47 Ursae Majoris b
An artist's impression of 47 Ursae Majoris b, depicting it as a Jovian-like planet.
|Discovered by||Marcy and|
Butler et al.
|Discovery site||United States|
|Discovery date||17 January 1996|
|Apastron||2.17 ± 0.05 AU (324,600,000 ± 7,500,000 km)|
|Periastron||2.03 ± 0.05 AU (303,700,000 ± 7,500,000 km)|
|2.10 ± 0.02 AU (314,200,000 ± 3,000,000 km)|
|Eccentricity||0.032 ± 0.014|
|1078 ± 2 d|
Average orbital speed
|21.3 ± 0.3|
|334 ± 23|
|Semi-amplitude||49.00 ± 0.87|
|Star||47 Ursae Majoris|
47 Ursae Majoris b (abbreviated 47 UMa b), formally named Taphao Thong /
In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Taphao Thong (Thai: ตะเภาทอง [tā.pʰāw.tʰɔ̄ːŋ]) for this planet. The winning name was submitted by the Thai Astronomical Society of Thailand. Taphaothong was one of two sisters associated with a Thai folk tale.
Like the majority of known extrasolar planets, Taphao Thong was discovered by detecting the changes in its star's radial velocity as the planet's gravity pulls the star around. This was achieved by observing the Doppler shift of the spectrum of Chalawan. After the discovery of the first extrasolar planet around a Sun-like star, Dimidium, astronomers Geoffrey Marcy and R. Paul Butler searched through their observational data for signs of extrasolar planets and soon discovered two: Taphao Thong and 70 Virginis b. The discovery of Taphao Thong was announced in 1996.
Orbit and mass
47 Ursae Majoris b orbits at a distance of 2.10 AU from its star, taking 1,078 days or 2.95 years to complete a revolution. It was the first long-period planet around a main sequence star to be discovered. Unlike the majority of known long-period extrasolar planets, the eccentricity of the orbit of 47 Ursae Majoris b is low.
A limitation of the radial velocity method used to detect 47 Ursae Majoris b is that only a lower limit on the planet's mass can be obtained. Preliminary astrometric measurements made by the Hipparcos satellite suggest the planet's orbit is inclined at an angle of 63.1° to the plane of the sky, which would imply a true mass 12% greater than the lower limit determined by radial velocity measurements. However, subsequent investigation of the data reduction techniques used suggests that the Hipparcos measurements are not precise enough to adequately characterise the orbits of substellar companions, and the true inclination of the orbit (and hence the true mass) are regarded as unknown.
Given the planet's high mass, it is likely that 47 Ursae Majoris b is a gas giant with no solid surface. Because the planet has only been detected indirectly, properties such as its radius, composition, and temperature are unknown. Due to its mass it is likely to have a surface gravity 6–8 times that of Earth. Assuming a composition similar to that of Jupiter and an environment close to chemical equilibrium, the upper atmosphere of the planet is expected to contain water clouds, as opposed to the ammonia clouds typical of Jupiter.
Although 47 Ursae Majoris b is outside its star's habitable zone, its gravitational influence would disrupt the orbit of planets in the outer part of the habitable zone. In addition, it may have disrupted the formation of terrestrial planets and reduced the delivery of water to any inner planets in the system. Therefore, planets located in the habitable zone of 47 Ursae Majoris are likely to be small and dry.
It has been theorized that light reflections and infrared emissions from 47 UMa b, along with tidal influence, could warm any moons in orbit around it to be habitable, despite the planet being outside the normally accepted habitable zone.
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