Review: R. M. Sainsbury: Reference without Referents

Szabó, Z. G.

doi:10.1093/mind/fzn143

Cited by 27 publications

(66 citation statements)

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“…Because Kepler -13A is part of a binary system (Aitken 1904) that is unresolved in the Kepler data, we must account for the additional flux its companion contributes to the light curve. The reported amount by which the light curve is diluted varies among studies, from 38-48% (Szabó et al 2011;Adams et al 2013;Shporer et al 2014). We use the value from Shporer et al (2014) in our analysis, removing 48% of the light in each SAP file.…”

Section: Companion Flux Contributionmentioning

confidence: 99%

“…While some previous studies have focused on analyzing a single, binned, phase-folded light curve that incorporates data from all available Kepler transit events at their respective times of publication (i.e. Barnes et al 2011;Szabó et al 2011;Esteves et al 2013Esteves et al , 2015Howarth & Morello 2017), by separately analyzing the binned and phase-folded light curves for each quarter we are able to determine any changes in the transit parameters over time. Phase-folding over entire quarters, rather than analyzing individual transit events like Szabó et al (2012) or Masuda (2015), has the benefit of increasing the signal-to-noise ratio of the transits which allows for more precise model fitting while preserving most of the gradual time-dependent variation.…”

Section: Transit Phase-folding and Binningmentioning

confidence: 99%

“…Kepler -13Ab was the first planetary system in which spin-orbit misalignment was identified using transit photometry alone (Szabó et al 2011;Barnes et al 2011). A number of groups have since investigated the transit asymmetries it presents (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…There are a number of important factors to consider when comparing these studies. As highlighted by Howarth & Morello (2017), the effective temperature of Kepler -13A has reported values between 7650-9107 K (Brown et al 2011;Szabó et al 2011;Huber et al 2014;Shporer et al 2014), the lower end of which places the star near the boundary between radiative and convective envelope regimes. This makes it unclear how strongly gravity darkening affects stars like Kepler -13A; for convective envelopes β is theoretically just 0.08 (Lucy 1967).…”

Section: Introductionmentioning

confidence: 99%

“…The intensity of gravity darkening is also influenced by stellar mass: low mass stars show more exaggerated gravity darkening or higher β values (Barnes et al 2011). However, the reported mass of Kepler -13A is also poorly constrained, with values ranging from 1.72-2.47 M (Borucki et al 2011;Szabó et al 2011;Shporer et al 2014;Huber et al 2014). This provides little clarity as to which stellar envelope regime and β value most accurately describe the star.…”

Section: Introductionmentioning

confidence: 99%

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Spin–Orbit Misalignment and Precession in the Kepler-13Ab Planetary System

Herman¹,

Mooij²,

Huang³

et al. 2017

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Gravity darkening induced by rapid stellar rotation provides us with a unique opportunity to characterize the spin-orbit misalignment of a planetary system through analysis of its photometric transit. We use the gravity-darkened transit modeling code simuTrans to reproduce the transit light curve of Kepler -13Ab by separately analyzing phase-folded transits for 12 short-cadence Kepler quarters. We verify the temporal change in impact parameter indicative of spin-orbit precession identified by Szabó et al. (2012) and Masuda (2015), reporting a rate of change db/dt = (−4.1 ± 0.2) × 10 −5 day −1 . We further investigate the effect of light dilution on the fitted impact parameter and find that less than 1% of additional light is sufficient to explain the seasonal variation seen in the Kepler quarter data. We then extend our precession analysis to the phase curve data from which we report a rate of change db/dt = (−3.2 ± 1.3) × 10 −5 day −1 . This value is consistent with that of the transit data at a lower significance and provides the first evidence of spin-orbit precession based solely on the temporal variation of the secondary eclipse.

