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Early analyses of exoplanet statistics from the Kepler Mission revealed thata model population of multiple-planet systems with low mutual inclinations(${\sim1^{\circ}-2^{\circ}}$) adequately describes the multiple-transitingsystems but underpredicts the number of single-transiting systems. Thisso-called "Kepler dichotomy" signals the existence of a sub-population ofmulti-planet systems possessing larger mutual inclinations. However, thedetails of these inclinations remain uncertain. In this work, we deriveconstraints on the intrinsic mutual inclination distribution by statisticallyexploiting Transit Duration Variations (TDVs) of the Kepler planet population.When planetary orbits are mutually inclined, planet-planet interactions causeorbital precession, which can lead to detectable long-term changes in transitdurations. These TDV signals are inclination-sensitive and have been detectedfor roughly two dozen Kepler planets. We compare the properties of the Keplerobserved TDV detections to TDV detections of simulated planetary systemsconstructed from two population models with differing assumptions about themutual inclination distribution. We find strong evidence for a continuousdistribution of relatively low mutual inclinations that is well-characterizedby a power law relationship between the median mutual inclination($\tilde{\mu}_{i,n}$) and the intrinsic multiplicity ($n$): $\tilde{\mu}_{i,n}= \tilde{\mu}_{i,5}(n/5)^{\alpha}$, where $\tilde{\mu}_{i,5} =1.10^{+0.15}_{-0.11}$ and $\alpha = -1.73^{+0.09}_{-0.08}$. These resultssuggest that late-stage planet assembly and possibly stellar oblateness are thedominant physical origins for the excitation of Kepler planet mutualinclinations.

Evidence for a Non-Dichotomous Solution to the Kepler Dichotomy: Mutual Inclinations of Kepler Planetary Systems from Transit Duration Variations