Constraining Stellar Rotation at the ZAMS

Douglas, Stephanie T.; Chavez, J.; Cargile, Phillip A.; Huang, Chelsea X.; Wright, Nicholas J.; Zhou, George; Howell, Steve B.; Kraus, Adam L.

doi:10.5281/zenodo.5131306

Cited by 4 publications

(2 citation statements)

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“…It is challenging to convert these stellar rotation periods to a precise age estimate, since on the pre-main-sequence the stars are spinning up due to thermal contraction rather than down due to magnetized braking. Regardless, the rotation period distributions of both CH-2 and RSG-5 seem consistent with other 30 Myr to 50 Myr clusters (e.g., IC 2602 and IC 2391; Douglas et al 2021). They also seem consistent with the false positive rates estimated from the colorabsolute magnitude diagrams.…”

Section: Stellar Rotation Periodssupporting

confidence: 83%

Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association

Bouma¹,

Kerr²,

Curtis³

et al. 2022

Preprint

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Section: Stellar Rotation Periodssupporting

confidence: 83%

Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association

Bouma¹,

Kerr²,

Curtis³

et al. 2022

Preprint

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“…The majority of these stars fall below the "slow sequence" of the Pleiades, consistent with a gyrochronal age for the δ Lyr cluster below 100 Myr. In fact, the rotation−color distributions of other 30 Myr to 50 Myr clusters (e.g., IC 2602 and IC 2391) are indistinguishable (Douglas et al 2021). Approximately 10 of the δ Lyr cluster stars appear as outliers above the "slow sequence."…”

Section: Stellar Rotation Periodsmentioning

confidence: 96%

A 38 Million Year Old Neptune-sized Planet in the Kepler Field

Bouma

Curtis

Masuda

et al. 2022

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Kepler 1627A is a G8V star previously known to host a 3.8 R ⊕ planet on a 7.2 day orbit. The star was observed by the Kepler space telescope because it is nearby (d = 329 pc) and it resembles the Sun. Here, we show using Gaia kinematics, TESS stellar rotation periods, and spectroscopic lithium abundances that Kepler 1627 is a member of the 38 − 5 + 6 Myr old δ Lyr cluster. To our knowledge, this makes Kepler 1627Ab the youngest planet with a precise age yet found by the prime Kepler mission. The Kepler photometry shows two peculiarities: the average transit profile is asymmetric, and the individual transit times might be correlated with the local light-curve slope. We discuss possible explanations for each anomaly. More importantly, the δ Lyr cluster is one of ∼103 coeval groups whose properties have been clarified by Gaia. Many other exoplanet hosts are candidate members of these clusters; their ages can be verified with the trifecta of Gaia, TESS, and ground-based spectroscopy.

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Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association

Bouma

Kerr

Curtis

et al. 2022

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Stellar positions and velocities from Gaia are yielding a new view of open cluster dispersal. Here we present an analysis of a group of stars spanning Cepheus (l = 100°) to Hercules (l = 40°), hereafter the Cep-Her complex. The group includes four Kepler objects of interest: Kepler-1643 b (R p = 2.32 ± 0.13 R ⊕, P = 5.3 days), KOI-7368 b (R p = 2.22 ± 0.12 R ⊕, P = 6.8 days), KOI-7913 Ab (R p = 2.34 ± 0.18 R ⊕, P = 24.2 days), and Kepler-1627 Ab (R p = 3.85 ± 0.11 R ⊕, P = 7.2 days). The latter Neptune-sized planet is in part of the Cep-Her complex called the δ Lyr cluster. Here we focus on the former three systems, which are in other regions of the association. Based on kinematic evidence from Gaia, stellar rotation periods from TESS, and spectroscopy, these three objects are also ≈40 million years (Myr) old. More specifically, we find that Kepler-1643 is 46 − 7 + 9 Myr old, based on its membership in a dense subcluster of the complex called RSG-5. KOI-7368 and KOI-7913 are 36 − 8 + 10 Myr old, and are in a diffuse region that we call CH-2. Based on the transit shapes and high-resolution imaging, all three objects are most likely planets, with false-positive probabilities of 6 × 10−9, 4 × 10−3, and 1 × 10−4 for Kepler-1643, KOI-7368, and KOI-7913, respectively. These planets demonstrate that mini-Neptunes with sizes of ≈2 Earth radii exist at ages of 40 Myr.

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Constraining Stellar Rotation at the ZAMS

Cited by 4 publications

References 0 publications

Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association

Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association

A 38 Million Year Old Neptune-sized Planet in the Kepler Field

Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association

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