@misc{9248742,
  abstract     = {{The pebble accretion scenario has been proposed as an alternative to the classical theory of planet formation via planetesimal core accretion. In this alternative scenario, once the rocky cores of planets exceed a certain threshold, the mass evolution of planetary embryos are thought to be driven through the accretion of small aggregates of dust grains, which form in the protoplanetary disk, called pebbles. This theory solves several problems within the classical scenario; primarily, that planets forming via core accretion must accrete mass on a time scale much longer than is feasible, while planets forming via pebble accretion gain masses comparable to those within the solar system, crucially on a timescale falling within the lifetime of the protoplanetary disk. Secondly, while the core accretion scenario accurately describes the masses of some planets within the solar system, the rate of mass accretion drops sharply with stellar distance, necessitating untenable assumptions about the column density of the protoplanetary disk in order to explain the masses of the farther planets such as Uranus and Neptune.
In this project we reproduce a 1D model of planetary formation via pebble accretion. We assume in this model that the pebbles are silicates and investigate their sublimation and survival-rates as they move through the protoplanetary envelope. By making use of a dimensionless filling factor, describing the solid volume fraction of the pebbles, we assume that the corresponding fraction of the volume of these pebbles is taken up by stellar gases within the pores of the mineral. We then use the sublimation temperature of (forsterite) silicates in order to predict the amounts of gas from these inclusions that are deposited into the magma ocean on the surface of the planet. Our goal is to investigate whether this mechanism may be a viable candidate for explaining the discrepancies between the isotopic compositions of four representative noble gas isotopes found within the sun and within the earth’s mantle. The results point to the model overestimating the delivery of the light 22Ne isotope, while under-delivering the three heavier 36Ar, 84Kr and 130Xe isotopes compared to survey measurements of the terrestrial surface and atmospheric inventories. Interpreting the results of the project as a proof-of-concept for the model of gas accretion into the protoplanetary core, the over-delivery of 22Ne shows that even by this simplified model there will likely be a meaningful contribution of gaseous material to the core material within the pebble accretion scenario.}},
  author       = {{Conradzon, Emrik}},
  language     = {{eng}},
  note         = {{Student Paper}},
  title        = {{Investigating the role of porous pebbles as vehicles for gas transport from the protoplanetary disk onto the surface of an accreting planet}},
  year         = {{2026}},
}