Dimidia – SpeedyLook encyclopedia

Posted on by

Halt [ first ] (Previously called 51 Pegasi b O Belerofonte ) It is an extrasolar planet, of the hot Jupiter type, which orbits the star Helvetios. He was the first to be discovered in a star of the main sequence and was announced on October 6, 1995 by Michel Mayor and Didier Queloz in the scientific journal Nature, volume 378, page 355, [ 2 ] Using the radial speed method at the Haute-Provence Observatory with the Elodie spectrograph. This discovery marked a great advance for astronomical research.

In 2017, traces of water were discovered in the planet’s atmosphere. [ 3 ] ​

Discovery [ To edit ]

After the announcement of the discovery its existence was confirmed by Dr. Geoffrey Marcy de la San Francisco State University and Dr. Paul Butler of the University of California, Berkeley using the Hamilton spectrograph located in the Lick Observatory near San José in California. [ 4 ] ​

Residue, before 51 Pegasi B, was informally called Belerofonte. After its discovery, its existence was confirmed through multiple observations that have allowed us to know many of its characteristics. The detection method was that of radial speeds that allows the product of the planet to be measured through the orbital inclination angle: m·sin (i) = 0.468 +/- 0.007 (measured in jovian masses). This method allows us to give a lower level or minimum mass that the planet should have. Radial speed variations have an amplitude of 59 m/s and show an orbital period of 4,239 ± 0.001 days. Se ha especulado mucho sobre la posible existencia de un compañero planetario de menor masa en órbitas más alejadas al punto de que 51 Pegasi está clasificado como uno de los sistemas candidatos a albergar un planeta terrestre en la llamada franja de habitabilidad, que en este sistema, With a star so similar to the sun, it is also between 1 and 2 UA.

Although it was initially stated that it could be a rocky body since the theories of formation of gaseous giants prohibited their formation for such short distances today it is believed that such a high value of the dough is only compatible with a gaseous giant Jupiter type.

The discovery of the first extrarasolar planet was an important success of astronomical research by showing astronomers that giant planets could exist in short -term orbits, something that until then was not considered. Once it was seen that such planets could exist, a trail of discoveries of similar planets followed. Residue currently belongs to a whole category of planets called hot juices. Planets as residue are not compatible with the current planetary training models, so their discovery encouraged the debate on the new theories of planetary migration according to which the planets could throughout their lives evolve their orbits being able to approach their star a lot closer to where they originally formed. The rethinking of the training and planetary evolution thesis still continues today with the discovery of more strange worlds with more extreme orbits and masses if possible.

First direct detection of visible light [ To edit ]

The first direct detection of the visible light spectrum reflected from an exoplanet has been made by an international astronomer team about 51 pegasi b. Astronomers studied the light of 51 Pegasi B using the planet -looking for a high precision radial speed (HARPS) in the Southern European Observatory (Chair Observatory) in Chile. [ 5 ] ​ [ 6 ] ​

See also [ To edit ]

References [ To edit ]

  1. ↑ «International Astronomical Union | IAU» . www.iau.org . Retrieved on December 18, 2015 .
  2. ↑ Major, Queloz. «A Jupiter-mass companion to a solar-type star» . nature .
  3. ↑ «Water detected in the atmosphere of hot Jupiter exoplanet 51 Pegasi b» . Phys.org . February 1, 2017.
  4. ↑ Geoffrey Marcy, Paul Butler and Eric Williams (June 1, 1997). «The Planet Around 51 Pegasi» . The Astrophysical Journal 481 : 926-935. Filed from the original July 21, 2001 . Retrieved on February 17, 2008 . .
  5. ↑ physicsworld.com 2015-04-22 First visible light detected directly from an exoplanet
  6. ↑ 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. Bibcode: 2015A&A…576A.134M . arXiv: 1504.05962 . doi: 10.1051/0004-6361/201425298 .