Systems with tightly-packed inner planets ( STIPs ) are very common . Chatterjee & Tan ( 11 ) proposed Inside-Out Planet Formation ( IOPF ) , an in situ formation theory , to explain these planets .
IOPF involves sequential planet formation from pebble-rich rings that are fed from the outer disk and trapped at the pressure maximum associated with the dead zone inner boundary ( DZIB ) .
Planet masses are set by their ability to open a gap and cause the DZIB to retreat outwards .
We present models for the disk density and temperature structures that are relevant to the conditions of IOPF .
For a wide range of DZIB conditions , we evaluate the gap opening masses of planets in these disks that are expected to lead to truncation of pebble accretion onto the forming planet .
We then consider the evolution of dust and pebbles in the disk , estimating that pebbles typically grow to sizes of a few cm during their radial drift from several tens of AU to the inner , \lesssim 1 \ > AU-scale disk .
A large fraction of the accretion flux of solids is expected to be in such pebbles .
This allows us to estimate the timescales for individual planet formation and entire planetary system formation in the IOPF scenario .
We find that to produce realistic STIPs within reasonable timescales similar to disk lifetimes requires disk accretion rates of \sim 10 ^ { -9 } \ > M _ { \odot } \ > { yr } ^ { -1 } and relatively low viscosity conditions in the DZIB region , i.e. , Shakura-Sunyaev parameter of \alpha \sim 10 ^ { -4 } .