Observations of Comet e 1904 (Borrelly)

Aitken, R. G.

doi:10.5479/ads/bib/1904licob.3r.78a

Cited by 7 publications

(8 citation statements)

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“…The Kepler-13 (aka KOI-13, BD+46 2629) system has long been known to be a proper motion binary (Aitken 1904). Szabó et al (2011) determined that it consists of two A-type stars with similar properties (see Table 1), which are separated by 1.12" (Adams et al 2012).…”

Section: The Kepler-13 Systemmentioning

confidence: 99%

A MISALIGNED PROGRADE ORBIT FOR KEPLER-13 Ab VIA DOPPLER TOMOGRAPHY

Johnson

Cochran

Albrecht

et al. 2014

ApJ

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Transiting planets around rapidly rotating stars are not amenable to precise radial velocity observations, such as are used for planet candidate validation, as they have wide, rotationally broadened stellar lines. Such planets can, however, be observed using Doppler tomography, wherein the stellar absorption line profile distortions during transit are spectroscopically resolved. This allows the validation of transiting planet candidates and the measurement of the stellar spin-planetary orbit (mis)alignment, an important statistical probe of planetary migration processes. We present Doppler tomographic observations which provide a direct confirmation of the hot Jupiter Kepler-13 Ab, and also show that the planet has a prograde, misaligned orbit, with λ = 58.6 • ± 2.0 • . Our measured value of the spin-orbit misalignment is in significant disagreement with the value of λ = 23 • ± 4 • previously measured by Barnes et al. (2011) from the gravity-darkened Kepler lightcurve. We also place an upper limit of 0.75M ⊙ (95% confidence) on the mass of Kepler-13 C, the spectroscopic companion to Kepler-13 B, the proper motion companion of the planet host star Kepler-13 A.

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Section: The Kepler-13 Systemmentioning

confidence: 99%

A MISALIGNED PROGRADE ORBIT FOR KEPLER-13 Ab VIA DOPPLER TOMOGRAPHY

Johnson

Cochran

Albrecht

et al. 2014

ApJ

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“…KOI-13 is a hierarchical triple stellar system, where KOI-13A and KOI-13B are a common proper-motion fast-rotating A-type stars (V A = 9.9, V B = 10.2) with ∼1 ′′ .2 angular separation, and KOI-13C is a 0.4-1M ⊙ star on a 65.8 day orbit around KOI-13B (Aitken 1904;Dommanget & Nys 1994;Szabó et al 2011;Santerne et al 2012). KOI-13b is a ∼1.4R Jup planet on a 1.76 day orbit around the system main component KOI-13A (Szabó et al 2011;Barnes et al 2011;Santerne et al 2012;Batalha et al 2013;Shporer et al 2014).…”

Section: Systems Parameters From Literaturementioning

confidence: 99%

“…To estimate the maximum fraction of the reflection/emission amplitude originating from thermal reemission, we follow Cowan & Agol (2011) and derive the no-albedo, noredistribution, effective dayside temperature T ǫ=0 , which translates in the Kepler band to the maximum emission amplitude A ref,ǫ=0 , both listed in Table 3 for the four systems. KOI-13 is a hierarchical triple stellar system, where KOI-13A and KOI-13B are a common proper-motion fast-rotating A-type stars (V A = 9.9, V B = 10.2) with ∼1 ′′ .2 angular separation, and KOI-13C is a 0.4-1M ⊙ star on a 65.8 day orbit around KOI-13B (Aitken 1904;Dommanget & Nys 1994;Szabó et al 2011;Santerne et al 2012). KOI-13b is a ∼1.4R Jup planet on a 1.76 day orbit around the system main component KOI-13A (Szabó et al 2011;Barnes et al 2011;Santerne et al 2012;Batalha et al 2013;Shporer et al 2014).…”

Section: Systems Parameters From Literaturementioning

confidence: 99%

BEER ANALYSIS OFKEPLERANDCoRoTLIGHT CURVES. II. EVIDENCE FOR SUPERROTATION IN THE PHASE CURVES OF THREEKEPLERHOT JUPITERS

