A Candidate Young Massive Planet in Orbit Around the Classical T Tauri Star Ci Tau*

Johns–Krull, Christopher M.; McLane, Jacob N.; Prato, L.; Crockett, Christopher; Jaffe, D. T.; Hartigan, Patrick; Beichman, Charles; Mahmud, N.; Chen, Wei; Skiff, B. A.; Cauley, P. Wilson; Jones, Joshua; Mace, Gregory N.

doi:10.3847/0004-637x/826/2/206

Cited by 126 publications

(102 citation statements)

References 120 publications

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“…It is tempting to ascribe some significance to the fact that the radius of the observed planet is only ∼ 30% beyond the corotation radius between the star and the disc (assuming that the 7 day photometric period of the star measured by Johns-Krull et al 2016 is the star's rotation period). Models of disc braking of young stars suggest that systems evolve to a state of disc locking where the disc is truncated slightly inside the corotation radius.…”

Section: Mpmentioning

confidence: 99%

“…The recent discovery of a radial velocity planet in the young, disc bearing star CI Tau (Johns-Krull et al 2016) offers the first opportunity to test theories for the formation and early evolution of hot Jupiters in discs. To date, planet discoveries in discs have derived from direct imaging (e.g Chauvin et al 2004Chauvin et al , 2005Neuhäuser et al 2005Neuhäuser et al , 2008Marois et al 2008;Kraus & Ireland 2012;Sallum et al 2015) due to difficulties in applying transit detection and radial velocity methods in young stars.…”

Section: Introductionmentioning

confidence: 99%

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The origin of the eccentricity of the hot Jupiter in CI Tau

Rosotti

Booth

Clarke

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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Following the recent discovery of the first radial velocity planet in a star still possessing a protoplanetary disc (CI Tau), we examine the origin of the planet's eccentricity (e ∼ 0.3). We show through long timescale (10 5 orbits) simulations that the planetary eccentricity can be pumped by the disc, even when its local surface density is well below the threshold previously derived from short timescale integrations. We show that the disc may be able to excite the planet's orbital eccentricity in < a Myr for the system parameters of CI Tau. We also perform two planet scattering experiments and show that alternatively the observed planet may plausibly have acquired its eccentricity through dynamical scattering of a migrating lower mass planet, which has either been ejected from the system or swallowed by the central star. In the latter case the present location and eccentricity of the observed planet can be recovered if it was previously stalled within the disc's magnetospheric cavity.

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Section: Mpmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The origin of the eccentricity of the hot Jupiter in CI Tau

Rosotti

Booth

Clarke

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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“…This system was recently found to have a candidate young massive planet based on radial velocity (RV) variations in the optical and IR (Johns-Krull et al 2016). The RV amplitude yields M sin i ∼ 8M Jup , which, in conjunction with a disk inclination of ≈46 • estimated from sub-mm continuum emission (Guilloteau et al 2014), corresponds to a planet mass of ∼11-12 M Jup .…”

Section: Tau (J04335200+2250301)mentioning

confidence: 99%

Identification of Young Stellar Variables with KELT for K2. I. Taurus Dippers and Rotators

Rodriguez

Ansdell

Oelkers

et al. 2017

ApJ

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One of the most well-studied young stellar associations, Taurus-Auriga, was observed by the extended Kepler mission, K2, in the spring of 2017. K2 Campaign 13 (C13) is a unique opportunity to study many stars in this young association at high photometric precision and cadence. Using observations from the Kilodegree Extremely Little Telescope (KELT) survey, we identify "dippers", aperiodic and periodic variables among K2 C13 target stars. This release of the KELT data (lightcurve data in e-tables) provides the community with long-time baseline observations to assist in the understanding of the more exotic variables in the association. Transient-like phenomena on timescales of months to years are known characteristics in the light curves of young stellar objects, making contextual pre-and post-K2 observations critical to understanding their underlying processes. We are providing a comprehensive set of the KELT light curves for known Taurus-Auriga stars in K2 C13. The combined data sets from K2 and KELT should permit a broad array of investigations related to star formation, stellar variability, and protoplanetary environments.

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“…Crockett et al 2012). As a result, only a handful of candidate close-in giant planets younger than 20 Myr have been unveiled so far, either using RV observations (Donati et al 2016;Johns-Krull et al 2016;Yu et al 2017) or transit photometry (David et al 2016;Mann et al 2016;David et al 2019a,b). None of them have a wellmeasured bulk density.…”

Section: Introductionmentioning

confidence: 99%

Simulated mass measurements of the young planet K2-33b

Klein

Donati

2020

Monthly Notices of the Royal Astronomical Society: Letters

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In this paper, we carry out simulations of radial velocity (RV) measurements of the mass of the 8-11 Myr Neptune-sized planet K2-33b using high-precision near infrared velocimeters like SPIRou at the Canada-France-Hawaii Telescope. We generate a RV curve containing a planet signature and a realistic stellar activity signal, computed for a central wavelength of 1.8 µm and statistically compatible with the light-curve obtained with K2. The modelled activity signal includes the effect of time-evolving dark and bright surface features hosting a 2 kG radial magnetic field, resulting in a RV signal of semi-amplitude ∼30 m s −1 . Assuming a 3-month visibility window, we build RV time-series including Gaussian white noise from which we retrieve the planet mass while filtering the stellar activity signal using Gaussian Process Regression. We find that 35/50 visits spread over 3 consecutive bright-time runs on K2-33 allow one to reliably detect planet RV signatures of respectively 10 and 5 m s −1 at precisions > 3σ. We also show that 30 visits may end up being insufficient in some cases to provide a good coverage of the stellar rotation cycle, with the result that the planet signature can go undetected or the mass estimation be plagued by large errors.

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A Candidate Young Massive Planet in Orbit Around the Classical T Tauri Star Ci Tau*

Cited by 126 publications

References 120 publications

The origin of the eccentricity of the hot Jupiter in CI Tau

The origin of the eccentricity of the hot Jupiter in CI Tau

Identification of Young Stellar Variables with KELT for K2. I. Taurus Dippers and Rotators

Simulated mass measurements of the young planet K2-33b

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