Recent observations have revealed two new classes of planetary orbits .
Rossiter-Mclaughlin ( RM ) measurements have revealed hot Jupiters in high-obliquity orbits .
In addition , direct-imaging has discovered giant planets at large ( \sim 100 AU ) separations via direct-imaging technique .
Simple-minded disk-migration scenarios are inconsistent with the high-inclination ( and even retrograde ) orbits as seen in recent RM measurements .
Furthermore , forming giant planets at large semi-major axis ( a ) may be challenging in the core-accretion paradigm .
We perform many N -body simulations to explore the two above-mentioned orbital architectures .
Planet–planet scattering in a multi-planet system can naturally excite orbital inclinations .
Planets can also get scattered to large distances .
Large- a planetary orbits created from planet–planet scattering are expected to have high eccentricities ( e ) .
Theoretical models predict that the observed long-period planets , such as Fomalhaut-b have moderate e \approx 0.3 .
Interestingly , these are also in systems with disks .
We find that if a massive-enough outer disk is present , a scattered planet may be circularized at large a via dynamical friction from the disk and repeated scattering of the disk particles .