A planet within the debris disk around the pre-main-sequence star AU Microscopii

Plavchan, Peter; Barclay, Thomas; Gagné, Jonathan; Gao, Peter; Cale, Bryson; Matzko, William; Dragomir, Diana; Quinn, S. N.; Feliz, Dax L.; Stassun, Keivan G.; Crossfield, Ian J. M.; Berardo, David; Latham, David W.; Tieu, Ben; Anglada-Escudé, G.; Ricker, G.; Vanderspek, R.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Rinehart, Stephen A.; Krishnamurthy, Akshata; Dynes, Scott; Doty, J.; Adams, Fred C.; Afanasev, Dennis; Beichman, C. A.; Bottom, Michael; Bowler, Brendan P.; Brinkworth, Carolyn; Brown, Carolyn J.; Cancino, Andrew; Ciardi, David R.; Clampin, Mark; Clark, Jake T.; Collins, Karen A.; Davison, C.; Foreman-Mackey, Daniel; Furlan, Elise; Gaidos, Eric; Geneser, Claire; Giddens, Frank; Gilbert, Emily A.; Hall, Ryan; Hellier, C.; Henry, Todd J.; Horner, Jonathan; Howard, Andrew W.; Huang, Chelsea X.; Huber, J.; Kane, Stephen R.; Kenworthy, Matthew A.; Kielkopf, John F.; Kipping, David; Klenke, Chris; Kruse, Ethan; Latouf, Natasha; Lowrance, P.; Mennesson, Bertrand; Mengel, M. W.; Mills, Sean M.; Morton, Tim; Narita, Norio; Newton, Elisabeth R.; Nishimoto, America; Okumura, Jack; Πάλλη, Ε.; Pepper, Joshua; Quintana, Elisa V.; Roberge, Aki; Roccatagliata, V.; Schlieder, Joshua E.; Tanner, Angelle; Teske, Johanna; Tinney, C. G.; Vanderburg, Andrew; Braun, Kaspar von; Walp, Bernie; Wang, Jason; Wang, Sharon Xuesong; Weigand, Denise; White, R. J.; Wittenmyer, Robert A.; Wright, D. E.; Youngblood, Allison; Zhang, Hui; Zilberman, P.

doi:10.1038/s41586-020-2400-z

Cited by 198 publications

(137 citation statements)

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“…K2 Howell et al 2014, TESS Ricker et al 2014& NGTS Wheatley et al 2018) discovering young ( 100 Myr) close-in planets has become possible. Notable recent examples are the four planets in the V1298 Tau system at an age of ∼ 24 Myr (David et al 2019), a ∼ 45 Myr old planet around DS Tuc A (Newton et al 2019), a ∼ 23 Myr old planet around AU Mic (Plavchan et al 2020) as well as other recent results from the thyme project (e.g. Rizzuto et al 2020).…”

Section: Introductionmentioning

confidence: 93%

Constraining the entropy of formation from young transiting planet

Owen

2020

Monthly Notices of the Royal Astronomical Society

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Recently K2 and TESS have discovered transiting planets with radii between ∼ 5-10 R⊕ around stars with ages <100 Myr. These young planets are likely to be the progenitors of the ubiquitous super-earths/sub-neptunes, that are well studied around stars with ages ≳ 1 Gyr. The formation and early evolution of super-earths/sub-neptunes are poorly understood. Various planetary origin scenarios predict a wide range of possible formation entropies. We show how the formation entropies of young (∼20-60 Myr), highly irradiated planets can be constrained if their mass, radius and age are measured. This method works by determining how low-mass a H/He envelope a planet can retain against mass-loss. This lower bound on the H/He envelope mass can then be converted into an upper bound on the entropy. If planet mass measurements with errors ≲ 20% can be achieved for the discovered young planets around DS Tuc A and V1298 Tau, then insights into their origins can be obtained. For these planets, higher measured planet masses would be consistent with standard core-accretion theory. In contrast, lower planet masses (≲ 6 − 7 M⊕) would require a “boil-off” phase during protoplanetary disc dispersal to explain.

