Comptes Rendus
no. S2
Hunting for Cold Exoplanets via Microlensing
[La chasse aux exoplanètes froides par la méthode des microlentilles]
Jean-Philippe Beaulieu1, 2
1 Institut d’Astrophysique de Paris, Sorbonne Universite, CNRS UMR 7095, 98bis Boulevard Arago, 75015 Paris, France
2 School of Physical Sciences, University of Tasmania, Private Bag 37 Hobart, Tasmania 7001 Australia
Comptes Rendus. Physique, Online first (2023), pp. 1-12.

La méthode des microlentilles gravitationnelles permet de détecter des planètes à des distances allant de quelques centaines de parsecs jusqu’au centre de notre Galaxie. La sensibilité maximale est atteinte pour les systèmes situés à mi-chemin du centre galactique, avec des planètes orbitant autour de l’étoile lentille à une distance de quelques UA. C’est la seule méthode qui permet actuellement de sonder les exoplanètes dans la gamme de masse Terre-Saturne au-delà de la limite des glaces, là où les scénarios d’accrétion de coeur prédisent que la plupart des planètes massives se formeraient. Bien que le nombre de planètes détectées soit relativement modeste (environ 130 planètes à ce jour) comparé aux méthodes de vitesse radiale et de transit, les microlentilles sondent une partie de l’espace des paramètres (séparation de l’hôte par rapport à la masse de la planète), qui n’est accessible à moyen terme à aucune autre technique. Les microlentilles ont permis de découvrir la première super-Terre froide et la première planète Jupiter en orbite autour d’une naine blanche. Elles ont aussi détecté des Terres, super-Terres, Neptunes, Saturnes, Jupiters, super-Jupiters, naines brunes orbitant autour d’étoiles de la séquence principale dans la gamme de masse 0.08-1M ⊙ . Cette approche a aussi permis d’observer des planètes circumbinaires, des Jupiters dans la zone habitable, le premier candidat exolune et des planètes soit non-liées à une étoile, soit sur des orbites très lointaines. Les microlentilles ont été les premièrs à montrer que la présence d’une planète est la règle pour les étoiles de notre galaxie et que les super-Terres et Neptunes sont plus abondantes que les planètes telluriques de plus petite masse. Les observations actuelles fourniront très prochainement la fonction de masse des planètes froides jusqu’à quelques masses terrestres. La phase suivante sera un grand relevé de 450 jours avec le télescope spatial Nancy Grace Roman de la NASA à partir de 2027. Il donnera plus de 3000 planètes et fournira la fonction de masse des planètes froides jusqu’à la masse de Mars. S’il est combiné à la mission spatiale Européenne Euclid, il sera en mesure de rechercher des planètes telluriques non-liées, de mesurer leur masse et leur abondance.

Microlensing can detect planets at distances ranging from a few hundred parsecs all the way to the Galactic center. The maximum sensitivity is reached for systems that are located half way to the galactic center, with planets orbiting the lens star at a separation of few AUs. It is the only method currently probing exoplanets in the Earth-Saturn mass range beyond the snow line, where the core accretion theory originally predicted that most massive planets would form. Although the number of detected planets is relatively modest (∼130 planets to date) compared to that discovered by radial velocity and transit methods, microlensing probes a part of the parameter space (host separation as a function of planet mass), which is mostly not accessible in the medium term to any other technique. Microlensing has discovered the first cold super-Earth, and the first Jupiter planet orbiting a white dwarf. It also detected a number of Earth, Super-Earth, Neptune, Saturn, Jupiter, super-Jupiter orbiting main sequence stars in the mass range 0.08-1M ⊙ . It also observed circumbinary planets, Jupiter in the habitable zone, the first exomoon candidate and free-floating planets. It has shown that having a planet is the rule for stars in our galaxy and shown that super-Earth and Neptune are more abundant than smaller mass telluric planets. Ground based microlensing will provide soon the mass function of cold planets down to few Earth Masses. The next phase, is a 450 days survey with the NASA Nancy Grace Roman Space Telescope from 2027. It will detect 3000+ planets and provide the mass function of cold planets down to the mass of Mars. If combined with the European Euclid Space mission, we will be able to probe for free-floating telluric planets and measure their masses.

Reçu le :
Accepté le :
Première publication :
DOI : 10.5802/crphys.151
Keywords: Exoplanets, Gravitational Lensing, Observations, Detection of Exoplanets, Planetary Systems, Micro-lensing
Mot clés : Exoplanètes, lentilles gravitationnelles, observations, détection des exoplanètes, systèmes planétaires, micro-lentilles
Jean-Philippe Beaulieu 1, 2

1 Institut d’Astrophysique de Paris, Sorbonne Universite, CNRS UMR 7095, 98bis Boulevard Arago, 75015 Paris, France
2 School of Physical Sciences, University of Tasmania, Private Bag 37 Hobart, Tasmania 7001 Australia
Licence : CC-BY 4.0
Droits d'auteur : Les auteurs conservent leurs droits 
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     author = {Jean-Philippe Beaulieu},
     title = {Hunting for {Cold} {Exoplanets} via {Microlensing}},
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Jean-Philippe Beaulieu. Hunting for Cold Exoplanets via Microlensing. Comptes Rendus. Physique, Online first (2023), pp. 1-12. doi : 10.5802/crphys.151.

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