Efficient Geometric Probabilities of Multi-Transiting Exoplanetary Systems From Corbits

Brakensiek, Joshua; Ragozzine, Darin

doi:10.3847/0004-637x/821/1/47

Cited by 69 publications

(64 citation statements)

References 54 publications

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“…First, we generate 10 4 systems randomly oriented in space for each simulated system; planets with impact parameters b < 1 are said to be transiting. We compared this method to Brakensiek & Ragozzine (2016)'s CORBITS and found that it produced consistent results.…”

Section: Comparison To Kepler Samplementioning

confidence: 93%

Forming Diverse Super-Earth Systems In Situ

MacDonald¹,

Dawson²,

Morrison

et al. 2020

ApJ

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Super-Earths and mini-Neptunes exhibit great diversity in their compositional and orbital properties. Their bulk densities span a large range, from those dense enough to be purely rocky to those needing a substantial contribution from volatiles to their volumes. Their orbital configurations range from compact, circular multi-transiting systems like Kepler-11 to systems like our Solar System's terrestrial planets with wider spacings and modest but significant eccentricities and mutual inclinations. Here we investigate whether a continuum of formation conditions resulting from variation in the amount of solids available in the inner disk can account for the diversity of orbital and compositional properties observed for super Earths, including the apparent dichotomy between single transiting and multiple transiting system. We simulate in situ formation of super-Earths via giant impacts and compare to the observed Kepler sample. We find that intrinsic variations among disks in the amount of solids available for in situ formation can account for the orbital and compositional diversity observed among Kepler's transiting planets. Our simulations can account for the planets' distributions of orbital period ratios, transit duration ratios, and transit multiplicity; higher eccentricities for single than multi transiting planets; smaller eccentricities for larger planets; scatter in the mass-radius relation, including lower densities for planets with masses measured with TTVs than RVs; and similarity in planets' sizes and spacings within each system. Our findings support the theory that variation among super-Earth and mini-Neptune properties is primarily locked in by different in situ formation conditions, rather than arising stochastically through subsequent evolution.

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Section: Comparison To Kepler Samplementioning

confidence: 93%

Forming Diverse Super-Earth Systems In Situ

MacDonald¹,

Dawson²,

Morrison

et al. 2020

ApJ

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show abstract

“…Above planet system generating processes assume the planets are randomly paired. In order to better match the observed period ratio (pr; Fabrycky et al 2014;Brakensiek & Ragozzine 2016) and radius ratio (rr) distributions (Ciardi et al 2013;Weiss et al 2018), we further adjust the orbit ratios and rrs of the generated planet systems. Before the adjustment, we first debias the observed pr and rr distributions.…”

Section: Adjusting Period Ratios and Radius Ratiosmentioning

confidence: 99%

“…Before the adjustment, we first debias the observed pr and rr distributions. For each observed adjacent tranet pair, we use the CORBITS algorithms (Brakensiek & Ragozzine 2016) to calculate the probability of detecting the outer tranet given that the inner one is detected. The inverse of the probability is adopted as the weight of the tranet pair.…”

Section: Adjusting Period Ratios and Radius Ratiosmentioning

confidence: 99%

Occurrence and Architecture of Kepler Planetary Systems as Functions of Stellar Mass and Effective Temperature

Jun

Xie

Zhou

2020

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The Kepler mission has discovered thousands of exoplanets around various stars with different spectral types (M, K, G, and F) and thus different masses and effective temperatures. Previous studies have shown that the planet occurrence rate, in terms of the average number of planets per star, drops with increasing stellar effective temperature (T eff ). In this paper, with the final Kepler Data Release (DR25) catalog, we revisit the relation between stellar effective temperature (as well as mass) and planet occurrence, but in terms of the fraction of stars with planets and the number of planets per planetary system (i.e., planet multiplicity). We find that both the fraction of stars with planets and planet multiplicity decrease with increasing stellar temperature and mass. Specifically, about 75% late-type stars (T eff < 5000 K) have Kepler -like planets with an average planet multiplicity of ∼2.8, while for early-type stars (T eff > 6500 K), this fraction and the average multiplicity fall down to ∼35% and ∼1.8, respectively. The decreasing trend in the fraction of stars with planets is very significant with ∆AIC> 30, though the trend in planet multiplicity is somewhat tentative with ∆AIC∼ 5. Our results also allow us to derive the dispersion of planetary orbital inclinations in relationship with stellar effective temperature. Interestingly, it is found to be similar to the well-known trend between obliquity and stellar temperature, indicating that the two trends might have a common origin.

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“…We use CORBITS (Brakensiek & Ragozzine 2016) to simulate random observations of all the systems. CORBITS computes the probability that any particular group of planets can be observed to transit in a multiple planet systems.…”

Section: Eccentricities and Inclinations Of Super-earthsmentioning

confidence: 99%

Dynamically Hot Super-Earths from Outer Giant Planet Scattering

Huang

Petrovich

Deibert

2017

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The hundreds of multiple planetary systems discovered by the Kepler mission are typically observed to reside in close-in ( 0.5 AU), low-eccentricity, and low-inclination orbits. We run N-body experiments to study the effect that unstable outer ( 1 AU) giant planets, whose end orbital configurations resemble those in the Radial Velocity population, have on these close-in multiple super-Earth systems. Our experiments show that the giant planets greatly reduce the multiplicity of the inner super-Earths and the surviving population can have large eccentricities (e 0.3) and inclinations (i 20• ) at levels that anti-correlate with multiplicity. Consequently, this model predicts the existence of a population of dynamically hot single-transiting planets with typical eccentricities and inclinations of ∼ 0.1 − 0.5 and ∼ 10• − 40• . We show that these results can explain the following observations: (i) the recent eccentricity measurements of Kepler super-Earths from transit durations; (ii) the tentative observation that single-transiting systems have a wider distribution of stellar obliquity angles compared to the multiple-transiting systems; (iii) the architecture of some eccentric super-Earths discovered by Radial Velocity surveys such as HD 125612c. Future observations from TESS will reveal many more dynamically hot single transiting planets, for which follow up Radial Velocity studies will be able to test our models and see whether they have outer giant planets. Subject headings: planets and satellites: dynamical evolution and stability

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Efficient Geometric Probabilities of Multi-Transiting Exoplanetary Systems From Corbits

Cited by 69 publications

References 54 publications

Forming Diverse Super-Earth Systems In Situ

Forming Diverse Super-Earth Systems In Situ

Occurrence and Architecture of Kepler Planetary Systems as Functions of Stellar Mass and Effective Temperature

Dynamically Hot Super-Earths from Outer Giant Planet Scattering

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