Asymmetric Transit Curves as Indication of Orbital Obliquity: Clues From the Late-Type Dwarf Companion in Koi-13

Szabó, Gy. M.; Szabo, Robert M.; Benkő, J. M.; Lehmann, H.; Mező, György; Simon, A. E.; Kővári, Zs.; Hodosán, Gabriella; Regály, Zs.; Kiss, L. L.

doi:10.1088/2041-8205/736/1/l4

Cited by 137 publications

(189 citation statements)

References 30 publications

Supporting

Mentioning

173

Contrasting

Order By: Relevance

“…For the other parameters, we choose uninformative priors. We limit the priors on the planet radius to be less than 2.2 R jup , which is the radius of the biggest planet found to date: KOI-13 (Szabó et al 2011). The exhaustive list of parameters and their priors are reported in Table A.1.…”

Section: The Posterior Distributionmentioning

confidence: 99%

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

Armstrong

Santerne

Veras

et al. 2015

A&A

View full text Add to dashboard Cite

Aims. The K2 mission has recently begun to discover new and diverse planetary systems. In December 2014, Campaign 1 data from the mission was released, providing high-precision photometry for ∼22 000 objects over an 80-day timespan. We searched these data with the aim of detecting more important new objects. Methods. Our search through two separate pipelines led to the independent discovery of K2-19b and c, a two-planet system of Neptune-sized objects (4.2 and 7.2 R ⊕ ), orbiting a K dwarf extremely close to the 3:2 mean motion resonance. The two planets each show transits, sometimes simultaneously owing to their proximity to resonance and the alignment of conjunctions. Results. We obtained further ground-based photometry of the larger planet with the NITES telescope, demonstrating the presence of large transit timing variations (TTVs), and used the observed TTVs to place mass constraints on the transiting objects under the hypothesis that the objects are near but not in resonance. We then statistically validated the planets through the PASTIS tool, independently of the TTV analysis.

show abstract

Section: The Posterior Distributionmentioning

confidence: 99%

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

Armstrong

Santerne

Veras

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…The same asymmetry is seen in our analysis, resulting in a red noise detection (β ≈ 1.40). Furthermore, the Kepler aperture contains a second star contributing about 45% of the observed flux (Szabó et al 2011), which we take into account in our modeling. We argue that the asymmetry introduced by gravitational darkening is on the order of 10 −4 and does not severely affect our analysis.…”

Section: Kepler-13mentioning

confidence: 99%

High-precision stellar limb-darkening measurements

Müller

Huber

Czesla

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Planetary transit light curves are influenced by a variety of fundamental parameters, such as the orbital geometry and the surface brightness distribution of the host star. Stellar limb darkening (LD) is therefore among the key parameters of transit modeling. In many applications, LD is presumed to be known and modeled based on synthetic stellar atmospheres. Aims. We measure LD in a sample of 38 Kepler planetary candidate host stars covering effective temperatures between 3000 K and 8900 K with a range of surface gravities from 3.8 to 4.7. In our study we compare our measurements to widely used theoretically predicted quadratic limb-darkening coefficients (LDCs) to check their validity. Methods. We carried out a consistent analysis of a unique stellar sample provided by the Kepler satellite. We performed a Markov chain Monte Carlo (MCMC) modeling of low-noise, short-cadence Kepler transit light curves, which yields reliable error estimates for the LD measurements in spite of the highly correlated parameters encountered in transit modeling. Results. Our study demonstrates that it is impossible to measure accurate LDCs by transit modeling in systems with high impact parameters (b 0.8). For the majority of the remaining sample objects, our measurements agree with the theoretical predictions, considering measurement errors and mutual discrepancies between the theoretical predictions. Nonetheless, theory systematically overpredicts our measurements of the quadratic LDC u 2 by about 0.07. Systematic errors of this order for LDCs would lead to an uncertainty on the order of 1% for the derived planetary parameters. Conclusions. We find that it is adequate to set the commonly used theoretical LDCs as fixed parameters in transit modeling. Furthermore, it is even indispensable to use theoretical LDCs in the case of transiting systems with a high impact parameter, since the host star's LD cannot be determined from their transit light curves.

show abstract

“…(1) Koch et al (2010); (2) Esteves et al (2013); (3) Heng & Demory (2013); (4) Dunham et al (2010); (5) ; (6) Jenkins et al (2010); (7) Fortney et al (2011); (8) Désert et al (2011); (9) Bonomo et al (2012); (10) Santerne et al (2011); (11) Bonomo et al (2013); (12) Szabó et al (2011); (13) Mazeh et al (2012); (14) Christiansen et al (2010); (15) Barclay et al (2012); (16) Alonso et al (2009a); (17) Snellen et al (2009); (18) Alonso et al (2009b).…”

Section: Referencesmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

Deleuil

Almenara

Santerne

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Hot Jupiters are still a fascinating exoplanet population that presents a diversity we are still far from understanding. Highprecision photometric observations combined with radial velocity measurements give us a unique opportunity to constrain their properties better, on both their internal structure and their atmospheric bulk properties. Aims. We initiated a follow-up program of Kepler-released planet candidates with the goal of confirming the planetary nature of a number of them through radial velocity measurements. For those that successfully passed the radial velocity screening, we furthermore performed a detailed exploration of their properties to characterize the systems. As a byproduct, these systematic observations allow us to consolidate the exoplanets' occurrence rate. Methods. We performed a complete analysis of the Kepler-412 system, listed as planet candidate KOI-202 in the Kepler catalog, by combining the Kepler observations from Q1 to Q15, to ground-based spectroscopic observations that allowed us to derive radial velocity measurements, together with the host-star parameters and properties. We also analyzed the light curve to derive the star's rotation period and the phase function of the planet, including the secondary eclipse. Results. We secured the planetary nature of Kepler-412b. We found the planet has a mass of 0.939 ± 0.085 M Jup and a radius of 1.325 ± 0.043 R Jup , which makes it a member of the bloated giant subgroup. It orbits its G3 V host star in 1.72 days. The system has an isochronal age of 5.1 Gyr, consistent with its moderate stellar activity as observed in the Kepler light curve and the rotation of the star of 17.2 ± 1.6 days. From the detected secondary we derived the day-side temperature as a function of the geometric albedo. We estimated that the geometrical albedo A g should be between 0.094 ± 0.015 and 0.013 +0.017 −0.013 and the brightness of the day side 2380 ± 40 K. The measured night-side flux corresponds to a night-side brightness temperature of 2154 ± 83 K, much greater than what is expected for a planet with homogeneous heat redistribution. From the comparison to star and planet evolution models, we found that dissipation should operate in the deep interior of the planet. This modeling also shows that despite its inflated radius, the planet presents a noticeable amount of heavy elements, which accounts for a mass fraction of 0.11 ± 0.04.

show abstract

Asymmetric Transit Curves as Indication of Orbital Obliquity: Clues From the Late-Type Dwarf Companion in Koi-13

Cited by 137 publications

References 30 publications

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

High-precision stellar limb-darkening measurements

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

Contact Info

Product

Resources

About