{"id":{"repo_id":"cent-lancashire","oai_identifier":"oai:clok.uclan.ac.uk:20511"},"canonical_url":"https://search.dev.ndltd.org/etd/cent-lancashire/oai:clok.uclan.ac.uk:20511","repository":{"repo_id":"cent-lancashire","name":"University of Central Lancashire","base_url":"https://clok.uclan.ac.uk/cgi/oai2"},"display":{"title":"The migration of giant planets in massive protoplanetary discs","abstract":"If giant planets form by disc fragmentation early on during disc evolution, then they interact with the gas in the disc and as a result they will likely migrate, i.e. drift inwards or outwards. This study aims to explore the migration patterns of giant planets in unstable discs using radiative hydrodynamic simulations. More specifically we examine the migration of planets within different mass discs and at different orbital radii. We find that planets initially migrate inwards quickly. They are able to open up a gap and the migration stops and turns to a slow outward migration. Therefore, planets forming early on are able to survive on wide orbits. However, many of these planets accrete enough mass to become brown dwarfs. This could explain the observations of giant planets at wide orbital radii from the host star.","abstract_html":"If giant planets form by disc fragmentation early on during disc evolution, then they interact with the gas in the disc and as a result they will likely migrate, i.e. drift inwards or outwards. This study aims to explore the migration patterns of giant planets in unstable discs using radiative hydrodynamic simulations. More specifically we examine the migration of planets within different mass discs and at different orbital radii. We find that planets initially migrate inwards quickly. They are able to open up a gap and the migration stops and turns to a slow outward migration. Therefore, planets forming early on are able to survive on wide orbits. However, many of these planets accrete enough mass to become brown dwarfs. This could explain the observations of giant planets at wide orbital radii from the host star.","abstract_has_math":false,"creators":["Robinson, Kate"],"institution":"University of Central Lancashire","degree_name":"msc","degree_level":"masters","degree_discipline":null,"degree_department":null,"school":null,"contributors":[],"advisors":[],"committee_chairs":[],"committee_members":[],"year":2016,"date_issued":"2016-07","date_published":"2016-07","updated_at":"2026-07-24T01:36:13Z","subjects":["F510 - Astrophysics"],"languages":["en"],"rights":[],"rights_urls":[],"identifier_entries":[]},"links":{"outbound_url":null,"outbound_label":null,"outbound_source":null},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:creator","label":"Author","values":["Robinson, Kate"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date","label":"Dc Date","values":["2016-07-01"]},{"key":"dc:date.issued","label":"Date","values":["2016-07"]},{"key":"dc:publisher.department","label":"Dc Publisher Department","values":["School of Physical Science and Computing"]},{"key":"dc:publisher.institution","label":"Dc Publisher Institution","values":["University of Central Lancashire"]},{"key":"dc:relation.isreferencedby","label":"Dc Relation Isreferencedby","values":["https://knowledge.lancashire.ac.uk/id/eprint/20511/"]},{"key":"dc:type","label":"Dc Type","values":["Thesis"]},{"key":"dc:type.qualificationlevel","label":"Dc Type Qualificationlevel","values":["masters"]},{"key":"dc:type.qualificationname","label":"Dc Type Qualificationname","values":["msc"]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["F510 - Astrophysics"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["en"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier.uri","label":"Identifier URI","values":["https://knowledge.lancashire.ac.uk/id/eprint/20511/1/20511%20Robinson%20Kate%20Final%20e-Thesis%20%28Master%20Copy%29.pdf","https://knowledge.lancashire.ac.uk/id/eprint/20511/2/20511%20Robinson%20Kate%20e-Thesis%20Submission%20Form.doc"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["If giant planets form by disc fragmentation early on during disc evolution, then they interact with the gas in the disc and as a result they will likely migrate, i.e. drift inwards or outwards. This study aims to explore the migration patterns of giant planets in unstable discs using radiative hydrodynamic simulations. More specifically we examine the migration of planets within different mass discs and at different orbital radii. We find that planets initially migrate inwards quickly. They are able to open up a gap and the migration stops and turns to a slow outward migration. Therefore, planets forming early on are able to survive on wide orbits. However, many of these planets accrete enough mass to become brown dwarfs. This could explain the observations of giant planets at wide orbital radii from the host star."]},{"key":"dc:format","label":"Dc Format","values":["application/pdf","application/msword"]},{"key":"dc:title","label":"Title","values":["The migration of giant planets in massive protoplanetary discs"]}]}],"canonical_facts":{"dc:creator":["Robinson, Kate"],"dc:date":["2016-07-01"],"dc:date.issued":["2016-07"],"dc:description.abstract":["If giant planets form by disc fragmentation early on during disc evolution, then they interact with the gas in the disc and as a result they will likely migrate, i.e. drift inwards or outwards. This study aims to explore the migration patterns of giant planets in unstable discs using radiative hydrodynamic simulations. More specifically we examine the migration of planets within different mass discs and at different orbital radii. We find that planets initially migrate inwards quickly. They are able to open up a gap and the migration stops and turns to a slow outward migration. Therefore, planets forming early on are able to survive on wide orbits. However, many of these planets accrete enough mass to become brown dwarfs. This could explain the observations of giant planets at wide orbital radii from the host star."],"dc:format":["application/pdf","application/msword"],"dc:identifier.uri":["https://knowledge.lancashire.ac.uk/id/eprint/20511/1/20511%20Robinson%20Kate%20Final%20e-Thesis%20%28Master%20Copy%29.pdf","https://knowledge.lancashire.ac.uk/id/eprint/20511/2/20511%20Robinson%20Kate%20e-Thesis%20Submission%20Form.doc"],"dc:language":["en"],"dc:publisher.department":["School of Physical Science and Computing"],"dc:publisher.institution":["University of Central Lancashire"],"dc:relation.isreferencedby":["https://knowledge.lancashire.ac.uk/id/eprint/20511/"],"dc:subject":["F510 - Astrophysics"],"dc:title":["The migration of giant planets in massive protoplanetary discs"],"dc:type":["Thesis"],"dc:type.qualificationlevel":["masters"],"dc:type.qualificationname":["msc"]},"updated_at":"2026-07-24T01:36:13Z"}