Hot Jupiters are a class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods (P<10 days). We can see what the occurrence rate and properties are of hot Jupiters closer to when they formed. MIT Libraries home DSpace@MIT.

From surveys using these two techniques, however, the measured HJ occurrence rates differ by a factor of two or more. For M dwarfs, the percentage of stars with a hot Jupiter is under debate.

When divided into stellar mass bins, we find the occurrence rate to be 0.71 ± 0.31% for G stars, 0.43 ± 0.15% for F stars, and 0.26 ± 0.11% for A stars.

• Studying patterns of planet occurrence informs formation theories ! Many hot Jupiters (HJs) are detected by the Doppler and transit techniques.

View Item . However, the occurrence rate of hot Jupiters differs by a factor of 2-3 between Doppler planet surveys and transit planet surveys. Hot Jupiters are too massive to form in situ because a lack of building materials close to a star. That, too, will help us distinguish between different formation scenarios.

(2009), 16 in Faedi et al.

the abundance of ’Cool Jupiters’ - analogs to the Solar system’s giant planets, Jupiter and Saturn. We also show that (sub)giant contamination in the Kepler sample cannot reconcile the two occurrence calculations. Occurrence Rate [per thousand stars] Using the latest Kepler data, we employ Bayesian statistical methods to measure an overall Hot Jupiter (HJ) occurrence rate of 5.8 ± 0.6 per thousand stars.

We find a net hot Jupiter occurrence rate of 0.41 ± 0.10% within this sample, consistent with the rate measured by Kepler for FGK stars. Theoretical models expect a lower occurrence rate than for larger main sequence stars. Request PDF | The Occurrence Rate of Hot Jupiters in the Kepler Field | We measure the rate of hot Jupiter occurrence in a sample of ~160,000 Kepler targets as a function of stellar mass. Hectochelle Observations Hectochelle is a high-resolution (R ≈ 34,000) single-order, multi-object echelle spectrograph (Szentgyorgyi et al. (2011) Marcy et al.

in the galactic disk for about 165 h. The main scientific goal of the project is the detection of transiting planet

Computing accurate occurrence rates can lend insight into planet-formation and migration-theories. Combined with the observed hot-Jupiter occurrence rate, our results for the survival rate imply that ≲8% (α = 10−3) to ≲43% (α = 10−1) of sun-like stars initially encounter an inwardly migrating hot Jupiter. (2013). From surveys using these two techniques, however, the measured HJ occurrence rates differ by a factor of two or more. We can see what the occurrence rate and properties are of hot Jupiters closer to when they formed. Many hot Jupiters (HJs) are detected by the Doppler and transit techniques. Wide-field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of

(2013) and 21 in Bergfors et al. Using the California Planet Survey sample and the Kepler sample, we investigate the causes for this difference in the HJ occurrence rate.

Observation and Sample 2.1.

That, too, will help us distinguish between different formation scenarios. We find a net hot Jupiter occurrence rate of 0.41 ± 0.10% within this sample, consistent with the rate measured by Kepler for FGK stars.

Using the California Planet Survey sample and the Kepler sample, we investigate the causes for this difference in the HJ occurrence rate. We conclude that other factors, such as binary … DSpace@MIT Home; MIT Open Access Articles We find a net hot Jupiter occurrence rate of 0.41 ± 0.10% within this sample, consistent with the rate measured by Kepler for FGK stars. HJ=Hot Jupiter occurrence rate, P trans=Transit probability • Investigate occurrence rate !

0 5 10 15 HJ Occurrence Rate [per thousand] 0 2000 4000 6000 Frequency 0 5 10 15 Gould et al.

Abstract. Each hot Jupiter candidate was assigned a reliability based on its location in the galactic plane and likelihood of being a false positive. (2005) Wright et al. Each hot Jupiter candidate was assigned a reliability based on its location in the galactic plane and likelihood of being a false positive. focused exclusively on transiting hot Jupiter systems and their sample sizes were small: 14 in Daemgen et al. 2011).It This selection bias fully accounts for the discrepancy in hot Jupiter occurrence rates inferred from these two detection methods.

2. Its membership of The American Astronomical Society (AAS), established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. We look for a deficit of HJs around cool stars with convective envelopes. Winn et … implications of the reported metallicity distribution on the hot Jupiter occurrence rate and possible directions of future studies in Section 6.



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