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A planet within the debris disk around the pre-main-sequence star AU Microscopii
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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. AU Mic possesses a relatively rare and spatially resolved3 edge-on debris disk extending from about 35 to 210 astronomical units from the star, and with clumps exhibiting non-Keplerian motion. 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. 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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Cited by 3 Pith papers
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Three new exoplanet systems from the Dispersed Matter Planet Project
DMPP-7 hosts a confirmed 0.72 Saturn-mass planet at P=4.93 days; HD 67200 and HD 2134 show moderate evidence for 2.7-2.8 day low-mass candidates that remain unconfirmed.
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Unstable magnetospheric accretion on the T Tauri star TW Hya
TW Hya’s large-scale field is a ~0.83 kG tilted dipole that varies yearly; accretion is unstable (rmag/rcor ≈ 0.33–0.40) and no close-in planet is detected above ~0.3–1 Mjup.
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CHEOPS photometry from 2024 reveals a reversal in the transit-timing variations of AU Mic c
2024 CHEOPS transit timings of AU Mic c show a reversal of the 2023 timing offset, indicating the large deviation was not sustained.
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