Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Abstract

The migration history of Jupiter in the Sun’s natal disk remains poorly constrained. Here we consider how Jupiter’s migration affects small-body reservoirs and how this constrains its original orbital distance from the Sun. We study the implications of large-scale and inward radial migration of Jupiter for the inner solar system while considering the effects of collisional evolution of planetesimals. We use analytical prescriptions to simulate the growth and migration of Jupiter in the gas disk. We assume the existence of a planetesimal disk inside Jupiter’s initial orbit. This planetesimal disk received an initial total mass and size–frequency distribution (SFD). Planetesimals feel the effects of aerodynamic gas drag and collide with one another, mostly while shepherded by the migrating Jupiter. Our main goal is to measure the amount of mass in planetesimals implanted into the main asteroid belt (MAB) and the SFD of the implanted population. We also monitor the amount of dust produced during planetesimal collisions. We find that the SFD of the planetesimal population implanted into the MAB tends to resemble that of the original planetesimal population interior to Jupiter. We also find that unless very little or no mass existed between 5 au and Jupiter’s original orbit, it would be difficult to reconcile the current low mass of the MAB with the possibility that Jupiter migrated from distances beyond 15 au. This is because the fraction of the original disk mass that gets implanted into the MAB is very large. Finally, we discuss the implications of our results in terms of dust production to the so-called NC–CC isotopic dichotomy.

Breaking Degeneracies in Formation Histories by Measuring Refractory Content in Gas Giants

“…It seems unlikely that the population of close-in giant planets universally begin forming at a few tens of au (a location at which it is difficult to form massive cores) and then migrated all the way to the inner disk. Large-scale migration models tend to overestimate the occurrence rates of hot Jupiters (Ida & Lin 2008;Bitsch et al 2019;Emsenhuber et al 2021) and also disagree with observations of the solar system (Deienno et al 2022). Moreover, radial velocity surveys indicate that giant planet occurrence peaks at intermediate distances (∼1-10 au; Fulton et al 2021).…”

Asymmetry in the number of L4 and L5 Jupiter Trojans driven by jumping Jupiter

“…Although Pirani et al (2019b) proposes that, during the gas-disk phase, Jupiter grew beyond ∼30 AU along with a companion planetary embryo which may generate P-and D-type Jupiter Trojans with the correct inclinations, this scenario seems too exotic. Finally, as we mentioned earlier, a large-scale inward migration of Jupiter may result in having too much mass into the main asteroid belt and hence conflicting with present day observations (Deienno et al 2022).…”

“…It is worth noting that to achieve the observed L4/L5 asymmetry, Jupiter has to migrate inwards more than 3.5 AU. Recent work by Deienno et al (2022), however, shows that such large-scale migration of Jupiter may cause some problems to the inner Solar System, such as the amount of mass implanted into the main belt could be very large and inconsistent with the current low mass of the main belt.…”

Leaky dust traps: How fragmentation impacts dust filtering by planets

“…Only after 7 Myr when the planet already reached a mass of about 200 M ⊕ is the gap deep enough and accretion halted. Allowing the planet to reach these masses at earlier times, however, would not change the dust redistribution since these massive planets are able to scatter planetesimals from the outer disk into the inner disk, which is inconsistent with observations from the meteoritic record at these early times (Deienno et al 2022).…”