 Possible Planets From Disk Morphology (2007)[]

Mini-Planet Embros Detected (Oct 2007)[]

Planet Visually Detected (Nov 2008)[]

Transit Detected from 1981 (2009)[]

Planet's Movement Confirmed (2010)[]

Mass and Temperature of Planet Taken (2011)[]

Feature Article on Imaged Planets (2011)[]

See Imaged Exoplanets for more systems

Planet B Responsible for Tilt in Disk, Not Another Planet (2011)[]

Diamond Planets Could be Forming (2012)[]

Fragments From Comets Found to have similar composition to those of solar system (Oct 2012)[]

Note in Exozodiac Survey (2014)[]

Two classes of comets (2014)[]

See also 49 Ceti System

Models Show Planet Warping Disks (2015)[]

Potential Target for a Cubesat (2016)[]

See Also[]