Formation of planets via pebble accretion

Master thesis (2021)

Authors

J.J.J. Liu Aerospace Engineering

Contributors

W. van der Wal Physical and Space Geodesy - CEG (supervisor 1)
S.M. Cazaux Astrodynamics & Space Missions - Aerospace Engineering (supervisor 2)
A. Menicucci Space Systems Egineering (supervisor 2)
Yamila Miguel Universiteit Leiden (supervisor 2)
Faculty
Aerospace Engineering
Copyright: © 2021 Jordi Liu
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Published Date

12-04-2021

Language

English

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Faculty

Aerospace Engineering

Abstract

Within a Protoplanetary disk (PPD), planets form from micron sized particles, but what are the processes taken for planet formation? How does the evolution of micron sized particles via settlement and coagulation lead to the gigantic planets as the ones in our Solar System? This thesis explores the planet formation process of pebble accretion which is a planet accretion model involving the accretion of smaller bodies onto larger planetesimals. The evolution of micron sized particles into millimetre – centimetre sized pebbles are discussed. These particles will experience growth via settlement and coagulation, radial drift before acting as reservoir for planet cores to accrete and grow from. From the results, it is found that planet formation via pebble accretion is more efficient in the outer regions of the Solar System, where pebble formation was favoured and resulted in smaller inner planets and larger ice giants.