Kinematic Groups in the Corona of the Ursa Majoris Flow Indicated by Gaia Data

Верещагин, С. В.; Чупина, Н. В.; Postnikova, E. S.

doi:10.1134/s1063772918080085

Cited by 2 publications

(2 citation statements)

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“…HD 63433 was first identified as a possible member of UMaG by Gaidos (1998) based on its kinematics and X-ray luminosity and has since been included as a candidate or likely member in multiple analyses (e.g., King et al 2003;Fuhrmann 2008 ;Vereshchagin et al 2018). The spatial and kinematic definition of UMaG was most recently updated by Gagné et al (2018), who identified central values of ( ) ( ) = -+ + X Y Z , , 7.5, 9.9, 21.9 pc and ( ) (…”

Section: Membership To Ursa Major and Agementioning

confidence: 99%

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

Mann

Johnson

Vanderburg

et al. 2020

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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 0.03 * ) star. Through kinematics, lithium abundance, and rotation, we confirm that HD 63433 is a member of the Ursa Major moving group (τ=414±23 Myr). Based on the TESS light curve and updated stellar parameters, we estimate that the planet radii are 2.15±0.10 R ⊕ and 2.67±0.12 R ⊕ , the orbital periods are 7.11

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Section: Membership To Ursa Major and Agementioning

confidence: 99%

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

Mann

Johnson

Vanderburg

et al. 2020

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show abstract

“…We adopt this measurement as the cluster age for analyses in this paper. HD 63433 was first identified as a possible member of UMaG by Gaidos (1998) based on its kinematics and X-ray luminosity, and has since been included as a candidate or likely member in multiple analyses (e.g., King et al 2003;Vereshchagin et al 2018). The spatial and kinematic definition of UMaG was most recently updated by Gagné et al (2018), who identified central values of (X, Y, Z) = (−7.5, +9.9, +21.9) pc and (U, V, W ) = (+14.8, +1.8, −10.2) km s −1 , along with full covariance matrices for these parameters.…”

Section: Membership To Ursa Major and Agementioning

confidence: 99%

TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

Mann,

Johnson,

Vanderburg

et al. 2020

Preprint

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Exoplanets can evolve significantly between birth and maturity as their atmospheres, orbits, and structures are shaped by their environment. Young planets (<1 Gyr) offer the opportunity to probe these sculpting processes. 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 ± 0.03) star. Through kinematics, lithium abundance, and rotation, we confirm that HD 63433 is a member of the Ursa Major moving group (τ = 414 ± 23 Myr). Based on the TESS light curve and updated stellar parameters, the planet radii are 2.15 ± 0.10R ⊕ and 2.67 ± 0.12R ⊕ , the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than abut 0.2. Using HARPS-N velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating the orbit is prograde. Since the host star is bright (V=6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.

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Kinematic Groups in the Corona of the Ursa Majoris Flow Indicated by Gaia Data

Cited by 2 publications

References 44 publications

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

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

TESS Hunt for Young and Maturing Exoplanets (THYME) III: a two-planet system in the 400 Myr Ursa Major Group

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