Faigler

Mazeh

2015

ApJ

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We analyzed the Kepler light curves of four transiting hot Jupiter systems -KOI-13, HAT-P-7, TrES-2, and Kepler-76, which show BEaming, Ellipsoidal and Reflection (BEER) phase modulations. The mass of the four planets can be estimated from either the beaming or the ellipsoidal amplitude, given the mass and radius of their parent stars. For KOI-13, HAT-P-7, and Kepler-76 we find that the beaming-based planetary mass estimate is larger than the mass estimated from the ellipsoidal amplitude, consistent with previous studies. This apparent discrepancy may be explained by equatorial superrotation of the planet atmosphere, which induces an angle shift of the planet reflection/emission phase modulation, as was suggested for Kepler-76 in the first paper of this series. We propose a modified BEER model that supports superrotation, assuming either a Lambertian or geometric reflection/emission phase function, and provides a photometry-consistent estimate of the planetary mass. Our analysis shows that for Kepler-76 and HAT-P-7, the Lambertian superrotation BEER model is highly preferable over an unshifted null model, while for KOI-13 it is preferable only at a 1.4σ level. For TrES-2 we do not find such preference. For all four systems the Lambertian superrotation model mass estimates are in excellent agreement with the planetary masses derived from, or constrained by, radial velocity measurements. This makes the Lambertian superrotation BEER model a viable tool for estimating the masses of hot Jupiters from photometry alone. We conclude that hot Jupiter superrotation may be a common phenomenon that can be detected in the visual light curves of Kepler.Subject headings: methods: data analysis -planets and satellites: fundamental parameters -planets and satellites: individual (KOI-13b, HAT-P-7b, TrES-2b,

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“…It is a common proper-motion binary with two bright (V A = 9.9 mag and V B = 10.2 mag, Dommanget & Nys 1994) stars angularly separated by ∼1.2 (Aitken 1904). One of these stars hosts a transiting planet candidate, KOI-13.01, orbiting every 1.76 days (Batalha et al 2012).…”

Section: Introductionmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Barros

et al. 2012

A&A

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We report the discovery of a new stellar companion in the KOI-13 system. KOI-13 is composed of two fast-rotating A-type stars of similar magnitude. One of these two stars hosts a transiting planet discovered by Kepler. We obtained new radial velocity measurements using the SOPHIE spectrograph at the Observatoire de Haute-Provence that reveal an additional companion in this system. This companion has a mass of between 0.4 M and 1 M and orbits one of the two main stars with a period of 65.831 ± 0.029 days and an eccentricity of 0.52 ± 0.02. The radial velocities of the two stars are derived using a model of two fast-rotating line profiles. From the residuals, we find a hint of the stellar variations seen in the Kepler light curve, which have an amplitude of about 1.41 km s −1 and a period close to the rotational period. This signal appears to be about three orders of magnitude larger than expected for stellar activity. From the analysis of the residuals, we also put a 3-σ upper limit on the mass of the transiting planet KOI-13.01 of 14.8 M Jup and 9.4 M Jup , depending on which star hosts the transit. We find that this new companion has no significant impact on the photometric determination of the mass of KOI-13.01 but is expected to affect precise infrared photometry. Finally, using dynamical simulations, we infer that the new companion is orbiting around KOI-13B and that the transiting planet candidate is expected to orbit KOI-13A. Thus, the transiting planet candidate KOI-13.01 is orbiting the main component of a hierarchical triple system.

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Observations of Comet e 1904 (Borrelly)

Cited by 7 publications

References 0 publications

A MISALIGNED PROGRADE ORBIT FOR KEPLER-13 Ab VIA DOPPLER TOMOGRAPHY

A MISALIGNED PROGRADE ORBIT FOR KEPLER-13 Ab VIA DOPPLER TOMOGRAPHY

BEER ANALYSIS OFKEPLERANDCoRoTLIGHT CURVES. II. EVIDENCE FOR SUPERROTATION IN THE PHASE CURVES OF THREEKEPLERHOT JUPITERS

SOPHIE velocimetry ofKeplertransit candidates

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