{"id":{"repo_id":"cent-lancashire","oai_identifier":"oai:clok.uclan.ac.uk:23091"},"canonical_url":"https://search.dev.ndltd.org/etd/cent-lancashire/oai:clok.uclan.ac.uk:23091","repository":{"repo_id":"cent-lancashire","name":"University of Central Lancashire","base_url":"https://clok.uclan.ac.uk/cgi/oai2"},"display":{"title":"Radio Observations of Discs around Young Stellar Objects","abstract":"In this thesis we study the disc surrounding the Young Stellar Object DG Tau B. We present observations at both cm and mm wavelengths using e-MERLIN and the EVLA respectively. We study the cold dust in the disc of DG Tau B by looking at its spectral energy distribution (SED). We also analyse the proper motions of DG Tau B and the classical T Tauri star DG Tau A to determine if they are a binary. We fit a modified blackbody to the DG Tau B SED and model the dust using a temperature of T=9.6±0.6K and a mass of M=0.30±0.03M . We see a radio excess which is found to have a spectral index of α = 1.4 ± 0.2, which is indicative of free-free or synchrotron emission. The emission from DG Tau B at cm wavelengths is studied at two epochs. The jet of DG Tau B is resolved with e-MERLIN in both the 2014 and 2016 data, whilst the disc of DG Tau B is only marginally resolved in 2016. The lack of cm blackbody emission from the DG Tau B disc, and shallow spectral index of the radio excess, may indicate that there are no cm-sized dust grains in the disc of DG Tau B. However, the disc of DG Tau B is resolved at mm wavelengths whilst the jet is not. This could either be attributed to mm-sized dust grains in the disc of DG Tau B or be an indication of the dust temperature in the disc. We study the proper motions of DG Tau A and B and find them to be consistent with each other. This could be explained if they have formed from the same star-forming region. Further investigation would need to be conducted in order to confirm if the two Young Stellar Objects are part of a binary system.","abstract_html":"In this thesis we study the disc surrounding the Young Stellar Object DG Tau B. We present observations at both cm and mm wavelengths using e-MERLIN and the EVLA respectively. We study the cold dust in the disc of DG Tau B by looking at its spectral energy distribution (SED). We also analyse the proper motions of DG Tau B and the classical T Tauri star DG Tau A to determine if they are a binary. We fit a modified blackbody to the DG Tau B SED and model the dust using a temperature of T=9.6±0.6K and a mass of M=0.30±0.03M . We see a radio excess which is found to have a spectral index of α = 1.4 ± 0.2, which is indicative of free-free or synchrotron emission. The emission from DG Tau B at cm wavelengths is studied at two epochs. The jet of DG Tau B is resolved with e-MERLIN in both the 2014 and 2016 data, whilst the disc of DG Tau B is only marginally resolved in 2016. The lack of cm blackbody emission from the DG Tau B disc, and shallow spectral index of the radio excess, may indicate that there are no cm-sized dust grains in the disc of DG Tau B. However, the disc of DG Tau B is resolved at mm wavelengths whilst the jet is not. This could either be attributed to mm-sized dust grains in the disc of DG Tau B or be an indication of the dust temperature in the disc. We study the proper motions of DG Tau A and B and find them to be consistent with each other. This could be explained if they have formed from the same star-forming region. Further investigation would need to be conducted in order to confirm if the two Young Stellar Objects are part of a binary system.","abstract_has_math":false,"creators":["Parker, Raeesa"],"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":2017,"date_issued":"2017-12","date_published":"2017-12","updated_at":"2026-07-24T01:36:23Z","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":["Parker, Raeesa"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date","label":"Dc Date","values":["2017-12-01"]},{"key":"dc:date.issued","label":"Date","values":["2017-12"]},{"key":"dc:publisher.department","label":"Dc Publisher Department","values":["School of Computing and Physical Sciences"]},{"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/23091/"]},{"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/23091/1/23091%20Parker%20Raeesa%20Final%20e-Thesis%20%28Master%20Copy%29.pdf","https://knowledge.lancashire.ac.uk/id/eprint/23091/2/23091%20Parker%20Raeesa%20e-Thesis%20Submission%20Form.doc"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["In