Mass–orbital tracks of protoplanets starting at M_p = 0.01 M_⊕ and r = [0.2: 20] au, with early-onset growth (t₀ = 0.01 Myr) and v_frag = 10 m s⁻¹, under MHD heating (left) and classical heating (right). The total pebble mass drifting through the snowline at t ≥ t₀ is 400 M_⊕. The characteristic masses in planetary evolution at t = 0.1 Myr are also shown as gray lines. Planets grow through pebble accretion until they reach the isolation mass (M_iso; solid line). When the growth timescale exceeds the migration timescale, migration becomes the dominant process (M_mig; dashed line). Gaps start to open when M_p reaches 2.3M_iso (M_gap; dotted line). Planets grow in a runaway manner when the growth timescale again becomes shorter than the migration timescale (M_RG; dash-dotted line). The points on each mass-orbital track show the elapsed time for every 0.5 Myr. The gray circles show the distribution of confirmed exoplanets orbiting stars with masses in the range of [0.8, 1.2] M_⊙ (NASA Exoplanet Archive 2024). The vertical blue lines show the location of the snowline at t = 0.1 Myr.