Spin-Orbit Alignment for the Circumbinary Planet Host Kepler-16 A

Winn, Joshua N.; Albrecht, S.; Johnson, John Asher; Torres, Guillermo; Cochran, William D.; Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard; Fischer, Debra A.; Doyle, Laurance R.; Welsh, William F.; Carter, Joshua A.; Fabrycky, Daniel C.; Ragozzine, Darin; Quinn, Samuel N.; Shporer, Avi; Howell, Steve B.; Latham, David W.; Orosz, Jerome A.; Prša, Andrej; Slawson, Robert W.; Borucki, W. J.; Koch, David; Barclay, Thomas; Boss, Alan P.; Christensen‐Dalsgaard, J.; Girouard, Forrest R.; Jenkins, Jon M.; Klaus, Todd C.; Meibom, S.; Morris, Robert; Sasselov, Dimitar; Still, M.; Cleve, Jeffrey Van

doi:10.1088/2041-8205/741/1/l1

Cited by 79 publications

(38 citation statements)

References 43 publications

(52 reference statements)

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“…Contrary to expectations, the low-mass stars in the MEarth system LSPM J1112+7626 (0.39 M and 0.27 M ; Irwin et al 2011) both have inflated radii and are cooler than predicted by theory. The secondary in Kepler-16 (0.20 M ;Doyle et al 2011;Winn et al 2011) is also inflated. Its temperature has not been determined, and the primary is a more massive K star.…”

Section: Discrepancies With Modelsmentioning

confidence: 94%

Fundamental properties of lower main‐sequence stars

Torres

2013

Astron Nachr

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The field of exoplanet research has revitalized interest in M dwarfs, which have become favorite targets of Doppler and transit surveys. Accurate measurements of their basic properties such as masses, radii, and effective temperatures have revealed significant disagreements with predictions from stellar evolution theory in the sense that stars are larger and cooler than expected. These anomalies are believed to be due to high levels of activity in these stars. The evidence for the radius discrepancies has grown over the years as more and more determinations have become available; however, fewer of these studies include accurate determinations of the temperatures. The ubiquitous mass-radius diagrams featured in many new discovery papers are becoming more confusing due to increased scatter, which may be due in part to larger than realized systematic errors affecting many of the published measurements. A discussion of these and other issues is given here from an observer's perspective, along with a summary of theoretical efforts to explain the radius and temperature anomalies.

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Section: Discrepancies With Modelsmentioning

confidence: 94%

Fundamental properties of lower main‐sequence stars

Torres

2013

Astron Nachr

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“…• (Winn et al 2011). Several other circumbinary planets have been found using Kepler data, including the multi-planet Kepler-47 system (Orosz et al 2012).…”