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Section: Companion Flux Contributionmentioning

confidence: 99%

Section: Transit Phase-folding and Binningmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Spin–Orbit Misalignment and Precession in the Kepler-13Ab Planetary System

Herman¹,

Mooij²,

Huang³

et al. 2017

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Giga-year evolution of Jupiter Trojans and the asymmetry problem

Sisto

Ramos

Beaugé

2014

Icarus

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We present a series of numerical integrations of observed and fictitious Jupiter Trojan asteroids, under the gravitational effects of the four outer planets, for time-spans comparable with the age of the Solar System. From these results we calculate the escape rate from each Lagrange point, and construct dynamical maps of "permanence" time in different regions of the phase space.Fictitious asteroids in L 4 and L 5 show no significant difference, showing almost identical dynamical maps and escape rates. For real Trojans, however, we found that approximately 23% o f the members of the leading swarm escaped after 4.5 Gyrs, while this number increased to 28.3% for L 5 . This implies that the asymmetry between the two populations increases with time, indicating that it may have been smaller at the time of formation/capture of these asteroids. Nevertheless, the difference in chaotic diffusion cannot, in itself, account for the current observed asymmetry (∼ 40%), and must be primarily primordial and characteristic of the capture mechanism of the Trojans.Finally, we calculate new proper elements for all the numbered Trojans using the semi-analytical approach of Beaugé and Roig (2001), and compare the results with the numerical estimations by Brož and Rosehnal (2011). For asteroids that were already numbered in 2011, both methods yield very similar results, while significant differences were found for those bodies that

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Are RRab stars fully radial?

Benkő

Szabo

2013

Proc. IAU

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Abstract. Thanks to the space missions CoRoT and Kepler new oscillation frequencies have been discovered in the Fourier spectra of Blazhko RR Lyrae stars. The period doubling (PD) yields half-integer frequencies between the fundamental mode and its harmonics. In many cases the first and/or second radial overtone frequencies also appear temporally. Some stars show extra frequencies that were identified as potential non-radial modes. We show here that all these frequencies can be explained by pure radial pulsation as linear combinations of the frequencies of radial fundamental and overtone modes. We homogeneously re-analyzed light curves of all the CoRoT and Kepler Blazhko RRab stars in which non-radial mode(s) were reported. We used the CoRoT 150-dayslong data co-added to get 8-min sampling and Kepler 3-years-long long-cadence (30-min sampling) data covering Q1-Q12. The CoRoT white fluxes were cleaned and de-trended. In the case of Kepler targets, we used the raw pixel frames applying our own proper tailor-made apertures for each star and quarter separately (Benkő et al., in preparation). The data were pre-whitened with the main pulsation frequencies and their harmonics, the modulation frequencies and as many modulation side peaks as possible. The resulting Fourier spectra and the frequency solutions from the literature are compared.V1127 Aql (CoRoT 100689962). Our identification of f 0 and f m are the same as in Chadid et al. (2010), but if we assume f = f 2 − f 0 , then f = 2(f 2 − f 0 ), where f 2 = 4.825397 d −1 is the frequency of the radial second overtone with the period ratio of 0.582. This identification eliminates the non-radial mode with its period ratio of 0.696. Poretti et al. (2010) have already noticed that V1127 Aql shows half-integer frequencies. If we accept the PD paradigm , the frequency f m1 can also be interpreted as a linear combination: 1.5f 0 − f . G12 found the following independent frequencies of CoRoT 105288363: f 0 , f m , f s (secondary Blazhko frequency), f 1 , f 2 , first and second radial overtone modes with the period ratios 0.745 and 0.590, respectively, and two non-radial modes, f N = 2.442 d

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Review: R. M. Sainsbury: Reference without Referents

Cited by 27 publications

References 0 publications

Spin–Orbit Misalignment and Precession in the Kepler-13Ab Planetary System

Spin–Orbit Misalignment and Precession in the Kepler-13Ab Planetary System

Giga-year evolution of Jupiter Trojans and the asymmetry problem

Are RRab stars fully radial?

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