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How did Jupiter form
| Content Provider | Semantic Scholar |
|---|---|
| Author | Ahlgren, Calle |
| Copyright Year | 2019 |
| Abstract | Two relatively new concepts in planetary science are planetary migration; wherein the planets migrate through the protoplanetary disk as they form, and pebble accretion; wherein the planetesimals which become terrestrial planets and giant planet cores grow through the accretion of small pebbles. Planetary migration has become a generally accepted concept but there is still much to be learned even about how it affected the formation of our own solar system. As such, the goal of this thesis is to add to this knowledge by investigating how far Jupiter might have migrated in the protoplanetary disk surrounding the young Sun. This is done by performing simulations of the growth and migration of planets evolving in a protoplanetary disk. These simulations are carried out using different initial planetesimal parameters in terms of distance from the host star and starting time of the accretion in relation to the lifetime of the protoplanetary disk. The Python code developed for the thesis to perform the simulations does so by numerically integrating the mass and radial distance from the host star of evolving planets according to the Euler method. In the case of the planet mass the integration follows pebble accretion and subsequently gas accretion for such planets that grow massive enough. The integration of the radial distance from the host star follows recent solutions wherein the migration of a gas accreting planet is not tied to the gas accretion rate onto the star as has been previously suggested. From the results of the simulations I find that the migration distance is heavily dependent on the ratio between the gas accretion and pebble accretion rates onto the host star. When using the low value of 0.01 for this ratio in the simulations Jupiter analogues are found to migrate almost 50 AU. By increasing the value to 0.1 on the other hand I find that the migration distance is reduced to less than 10 AU. The simulations in the thesis follow a simplified model of the planet formation process. As such, these results should be seen as a stepping stone towards more accurate results. |
| File Format | PDF HTM / HTML |
| Alternate Webpage(s) | http://lup.lub.lu.se/luur/download?fileOId=8970161&func=downloadFile&recordOId=8970160 |
| Language | English |
| Access Restriction | Open |
| Content Type | Text |
| Resource Type | Article |
