Very Low Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Ii. A Short-Period Companion Orbiting an F Star With Evidence of a Stellar Tertiary and Significant Mutual Inclination

Fleming, Scott W.; Ge, Jian; Barnes, Rory; Beatty, Thomas G.; Crepp, Justin R.; Lee, Nathan De; Esposito, M.; Femenia, Bruno; Ferreira, Letícia D.; Gary, B. L.; Gaudi, B. Scott; Ghezzi, Luan; Hernández, J. I. González; Hebb, Leslie; Jiang, Peng; Lee, Brian; Nelson, Ben A.; Mello, G. F. Porto de; Shappee, B. J.; Stassun, Keivan G.; Thompson, Todd A.; Tofflemire, Benjamin M.; Wisniewski, John P.; Wood‐Vasey, W. M.; Agol, Eric; Prieto, C. Allende; Bizyaev, Dmitry; Brewington, H.; Cargile, Phillip A.; Coban, L.; Costello, Korena S.; Costa, Luis N. da; Good, Melanie; Hua, Nelson; Kane, Stephen R.; Lander, Gary R.; Liu, Jian; Ma, Bo; Mahadevan, Suvrath; Maia, M. A. G.; Malanushenko, Viktor; Muna, Demitri; Nguyen, Duy Cuong; Oravetz, Daniel; Paegert, Martin; Pan, Kaike; Pepper, Joshua; Rebolo, R.; Roebuck, Eric J.; Santiago, B.; Schneider, Donald P.; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie A.; Vincent, Chelsea; Wan, Xiaoke; Wang, Ji; Weaver, B. A.; Weaver, Gwendolyn M.; Zhao, Bo

doi:10.1088/0004-6256/144/3/72

Cited by 16 publications

(12 citation statements)

References 85 publications

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“…Despite these challenges, the MARVELS DR11 reductions have been used to study low-mass and substellar companions (Fleming et al 2012;Wisniewski et al 2012;Ma et al 2013), brown dwarfs in the "desert" (Lee et al 2011), and exotic orbital systems (Mack et al 2013). Figure 5 shows MARVELS RV measurements of two stars with known exoplanets, showing that MARVELS data are in good agreement with existing orbital models for these systems.…”

Section: Current Status and Remaining Challengesmentioning

confidence: 82%

The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data From SDSS-Iii

Alam

Albareti

Prieto

et al. 2015

ApJS

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Section: Current Status and Remaining Challengesmentioning

confidence: 82%

The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data From SDSS-Iii

Alam

Albareti

Prieto

et al. 2015

ApJS

Self Cite

2,207

1,334

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“…The governing equations are calculated with a 4th order Runge-Kutta integrator (although Euler's method works surprisingly well), with an adaptive timestep determined by the most rapidly evolving parameter. This software package and its variants have been used on a wide range of binary systems, including exoplanets Barnes 2015), binary stars (Gómez Maqueo Chew et al 2012, brown dwarfs (Fleming et al 2012;Ma et al 2013), and exomoons . For the simulations presented below, I used the Runge-Kutta method with a timestep that was 1% of the shortest dynamical time (x/(dx/dt), where x is one of the 6 independent variables), and assumed a planet became tidally locked if its rotation period reached 1% of the equilibrium rotation period.…”

Section: Numerical Methods (Eqtide)mentioning

confidence: 99%

Tidal locking of habitable exoplanets

Barnes

2017

Celest Mech Dyn Astr

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Potentially habitable planets can orbit close enough to their host star that the differential gravity across their diameters can produce an elongated shape. Frictional forces inside the planet prevent the bulges from aligning perfectly with the host star and result in torques that alter the planet's rotational angular momentum. Eventually the tidal torques fix the rotation rate at a specific frequency, a process called tidal locking. Tidally locked planets on circular orbits will rotate synchronously, but those on eccentric orbits will either librate or rotate super-synchronously. Although these features of tidal theory are well known, a systematic survey of the rotational evolution of potentially habitable exoplanets using classic equilibrium tide theories has not been undertaken. I calculate how habitable planets evolve under two commonly used models and find, for example, that one model predicts that the Earth's rotation rate would have synchronized after 4.5 Gyr if its initial rotation period was 3 days, it had no satellites, and it always maintained the modern Earth's tidal properties. Lower mass stellar hosts will induce stronger tidal effects on potentially habitable planets, and tidal locking is possible for most planets in the habitable zones of GKM dwarf stars. For fast-rotating planets, both models predict eccentricity growth and that circularization can only occur once the rotational frequency is similar to the orbital frequency. The orbits of potentially habitable planets of very late M dwarfs ( < ∼ 0.1 M ) are very likely to be circularized within 1 Gyr, and hence, those planets will be synchronous rotators. Proxima b is almost assuredly tidally locked, but its orbit may not have circularized yet, so the planet could be rotating super-synchronously today. The evolution of the isolated and potentially habitable Kepler planet candidates is computed and about half could be tidally locked. Finally, projected TESS planets are simulated over a wide range of assumptions, and the vast majority of potentially habitable cases are found to tidally lock within 1 Gyr. These results suggest Electronic supplementary material The online version of this article

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“…As described in Fleming et al (2012), the best frames are selected via the brightest pixel (BP) method. The frames with the brightest X% of BPs are combined to generate a final image, where X = {1, 5, 15, 30, 50, 80} for TYC 3010.…”

Section: Fastcam Lucky Imagingmentioning

confidence: 99%

A Cautionary Tale: Marvels Brown Dwarf Candidate Reveals Itself to Be a Very Long Period, Highly Eccentric Spectroscopic Stellar Binary

Mack

Deshpande

et al. 2013

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We report the discovery of a highly eccentric, double-lined spectroscopic binary star system (TYC 3010-1494-1), comprising two solar-type stars that we had initially identified as a single star with a brown dwarf companion. At the moderate resolving power of the MARVELS spectrograph and the spectrographs used for subsequent radialvelocity (RV) measurements (R 30,000), this particular stellar binary mimics a single-lined binary with an RV signal that would be induced by a brown dwarf companion (M sin i ∼ 50 M Jup) to a solar-type primary. At least three properties of this system allow it to masquerade as a single star with a very-low-mass companion: its large eccentricity (e ∼ 0.8), its relatively long period (P ∼ 238 days), and the approximately perpendicular orientation of the semi-major axis with respect to the line of sight (ω ∼ 189 •). As a result of these properties, for ∼95% of the orbit the two sets of stellar spectral lines are completely blended, and the RV measurements based on centroiding on the apparently single-lined spectrum is very well fit by an orbit solution indicative of a brown dwarf companion on a more circular orbit (e ∼ 0.3). Only during the ∼5% of the orbit near periastron passage does the true, double-lined nature and large RV amplitude of ∼15 km s −1 reveal itself. The discovery of this binary system is an important lesson for RV surveys searching for substellar companions; at a given resolution and observing cadence, a survey will be susceptible to these kinds of astrophysical false positives for a range of orbital parameters. Finally, for surveys like MARVELS that lack the resolution for a useful line bisector analysis, it is imperative to monitor the peak of the cross-correlation function for suspicious changes in width or shape, so that such false positives can be flagged during the candidate vetting process.

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Very Low Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Ii. A Short-Period Companion Orbiting an F Star With Evidence of a Stellar Tertiary and Significant Mutual Inclination

Cited by 16 publications

References 85 publications

The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data From SDSS-Iii

The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data From SDSS-Iii

Tidal locking of habitable exoplanets

A Cautionary Tale: Marvels Brown Dwarf Candidate Reveals Itself to Be a Very Long Period, Highly Eccentric Spectroscopic Stellar Binary

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