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Title:
Very Low Density Planets around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event
Authors:
Masuda, Kento
Affiliation:
AA(Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan)
Publication:
The Astrophysical Journal, Volume 783, Issue 1, article id. 53, 8 pp. (2014). (ApJ Homepage)
Publication Date:
03/2014
Origin:
IOP
Astronomy Keywords:
methods: numerical, planets and satellites: formation, planets and satellites: gaseous planets, planets and satellites: individual: Kepler-51 KOI-620 KIC 11773022, planets and satellites: interiors, techniques: photometric
DOI:
10.1088/0004-637X/783/1/53
Bibliographic Code:
2014ApJ...783...53M

Abstract

We present an analysis of the transit timing variations (TTVs) in the multi-transiting planetary system around Kepler-51 (KOI-620). This system consists of two confirmed transiting planets, Kepler-51b (P b = 45.2 days) and Kepler-51c (P c = 85.3 days), and one transiting planet candidate KOI-620.02 (P 02 = 130.2 days), which lie close to a 1: 2: 3 resonance chain. Our analysis shows that their TTVs are consistently explained by the three-planet model, and constrains their masses as M_b = 2.1_{-0.8}^{+1.5} \,M_{\oplus } (Kepler-51b), M c = 4.0 ± 0.4 M (Kepler-51c), and M 02 = 7.6 ± 1.1 M (KOI-620.02), thus confirming KOI-620.02 as a planet in this system. The masses inferred from the TTVs are rather small compared to the planetary radii based on the stellar density and planet-to-star radius ratios determined from the transit light curves. Combining these estimates, we find that all three planets in this system have densities among the lowest determined, ρ p <~ 0.05 g cm-3. With this feature, the Kepler-51 system serves as another example of low-density compact multi-transiting planetary systems. We also identify a curious feature in the archived Kepler light curve during the double transit of Kepler-51b and KOI-620.02, which could be explained by their overlapping on the stellar disk (a planet-planet eclipse). If this is really the case, the sky-plane inclination of KOI-620.02's orbit relative to that of Kepler-51b is given by \Delta \Omega = -25.3_{-6.8}^{+6.2}\,{deg}, implying significant misalignment of their orbital planes. This interpretation, however, seems unlikely because such an event that is consistent with all of the observations is found to be exceedingly rare.
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