Section: Individual Planets and Planetary Systemsmentioning

confidence: 99%

Advances in exoplanet science from Kepler

Lissauer

Dawson

Tremaine

2014

Nature

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Numerous telescopes and techniques have been used to find and study extrasolar planets, but none has been more successful than NASA's Kepler Space Telescope. Kepler has discovered the majority of known exoplanets, the smallest planets to orbit normal stars, and the worlds most likely to be similar to our home planet. Most importantly, Kepler has provided our first look at typical characteristics of planets and planetary systems for planets with sizes as small as and orbits as large as those of the Earth.Kepler is a 0.95 m aperture space telescope launched by NASA in 2009Koch et al. 2010). Kepler identifies those exoplanets whose orbits happen to appear edge-on by searching for periodic dips caused by planetary transits (partial eclipses) of the stellar discs. Above Earth's atmosphere, and in an Earth-trailing heliocentric orbit away from the glare and thermal variations of low Earth orbit, Kepler monitored the brightness of more than 10 5 stars at 30-minute cadence for four years. Kepler's unique asset is an unprecedented photometric precision of ∼ 30 parts per million (ppm) for 12th magnitude stars with data binned in 6.5 hour intervals (Gilliland et al. 2011). This time interval is used as a benchmark because the Earth takes 13 hours to transit the Sun as viewed by a distant observer in the ecliptic plane, and observers slightly away from the ecliptic view a transit of shorter duration. Such high-precision measurements are only possible in space, where stars do not twinkle, and are required to search for Earth-like worlds because the transit of such a planet across the disc of a Sun-like star blocks only 80 ppm of the stellar flux. For comparison, the transit of a Jupiter-size planet across a similar star blocks 1% of the flux, and this dip is straightforward to detect using ground-based telescopes.Transits of ∼ 3600 planet candidates, the vast majority of which represent true exoplanets as described below, have been identified in the first three years of Kepler data ( Figure 1). The discovery of these worlds, most of which have orbital periods (local "years") shorter than a few Earth months, has greatly expanded the zoo of known exoplanet types. Kepler planets have radii, R p , intermediate between those of Earth and Neptune (1 -3.8 R ⊕ , where R ⊕ = 6371 km is the Earth's radius); planets in this size range are missing from our Solar System. These planets have a wide range of densities Lissauer et al. 2011a;Doyle et al. 2011;Carter et al. 2012;Jontof-Hutter et al. 2014;Marcy et al. 2014), probably because they have atmospheres with a wide range of properties. Nonetheless, theoretical models of their interiors (e.g., Fortney et al. 2007) imply that all of the planets in this class are "gas-poor", that is, less than half -in most cases far less -of their mass consists of hydrogen and helium (H/He). In contrast, H/He make up more than 98% of our Sun's mass as well as substantial majorities of the masses of Jupiter, Saturn, and almost all known giant exoplanets with R p > 9 R ⊕ .Kepler's primary mission is to c...

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“…For transiting exoplanets, on the other hand, the Rossiter-McLaughlin (RM) effect has now been widely exploited (e.g., Queloz et al 2000;Winn et al 2005Winn et al , 2009Winn et al , 2010bWinn et al , 2011Hébrard et al 2008;Triaud et al 2010;Hirano et al 2011;Albrecht et al 2012Albrecht et al , 2013. This technique is sensitive to the angle λ between the sky-projected orbital and spin axes (the projected spin-orbit angle).…”

Section: Introductionmentioning

confidence: 99%

Spin–orbit Alignment of Exoplanet Systems: Ensemble Analysis Using Asteroseismology

Campante

Lund

Kuszlewicz

et al. 2016

ApJ

100

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The angle ψ between a planet's orbital axis and the spin axis of its parent star is an important diagnostic of planet formation, migration, and tidal evolution. We seek empirical constraints on ψ by measuring the stellar inclination i s via asteroseismology for an ensemble of 25 solar-type hosts observed with NASA's Kepler satellite. Our results for i s are consistent with alignment at the 2σ level for all stars in the sample, meaning that the system surrounding the red-giant star Kepler-56 remains as the only unambiguous misaligned multiple-planet system detected to date. The availability of a measurement of the projected spin-orbit angle λ for two of the systems allows us to estimate ψ. We find that the orbit of the hot Jupiter HAT-P-7b is likely to be retrograde ( 116 . 4 14.730.2, whereas that of Kepler-25c seems to be well aligned with the stellar spin axis ( 12 . 6 11.0 6.7While the latter result is in apparent contradiction with a statement made previously in the literature that the multi-transiting system Kepler-25 is misaligned, we show that the results are consistent, given the large associated uncertainties. Finally, we perform a hierarchical Bayesian analysis based on the asteroseismic sample in order to recover the underlying distribution of ψ. The ensemble analysis suggests that the directions of the stellar spin and planetary orbital axes are correlated, as conveyed by a tendency of the host stars to display large values of inclination.

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Spin-Orbit Alignment for the Circumbinary Planet Host Kepler-16 A

Cited by 79 publications

References 43 publications

Fundamental properties of lower main‐sequence stars

Fundamental properties of lower main‐sequence stars

Advances in exoplanet science from Kepler

Spin–orbit Alignment of Exoplanet Systems: Ensemble Analysis Using Asteroseismology

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