Jump to content

51 Pegasi b

Coordinates: Sky map 22h 57m 28.0s, +20° 46′ 08″
From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by PlanetStar (talk | contribs) at 20:02, 21 April 2016 (Revert to revision 702801247 dated 2016-02-01 19:19:13 by Drbogdan using popups). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

Template:Planetbox begin Template:Planetbox star Template:Planetbox orbit Template:Planetbox character Template:Planetbox discovery Template:Planetbox catalog Template:Planetbox reference Template:Planetbox end

51 Pegasi b (abbreviated 51 Peg b), unofficially dubbed Bellerophon, later named Dimidium, is an extrasolar planet approximately 50 light-years away in the constellation of Pegasus. It was the first exoplanet to be discovered orbiting a main-sequence star,[1] the Sun-like 51 Pegasi, and marked a breakthrough in astronomical research. It is the prototype for a class of planets called hot Jupiters.

Name

51 Pegasi is the Flamsteed designation of the host star. On its discovery, the planet was designated 51 Pegasi b by its discoverers and unofficially dubbed Bellerophon by the astronomer Geoffrey Marcy, in keeping with the convention of naming planets after Greek and Roman mythological figures (Bellerophon was a figure from Greek mythology who rode the winged horse Pegasus).[2]

In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars.[3] The process involved public nomination and voting for the new names.[4] In December 2015, the IAU announced the winning name was Dimidium for this planet.[5] The name was submitted by the Astronomische Gesellschaft Luzern, Switzerland. 'Dimidium' is Latin for 'half', referring to the planet's mass of at least half the mass of Jupiter.[6]

Discovery

The location of 51 Pegasi in Pegasus.

The exoplanet's discovery was announced on October 6, 1995, by Michel Mayor and Didier Queloz of the University of Geneva in the journal Nature.[7] They used the radial velocity method with the ELODIE spectrograph on the Observatoire de Haute-Provence telescope in France and made world headlines with their announcement.

The planet was discovered using a sensitive spectroscope that could detect the slight and regular velocity changes in the star's spectral lines of around 70 metres per second. These changes are caused by the planet's gravitational effects from just 7 million kilometres' distance from the star.

On October 12, 1995, less than a week after the announcement of the discovery, confirmation came from Geoffrey Marcy and Paul Butler of the University of California, Berkeley, using the Hamilton Spectrograph at the Lick Observatory near San Jose in California.

This was the first discovery of an exoplanet orbiting a Sun-like star (the first exoplanet discovery was made by Aleksander Wolszczan in 1992, around pulsar PSR 1257). It marked a turning point and forced astronomers to accept that giant planets could exist in short-period orbits. Once astronomers realized that it was worth looking for giant planets with the currently available technology, much more telescope time was devoted to radial velocity planet searches, and hence many more exoplanets in the Sun's neighborhood have been discovered.

Physical characteristics

After its discovery, many teams confirmed the planet's existence and obtained more observations of its properties. It was discovered that the planet orbits the star in around 4 days. It is much closer to it than Mercury is to the Sun,[1] moves at an orbital speed of 136 km/s, yet has a minimum mass about half that of Jupiter (about 150 times that of the Earth). At the time, the presence of a huge world so close to its star was not compatible with theories of planet formation and was considered an anomaly. However, since then, numerous other 'hot Jupiters' have been discovered[1] (see 55 Cancri and τ Boötis, for example), and astronomers are revising their theories of planet formation to account for them by studying orbital migration.

Assuming the planet is perfectly grey with no greenhouse or tidal effects, and a Bond albedo of 0.1, the temperature would be 1265 K (approximately 1000 °C / 1800 °F). This is between the predicted temperatures of HD 189733 b and HD 209458 b (1180–1392 K), before they were measured.[8]

In the report of the discovery it was initially speculated that 51 Pegasi b was the stripped core of a brown dwarf that formed in situ and was therefore composed of heavy elements, but it is now believed to be a gas giant. It is sufficiently massive that its thick atmosphere is not blown away by the star's solar wind.

51 Pegasi b probably has a greater radius than that of Jupiter despite its lower mass. This is because its superheated atmosphere must be puffed up into a thick but tenuous layer surrounding it. Beneath this, the gases that make up the planet would be so hot that the planet would glow red. Clouds of silicates may exist in the atmosphere.

The planet is tidally locked to its star, always presenting the same face to it.

The planet (with Upsilon Andromedae b) is deemed a candidate for direct imaging by Planetpol.[9] It is also a candidate for "near-infrared characterisation.... with the VLTI Spectro-Imager".[8]

The earlier, rocky-planet model was utilized as a setting by Hal Clement in the story Exchange Rate.

Direct detection of visible light

The first ever direct detection of the visible light spectrum reflected from an exoplanet has been made by an international team of astronomers on 51 Pegasi b. The astronomers studied light from 51 Pegasi b using the High Accuracy Radial velocity Planet Searcher (HARPS) instrument at the European Southern Observatory's La Silla Observatory in Chile.[10][11]

See also

References

  1. ^ a b c How the Universe Works 3. Vol. Jupiter: Destroyer or Savior?. Discovery Channel. 2014.
  2. ^ University of California at Berkeley News Release 1996-17-01
  3. ^ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  4. ^ NameExoWorlds The Process
  5. ^ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  6. ^ NameExoWorlds The Approved Names
  7. ^ Mayor, Michael; Queloz, Didier (1995). "A Jupiter-mass companion to a solar-type star". Nature. 378 (6555): 355–359. Bibcode:1995Natur.378..355M. doi:10.1038/378355a0.
  8. ^ a b Renard, S.; Absil, O.; Berger, J. -P.; Bonfils, X.; Forveille, T.; Malbet, F. (2008). "Prospects for near-infrared characterisation of hot Jupiters with the VLTI Spectro-Imager (VSI)". Proceedings of SPIE. Optical and Infrared Interferometry. 7013: 70132Z. arXiv:0807.3014. Bibcode:2008SPIE.7013E..2ZR. doi:10.1117/12.790494.
  9. ^ Lucas, P. W.; Hough, J. H.; Bailey, J. A.; Tamura, M.; Hirst, E.; Harrison, D. (2007). "Planetpol polarimetry of the exoplanet systems 55 Cnc and tau Boo". Monthly Notices of the Royal Astronomical Society. 393: 229. arXiv:0807.2568. Bibcode:2009MNRAS.393..229L. doi:10.1111/j.1365-2966.2008.14182.x.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  10. ^ physicsworld.com 2015-04-22 First visible light detected directly from an exoplanet
  11. ^ Martins, J. H. C.; Santos, N. C.; Figueira, P.; Faria, J. P.; Montalto, M.; Boisse, I.; Ehrenreich, D.; Lovis, C.; Mayor, M.; Melo, C.; Pepe, F.; Sousa, S. G.; Udry, S.; Cunha, D. (2015). "Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b". Astronomy & Astrophysics. 576: A134. arXiv:1504.05962. Bibcode:2015A&A...576A.134M. doi:10.1051/0004-6361/201425298.

Further reading


Retrieved from "https://en.wikipedia.org/w/index.php?title=51_Pegasi_b&oldid=716440401"