NEWS
Evidence discovered for two distinct giant planet populations
2017 July 05

Artistic impression that shows the formation of a gas giant planet in the ring of dust around a young star. Credit: ESO/L. CalŃadaPlanet mass vs metallicity for the analysed stars. In the plot one can see the position of the two populations of giant planets. Credit: Santos et al. 2017Artistic impression of a young star surrounded by a protoplanetary disc. Concentric rings of gas, with gaps indicating where planets are forming, are visible. Credit: ESO/L.CalŠada
In a paper1 highlighted today by Astronomy & Astrophysics journal, a team2 of researchers from the Instituto de Astrofísica e Ciências do Espaço (IA3) discovered observational evidence for the existence of two distinct populations of giant planets.

So far, more than 3500 planets have been detected orbiting solar type stars. Although recent results suggest that most planets in our Galaxy are rocky like Earth, a large population of giant planets, with masses that can go up to 10 or 20 times the mass of Jupiter (itself 320 times the mass of the Earth), was also discovered.

A large amount of the information about how these planets are formed is coming from the analysis of the connection between the planets and their host star. Initial findings have shown, for example, that there is a tight connection between the metallicity4 of the star and the planet occurrence or frequency. Stellar mass has also been suggested to influence planet formation efficiency.

State-of the art models of planet formation suggest that two main avenues exist for the formation of gas giants. The so called core-accretion process says that first you form a rocky/icy core, and then this core draws gas around it, giving origin to a giant planet. The other suggests that instabilities in the protoplanetary disk5 can lead to the formation of gas clumps, which then contract to form a giant planet.

Vardan Adibekyan (IA & Universidade do Porto) comments: “Our team, using public exoplanet data, obtained an interesting observational evidence that giant planets such us Jupiter and its larger mass cousins, several thousand times more massive than the Earth (of which we do not have an example in the Solar System) form in different environments, and make two distinct populations.”

While objects smaller than about 4 Jupiter masses show a strong preference for metal-rich stars, in the 4 to 20 Jupiter mass range, host stars tend to be more metal-poor and more massive, suggesting that these massive giant planets form with a different mechanism than their lower mass brothers. Nuno Cardoso Santos  (IA & Faculdade de Ciências da Universidade do Porto) adds: “The result now published suggests that both mechanisms may be at play, the first forming the lower mass planets, and the other one responsible for the formation of the higher mass ones.”

On one side, the lower mass giant planets (mass below 4 Jupiter masses) seem to be formed by the core-accretion process, around more metal-rich stars, while more massive planets seem to be formed mainly through gravitational instability. But Adibekyan adds that: “Although this discovery was a large and important step towards a complete understanding of planet formation, it is not the last and final one. Our team will enthusiastically continue addressing many still open questions.”

Observations with GAIA (ESA), whose sensitivity will allow the detection of thousands of giant exoplanets in long period orbits around stars of different masses, may shed some light into this. In the near future, missions like ESA’s CHEOPS  and PLATO, or NASA’s TESS, which will allow for the study of mass-radius relation, along with studies of their atmospheric composition using instruments such as ESO’s ESPRESSO at the VLT and HIRES at the ELT, or the James Webb Space Telescope (JWST), may also bring new constraints about the processes of planet formation.

NOTES
  1. The article “Observational evidence for two distinct giant planet populations” was published in the journal Astronomy & Astrophysics Vol. 603, A30 (DOI: 10.1051/0004-6361/201730761).
  2. The team is N. C. SantosV. AdibekyanP. FigueiraD. T. AndreasenS. C. C. Barros, E. Delgado-MenaO. Demangeon, J. P. Faria, M. Oshagh, S. G. SousaP. T. P. Viana, and A.C.S. Ferreira.
  3. The Instituto de Astrofísica e Ciências do Espaço (Institute of Astrophysics and Space Sciences – IA) is the largest Portuguese research unit in space sciences and integrates researchers from the University of Lisbon and the University of Porto. The institute encompasses most of the field’s national scientific output and it was evaluated as Excellent in the last evaluation from the European Science Foundation (ESF). IA’s activity is funded by national and international funds, including Fundação para a Ciência e a Tecnologia (UID/FIS/04434/2013), POPH/FSE and FEDER through COMPETE 2020.
  4. In astronomy, elements that are not hydrogen or helium are generally referred to as “metals”. The metallicity of a star refers to the quantity of “metals” that it has in its composition.
  5. A protoplanetary disk is a disk of gas and dust which rotates around a central star (or stars). This material will eventually give birth to planets.

Contacts
Science Communication Group

Instituto de Astrof√≠sica e Ci√™ncias do Espa√ßo Universidade do Porto Faculdade de Ciências da Universidade de Lisboa Funda√ß√£o para a Ci√™ncia e a Tecnologia