this thesis we study the disc surrounding the Young Stellar Object DG Tau B. We present observations at both cm and mm wavelengths using e-MERLIN and the EVLA respectively. We study the cold dust in the disc of DG Tau B by looking at its spectral energy distribution (SED). We also analyse the proper motions of DG Tau B and the classical T Tauri star DG Tau A to determine if they are a binary. We fit a modified blackbody to the DG Tau B SED and model the dust using a temperature of T=9.6±0.6K and a mass of M=0.30±0.03M . We see a radio excess which is found to have a spectral index of α = 1.4 ± 0.2, which is indicative of free-free or synchrotron emission. The emission from DG Tau B at cm wavelengths is studied at two epochs. The jet of DG Tau B is resolved with e-MERLIN in both the 2014 and 2016 data, whilst the disc of DG Tau B is only marginally resolved in 2016. The lack of cm blackbody emission from the DG Tau B disc, and shallow spectral index of the radio excess, may indicate that there are no cm-sized dust grains in the disc of DG Tau B. However, the disc of DG Tau B is resolved at mm wavelengths whilst the jet is not. This could either be attributed to mm-sized dust grains in the disc of DG Tau B or be an indication of the dust temperature in the disc. We study the proper motions of DG Tau A and B and find them to be consistent with each other. This could be explained if they have formed from the same star-forming region. Further investigation would need to be conducted in order to confirm if the two Young Stellar Objects are part of a binary system."]},{"key":"dc:format","label":"Dc Format","values":["application/pdf","application/msword"]},{"key":"dc:title","label":"Title","values":["Radio Observations of Discs around Young Stellar Objects"]}]}],"canonical_facts":{"dc:creator":["Parker, Raeesa"],"dc:date":["2017-12-01"],"dc:date.issued":["2017-12"],"dc:description.abstract":["In this thesis we study the disc surrounding the Young Stellar Object DG Tau B. We present observations at both cm and mm wavelengths using e-MERLIN and the EVLA respectively. We study the cold dust in the disc of DG Tau B by looking at its spectral energy distribution (SED). We also analyse the proper motions of DG Tau B and the classical T Tauri star DG Tau A to determine if they are a binary. We fit a modified blackbody to the DG Tau B SED and model the dust using a temperature of T=9.6±0.6K and a mass of M=0.30±0.03M . We see a radio excess which is found to have a spectral index of α = 1.4 ± 0.2, which is indicative of free-free or synchrotron emission. The emission from DG Tau B at cm wavelengths is studied at two epochs. The jet of DG Tau B is resolved with e-MERLIN in both the 2014 and 2016 data, whilst the disc of DG Tau B is only marginally resolved in 2016. The lack of cm blackbody emission from the DG Tau B disc, and shallow spectral index of the radio excess, may indicate that there are no cm-sized dust grains in the disc of DG Tau B. However, the disc of DG Tau B is resolved at mm wavelengths whilst the jet is not. This could either be attributed to mm-sized dust grains in the disc of DG Tau B or be an indication of the dust temperature in the disc. We study the proper motions of DG Tau A and B and find them to be consistent with each other. This could be explained if they have formed from the same star-forming region. Further investigation would need to be conducted in order to confirm if the two Young Stellar Objects are part of a binary system."],"dc:format":["application/pdf","application/msword"],"dc:identifier.uri":["https://knowledge.lancashire.ac.uk/id/eprint/23091/1/23091%20Parker%20Raeesa%20Final%20e-Thesis%20%28Master%20Copy%29.pdf","https://knowledge.lancashire.ac.uk/id/eprint/23091/2/23091%20Parker%20Raeesa%20e-Thesis%20Submission%20Form.doc"],"dc:language":["en"],"dc:publisher.department":["School of Computing and Physical Sciences"],"dc:publisher.institution":["University of Central Lancashire"],"dc:relation.isreferencedby":["https://knowledge.lancashire.ac.uk/id/eprint/23091/"],"dc:subject":["F510 - Astrophysics"],"dc:title":["Radio Observations of Discs around Young Stellar Objects"],"dc:type":["Thesis"],"dc:type.qualificationlevel":["masters"],"dc:type.qualificationname":["msc"]},"updated_at":"2026-07-24T01:36:23Z"}