Radio Observations of Discs around Young Stellar Objects
type: CreativeWork
description: 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: 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.
author: Parker, Raeesa
language: en
keywords: F510 - Astrophysics
date published: 2017-12
date modified: 2026-07-24T01:36:23Z
provider: University of Central Lancashire
publisher: Networked Digital Library of Theses and Dissertations
type: WebPage
source organization: University of Central Lancashire