TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major Group

  title={TESS Hunt for Young and Maturing Exoplanets (THYME). III. A Two-planet System in the 400 Myr Ursa Major Group},
  author={Andrew W. Mann and Marshall C. Johnson and Andrew M. Vanderburg and Adam L. Kraus and Aaron C. Rizzuto and Mackenna L. Wood and Jonathan L. Bush and Keighley E. Rockcliffe and Elisabeth R. Newton and David W. Latham and Eric E. Mamajek and George Zhou and Samuel N. Quinn and Pa Chia Thao and Serena Benatti and Rosario Cosentino and Silvano Desidera and A. Harutyunyan and Christophe Lovis and Annelies Mortier and Francesco A. Pepe and Ennio Poretti and Thomas G. Wilson and Martti H. Kristiansen and Robert Gagliano and Thomas Lee Jacobs and Daryll M. LaCourse and Mark R. Omohundro and Hans M. Schwengeler and Ivan A. Terentev and Stephen R. Kane and Michelle L. Hill and Markus Rabus and Gilbert A. Esquerdo and Perry L. Berlind and Karen A. Collins and Gabriel Murawski and Nezar Hazam Sallam and Michael M. Aitken and Bob Massey and George R. Ricker and Roland K. Vanderspek and Sara Seager and Joshua N. Winn and Jon M. Jenkins and Thomas Barclay and Douglas A. Caldwell and Diana Dragomir and John P. Doty and Ana Glidden and Peter Tenenbaum and Guillermo Torres and Joseph D. Twicken and Steven Villanueva Jr},
  journal={arXiv: Earth and Planetary Astrophysics},
Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets ($<$1 Gyr) offer an opportunity to probe the critical early stages of this evolution, where planets evolve the fastest. However, most of the known young planets orbit prohibitively faint stars. We present the discovery of two planets transiting HD 63433 (TOI 1726, TIC 130181866), a young Sun-like ($M_*=0.99\pm0.03$) star. Through kinematics… 
Detection of Ongoing Mass Loss from HD 63433c, a Young Mini-Neptune
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The TESS-Keck Survey. III. A Stellar Obliquity Measurement of TOI-1726 c
We report the measurement of a spectroscopic transit of TOI-1726 c, one of two planets transiting a G-type star with $V$ = 6.9 in the Ursa Major Moving Group ($\sim$400 Myr). With a precise age
The Visual Survey Group: A Decade of Hunting Exoplanets and Unusual Stellar Events with Space-Based Telescopes
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Mature super-Earths and sub-Neptunes are predicted to be ≃ Jovian radius when younger than 10 Myr. Thus, we expect to find 5–15 R ⊕ planets around young stars even if their older counterparts harbor
A PSF-based Approach to TESS High quality data Of Stellar clusters (PATHOS) – IV. Candidate exoplanets around stars in open clusters: frequency and age–planetary radius distribution
The knowledge of the ages of stars hosting exoplanets allows us to obtain an overviewon the evolution of exoplanets and understand the mechanisms affecting their life. The measurement of the ages of
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Activity of Two Young Stars of Solar Type with Planetary Systems from the Ursa Major Moving Group of Stars and the Stream Psc-Eri
High precision data from the archive of the TESS space mission are used as the basis of a study of the photometric variability of two young analogs of the Sun with planetary systems: the stars HD


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Atmospheric Escape and the Evolution of Close-In Exoplanets
  • J. Owen
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  • 2019
Exoplanets with substantial hydrogen/helium atmospheres have been discovered in abundance, many residing extremely close to their parent stars. The extreme irradiation levels that these atmospheres
Contrast sensitivities in the Gaia Data Release 2
The source detection sensitivity of Gaia is reduced near sources. To characterise this contrast sensitivity is important for understanding the completeness of the Gaia data products, in particular
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Context. Gaia Data Release 2 (Gaia DR2) contains results for 1693 million sources in the magnitude range 3 to 21 based on observations collected by the European Space Agency Gaia satellite during the
Real-time processing of the imaging data from the network of Las Cumbres Observatory Telescopes using BANZAI
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The Rossiter-McLaughlin effect observed for transiting exoplanets often requires prior knowledge of the stellar projected equatorial rotational velocity (v sini). This is usually provided by