Journal
NATURE
Volume 582, Issue 7813, Pages 497-+Publisher
NATURE PORTFOLIO
DOI: 10.1038/s41586-020-2400-z
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Funding
- NASA [16-APROBES16-0020, NNH14CK55B, NAS5-26555]
- NASA (Exoplanet Exploration Program)
- National Science Foundation (Astronomy and Astrophysics grant) [1716202]
- Mount Cuba Astronomical Foundation
- George Mason University
- NASA's Science Mission directorate
- W. M. Keck Foundation
- Australian Research Council [LE160100001, DP180100972]
- University of Southern Queensland
- MIT
- Nanjing University
- University of Louisville
- University of California Riverside
- University of Florida
- University of Texas at Austin
- JSPS KAKENHI [JP18H01265, 18H05439]
- JST PRESTO grant [JPMJPR1775]
- NSFC [11673011]
- MINECO [ESP2016-80435-C2-2-R]
- NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51372.001-A]
- National Science Foundation [AST-1909209]
- Heising-Simons Foundation 51 Pegasi b fellowship
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1716202] Funding Source: National Science Foundation
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AU Microscopii (AU Mic) is the second closest pre-main-sequence star, at a distance of 9.79 parsecs and with an age of 22 million years(1). AU Mic possesses a relatively rare(2) and spatially resolved(3) edge-on debris disk extending from about 35 to 210 astronomical units from the star(4), and with clumps exhibiting non-Keplerian motion(5-7). Detection of newly formed planets around such a star is challenged by the presence of spots, plage, flares and other manifestations of magnetic 'activity' on the star(8,9). Here we report observations of a planet transiting AU Mic. The transiting planet, AU Mic b, has an orbital period of 8.46 days, an orbital distance of 0.07 astronomical units, a radius of 0.4 Jupiter radii, and a mass of less than 0.18 Jupiter masses at 3 sigma confidence. Our observations of a planet co-existing with a debris disk offer the opportunity to test the predictions of current models of planet formation and evolution.
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