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Section: Introductionmentioning

confidence: 93%

Constraining the entropy of formation from young transiting planet

Owen

2020

Monthly Notices of the Royal Astronomical Society

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“…This modeling should help identify the regions of parameter space that each mass‐loss mechanism dominates. Further, observations of atmospheric escape for the emerging class of very young planets that are the likely antecedents of mature sub‐Neptune size planets (David, Cody, et al., 2019; David, Petigura, et al., 2019; David et al., 2016; Newton et al., 2019; Plavchan et al., 2020; Rizzuto et al., 2020) offer the hope of distinguishing between the photoevaporative and core‐powered atmospheric loss mechanisms. Ultimately, our quantitative insights into how these planets formed, such as the core‐mass function and how much H/He these planets accreted, depend strongly on the assumed mass‐loss model.…”

Section: Future Directionsmentioning

confidence: 99%

The Nature and Origins of Sub‐Neptune Size Planets

2021

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Planets intermediate in size between the Earth and Neptune, and orbiting closer to their host stars than Mercury does the Sun, are the most common type of planet revealed by exoplanet surveys over the last quarter century. Results from NASA's Kepler mission have revealed a bimodality in the radius distribution of these objects, with a relative underabundance of planets between 1.5 and 2.0 R⊕. This bimodality suggests that sub‐Neptunes are mostly rocky planets that were born with primary atmospheres a few percent by mass accreted from the protoplanetary nebula. Planets above the radius gap were able to retain their atmospheres (“gas‐rich super‐Earths”), while planets below the radius gap lost their atmospheres and are stripped cores (“true super‐Earths”). The mechanism that drives atmospheric loss for these planets remains an outstanding question, with photoevaporation and core‐powered mass loss being the prime candidates. As with the mass‐loss mechanism, there are two contenders for the origins of the solids in sub‐Neptune planets: the migration model involves the growth and migration of embryos from beyond the ice line, while the drift model involves inward‐drifting pebbles that coagulate to form planets close‐in. Atmospheric studies have the potential to break degeneracies in interior structure models and place additional constraints on the origins of these planets. However, most atmospheric characterization efforts have been confounded by aerosols. Observations with upcoming facilities are expected to finally reveal the atmospheric compositions of these worlds, which are arguably the first fundamentally new type of planetary object identified from the study of exoplanets.

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“…With the library of all-sky photometry made available by the Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2016), planets around bright young stars have been identified (e.g., Newton et al 2019;E. R. Newton et al 2020, in preparation;Mann et al 2020;Plavchan et al 2020;Rizzuto et al 2020). These are the first planets around bright young stars that are suitable for in-depth characterizations, enabling the first obliquity measurements of newly formed planets (Montet et al 2020;Zhou et al 2020), as well as atmospheric studies in the near future.…”

Section: Introductionmentioning

confidence: 99%

Two Young Planetary Systems around Field Stars with Ages between 20 and 320 Myr from TESS

Zhou

Quinn

Irwin

et al. 2020

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Zhou et al. Planets around young stars trace the early evolution of planetary systems. We report the discovery and validation of two planetary systems with ages 300 Myr from observations by the Transiting Exoplanet Survey Satellite. TOI-251 is a 40 − 320 Myr old G star hosting a 2.74 +0.18 −0.18 R ⊕ mini-Neptune with a 4.94 day period. TOI-942 is a 20−160 Myr old K star hosting a system of inflated Neptune-sized planets, with TOI-942b orbiting with a period of 4.32 days, with a radius of 4.81 +0.20 −0.20 R ⊕ , and TOI-942c orbiting in a period of 10.16 days with a radius of 5.79 +0.19 −0.18 R ⊕. Though we cannot place either host star into a known stellar association or cluster, we can estimate their ages via their photometric and spectroscopic properties. Both stars exhibit significant photometric variability due to spot modulation, with measured rotation periods of ∼ 3.5 days. These stars also exhibit significant chromospheric activity, with age estimates from the chromospheric calcium emission lines and X-ray fluxes matching that estimated from gyrochronology. Both stars also exhibit significant lithium absorption, similar in equivalent width to well-characterized young cluster members. TESS has the potential to deliver a population of young planet-bearing field stars, contributing significantly to tracing the properties of planets as a function of their age.

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A planet within the debris disk around the pre-main-sequence star AU Microscopii

Cited by 198 publications

References 50 publications

Constraining the entropy of formation from young transiting planet

Constraining the entropy of formation from young transiting planet

The Nature and Origins of Sub‐Neptune Size Planets

Two Young Planetary Systems around Field Stars with Ages between 20 and 320 Myr from TESS

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