The Mysterious Dimmings of the T Tauri Star V1334 Tau

Rodriguez, Joseph E.; Zhou, George; Cargile, Phillip A.; Stevens, Daniel J.; Osborn, H.; Shappee, B. J.; Reed, Phillip A.; Lund, Michael B.; Relles, Howard M.; Latham, David W.; Eastman, Jason D.; Stassun, Keivan G.; Bieryla, Allyson; Esquerdo, Gilbert A.; Berlind, P.; Calkins, M.; Vanderburg, Andrew; Gaidos, Eric; Ansdell, Megan; Siverd, Robert J.; Beatty, Thomas G.; Kochanek, C. S.; Pepper, Joshua; Gaudi, B. Scott; West, R. G.; Pollacco, D.; James, D. J.; Kuhn, Rudolf B.; Stanek, K. Z.; Holoien, T. W. S.; Prieto, J. L.; Johnson, Samson A.; Sergi, Anthony; McCrady, Nate; Johnson, John Asher; Wright, Jason T.; Wittenmyer, Robert A.; Horner, Jonathan

doi:10.3847/1538-4357/aa5da5

Cited by 23 publications

(17 citation statements)

References 59 publications

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“…We then use MINESweeper, a newly developed Bayesian approach for determining stellar parameters using the newest MESA Isochrones & Stellar Tracks (MIST) evolutionary models (Choi et al 2016;Dotter 2016) to infer probability distribution functions for the age and distance of each cluster member. A detailed description of MINESweeper will be given in Cargile et al (in prep); examples of its use include Rodriguez et al (2017), Temple et al (2017), and Dotter et al (2017). MINESweeper provides full posterior distributions of all predicted stellar parameters from the MIST models, including ages, masses, and radii.…”

Section: Our Bayesian Approach and Resultsmentioning

confidence: 99%

A New Look at an Old Cluster: The Membership, Rotation, and Magnetic Activity of Low-mass Stars in the 1.3 Gyr Old Open Cluster NGC 752

Agüeros

Bowsher

Bochanski

et al. 2018

ApJ

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The nearby open cluster NGC 752 presents a rare opportunity to study stellar properties at ages >1 Gyr. However, constructing a membership catalog for it is challenging; most surveys have been limited to identifying its giants and dwarf members earlier than mid-K. We supplement past membership catalogs with candidates selected with updated photometric and proper-motion criteria, generating a list of 258 members, a >50% increase over previous catalogs. Using a Bayesian framework to fit MESA Isochrones & Stellar Tracks evolutionary models to literature photometry and the Tycho-Gaia Astrometric Solution data available for 59 cluster members, we infer the age of, and distance to, NGC 752: 1.34 ± 0.06 Gyr and 438 +8 −6 pc. We also report the results of our optical monitoring of the cluster using the Palomar Transient Factory. We obtain rotation periods for 12 K and M cluster members, the first periods measured for such low-mass stars with a well-constrained age >1 Gyr. We compare these new periods to data from the younger clusters Praesepe and NGC 6811, and to a theoretical model for angular-momentum loss, to examine stellar spin down for low-mass stars over their first 1.3 Gyr. While on average NGC 752 stars are rotating more slowly than their younger counterparts, the difference is not significant. Finally, we use our spectroscopic observations to measure Hα for cluster stars, finding that members earlier than ≈M2 are magnetically inactive, as expected at this age. Forthcoming Gaia data should solidify and extend the membership of NGC 752 to lower masses, thereby increasing its importance for studies of low-mass stars.

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Section: Our Bayesian Approach and Resultsmentioning

confidence: 99%

A New Look at an Old Cluster: The Membership, Rotation, and Magnetic Activity of Low-mass Stars in the 1.3 Gyr Old Open Cluster NGC 752

Agüeros

Bowsher

Bochanski

et al. 2018

ApJ

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“…Cody et al 2014;Rodriguez et al 2015). These dips can repeat on timescales from days to decades, and can cause eclipses which last for timescales ranging from hours to years (Rodriguez et al 2017). Disk clumps that occult a rotating planet might cause radial velocity signals by introducing asymmetries in the planet's rotation profile.…”

Section: Orbit About the Host Starmentioning

confidence: 99%

Detecting Exomoons via Doppler Monitoring of Directly Imaged Exoplanets

Vanderburg

Rappaport

Mayo

2018

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Recently, Teachey, Kipping, and Schmitt (2018) reported the detection of a candidate exomoon, tentatively designated Kepler-1625b I, around a giant planet in the Kepler field. The candidate exomoon would be about the size and mass of Neptune, considerably larger than any moon in our Solar System, and if confirmed, would be the first in a new class of giant moons or binary planets. Motivated by the large mass ratio in the Kepler-1625b planet and satellite system, we investigate the detectability of similarly massive exomoons around directly imaged exoplanets via Doppler spectroscopy. The candidate moon around Kepler-1625b would induce a radial velocity signal of about 200 m s −1 on its host planet, large enough that similar moons around directly imaged planets orbiting bright, nearby stars might be detected with current or next generation instrumentation. In addition to searching for exomoons, a radial velocity survey of directly imaged planets could reveal the orientations of the planets' spin axes, making it possible to identify Uranus analogs.

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“…This period is consistent with past measurements of the photometric period. In other epochs, including our monitoring in 2014-2015 and the 2008-2014 light curves described by Rodriguez et al (2017b), any modulation from spots is masked by the much stronger variability caused by extinction.…”

Section: Spot Modulation In 2015-2016mentioning

confidence: 99%

Star–Disk Interactions in Multiband Photometric Monitoring of the Classical T Tauri Star GI Tau

Guo

Herczeg

Jose

et al. 2018

ApJ

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The variability of young stellar objects is mostly driven by star-disk interactions. In long-term photometric monitoring of the accreting T Tauri star GI Tau, we detect extinction events with typical depths of DṼ 2.5 mag that last for days to months and often appear to occur stochastically. In 2014-2015, extinctions that repeated with a quasi-period of 21 days over several months are the first empirical evidence of slow warps predicted by magnetohydrodynamic simulations to form at a few stellar radii away from the central star. The reddening is consistent with =  R 3.85 0.5 V and, along with an absence of diffuse interstellar bands, indicates that some dust processing has occurred in the disk. The 2015-2016 multiband light curve includes variations in spot coverage, extinction, and accretion, each of which results in different traces in color-magnitude diagrams. This light curve is initially dominated by a month-long extinction event and a return to the unocculted brightness. The subsequent light curve then features spot modulation with a 7.03 day period, punctuated by brief, randomly spaced extinction events. The accretion rate measured from U-band photometry ranges from´-1.3 10 8 to´-1.1 10 10 M e yr −1 (excluding the highest and lowest 5% of high-and low-accretion rate outliers), with an average of4.7 -10 9 M e yr −1 . A total of 50% of the mass is accreted during bursts of >´-12.8 10 9 M e yr -1, which indicates limitations on analyses of disk evolution using single-epoch accretion rates.

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The Mysterious Dimmings of the T Tauri Star V1334 Tau

Cited by 23 publications

References 59 publications

A New Look at an Old Cluster: The Membership, Rotation, and Magnetic Activity of Low-mass Stars in the 1.3 Gyr Old Open Cluster NGC 752

A New Look at an Old Cluster: The Membership, Rotation, and Magnetic Activity of Low-mass Stars in the 1.3 Gyr Old Open Cluster NGC 752

Detecting Exomoons via Doppler Monitoring of Directly Imaged Exoplanets

Star–Disk Interactions in Multiband Photometric Monitoring of the Classical T Tauri Star GI Tau

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