astro.wikisort.org - Meteorite

16 Cygni Bb or HD 186427 b is an extrasolar planet approximately 69 light-years (21 parsecs) away in the constellation of Cygnus.[2] The planet was discovered orbiting the Sun-like star 16 Cygni B, one of two solar-mass (M_☉) components of the triple star system 16 Cygni in 1996.[3] It orbits its star once every 799 days and was the first eccentric Jupiter and planet in a double star system to be discovered. The planet is abundant in lithium.[4]

16 Cygni Bb

Discovery
Discovered by	William D. Cochran, Artie P. Hatzes, R. Paul Butler, Geoff Marcy
Discovery site	United States
Discovery date	22 October 1996
Detection method	Radial velocity
Orbital characteristics
Semi-major axis	1.681 ± 0.097 AU (251,500,000 ± 14,500,000 km)
Eccentricity	0.689 ± 0.011[1]
Orbital period (sidereal)	798.5 ± 1.0 d
Inclination	45 or 135[1]
Time of periastron	2,446,549.1 ± 6.6
Argument of periastron	83.4 ± 2.1[1]
Semi-amplitude	50.5 ± 1.6
Star	16 Cygni B
Physical characteristics
Mass	2.38 ± 0.04[1] MJ

Discovery

In October 1996, the discovery of a planetary-mass companion to the star 16 Cygni B was announced, with a mass at least 1.68 times that of Jupiter (M_J). At the time, it had the highest orbital eccentricity of any known planet. The discovery was made by measuring the star's radial velocity.

As the inclination of the orbit cannot be directly measured and as no dynamic model of the system was then published, only a lower limit on the mass could then be determined.[1][5]

Orbit

Unlike the planets in the Solar System, the planet's orbit is highly elliptical, and its distance varies from 0.54 AU (50 million mi; 81 million km) at periastron to 2.8 AU (260 million mi; 420 million km) at apastron.[6] This high eccentricity may have been caused by tidal interactions in the binary star system, and the planet's orbit may vary chaotically between low and high-eccentricity states over a period of tens of millions of years.[7]

Preliminary astrometric measurements in 2001 suggested the orbit of 16 Cygni Bb may be highly inclined with respect to our line of sight (at around 173°).[8] This would mean the object's mass may be around 14 M_J; the dividing line between planets and brown dwarfs is at 13 M_J. However these measurements were later proved useful only for upper limits.[9]

Physical characteristics

Because the planet has only been detected indirectly by measurements of its parent star, properties such as its radius, composition, and temperature are unknown.

A mathematical study in 2012 showed that a mass of about 2.4 M_J would be most stable in this system.[1] This would make the body a true planet.

The planet's highly eccentric orbit means the planet would experience extreme seasonal effects. Despite this, simulations suggest that an Earth-like moon, should it have formed in an orbit so close to the parent star, would be able to support liquid water at its surface for part of the year.[10]

See also

• 83 Leonis Bb
• HD 80606 b
• Lists of exoplanets

References

External links

• Jean Schneider (2011). "Notes for Planet 16 Cyg B b". Extrasolar Planets Encyclopaedia. Retrieved 30 September 2011.
• "16 Cygni 2?". SolStation. Retrieved 2008-06-24.
• "16 Cygni-B". University of Illinois at Urbana–Champaign. The Planet Project. Archived from the original on 2008-05-18. Retrieved 2008-06-24.
• "16 Cyg B". Exoplanets. Archived from the original on 2009-11-25. Retrieved 2009-05-03.

На других языках

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- [en] 16 Cygni Bb

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[es] 16 Cygni Bb

16 Cygni Bb es un planeta extrasolar orbitando alrededor de la estrella 16 Cygni, una de las dos masas solares del triple sistema de estrellas del sistema 16 Cygni. Hace una órbita completa cada 799 días y fue el primer júpiter excéntrico en ser descubierto.

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[ru] 16 Лебедя B b

16 Лебедя B b — экзопланета у звезды 16 Лебедя B в тройной системе 16 Лебедя. Находится на расстоянии около 69 св. лет от Солнца в созвездии Лебедя.

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