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The rapid growth in the number of known exoplanets has revealed the existenceof several distinct planetary populations in the observed mass-period diagram.Two of the most surprising are, (1) the concentration of gas giants around 1AUand (2) the accumulation of a large number of low-mass planets with tightorbits, also known as super-Earths and hot Neptunes. We have recently shownthat protoplanetary disks have multiple planet traps that are characterized byorbital radii in the disks and halt rapid type I planetary migration. Bycoupling planet traps with the standard core accretion scenario, we showed thatone can account for the positions of planets in the mass-period diagram. Inthis paper, we demonstrate quantitatively that most gas giants formed at planettraps tend to end up around 1 AU with most of these being contributed by deadzones and ice lines. In addition, we show that a large fraction of super-Earthsand hot Neptunes are formed as "failed" cores of gas giants - this populationbeing constituted by comparable contributions from dead zone and heattransition traps. Our results are based on the evolution of forming planets inan ensemble of disks where we vary only the lifetimes of disks as well as theirmass accretion rates onto the host star. We show that a statistical treatmentof the evolution of a large population of planetary cores initially caught inplanet traps accounts for the existence of three distinct exoplantarypopulations - the hot Jupiters, the more massive planets at roughly orbitalradii around 1 AU orbital, and the short period SuperEarths and hot Neptunes.There are very few evolutionary tracks that feed into the large orbital radiicharacteristic of the imaged Jovian planet, which agrees with recent surveys.Finally, we find that low-mass planets in tight orbits become the dominantplanetary population for low mass stars ($M_* \le 0.7 M_{\odot}$).

Planetary Populations in the Mass-Period Diagram: A Statistical Treatment of Exoplanet Formation and the Role of Planet Traps