Go to  Advanced Search

Aspects of magnetic fields in the late stages of stellar evolution

Show simple item record

dc.contributor.author Thirumalai, Anand
dc.date.accessioned 2012-10-03T22:43:18Z
dc.date.available 2012-10-03T22:43:18Z
dc.date.copyright 2012 en_US
dc.date.issued 2012-10-03
dc.identifier.uri http://hdl.handle.net/2429/43341
dc.description.abstract We investigate the implications of a magnetic field in the late stages of stellar evolution, in relation to the process of mass-loss via a stellar wind. We develop the very first hybrid magnetohydrodynamic-dust-driven wind model for intermediate-mass Asymptotic Giant Branch (AGB) stars. This model consists of incorporating a canonical Weber-Davis magneto-centrifugal scenario with the effects of radiation pressure on dust grains in the envelope of an AGB star. This results in a dual-fluid description, the solution of which is seen to possess traits of both types of winds. In this context, we additionally investigate the implications of spots on the photosphere that alter the location of dust formation and hence the wind solutions. This model is adapted to tackle the case of the red supergiant Betelgeuse. The underlying motivation is to delineate a new mechanism for solving the problem of transport of stellar material from the photosphere out to the dust formation radius, many stellar radii away. Various dust formation scenarios are investigated and it is concluded that the simplest of such scenarios, with silicate dust forming at a large distance, is the most viable one as well. This theory is also applied to the low-mass end of AGB stars; the star Mira. By applying a modified wind model we solve for a hybrid MHD-dust-driven wind solution and find that the magnetic field required to model the observed wind is about 4 G, well within the range of current estimates for AGB stars. We also formulate a hot-spot model to rationalise dust shells at a distance of several stellar radii. Finally, we study the effects of a strong magnetic field in post-AGB compact objects; magnetised white dwarfs and neutron stars. We develop a fast and efficient solution for Hartree-Fock atoms in strong magnetic fields using pseudospectral methods. The atomic structure package developed for this purpose is seen to be many orders of magnitude faster than finite-element based methods. We also obtain for the first time, estimates for the binding energies of certain low-lying states of the lithium atom, that have not been reported thus far in the literature. en_US
dc.language.iso eng en_US
dc.publisher University of British Columbia en
dc.title Aspects of magnetic fields in the late stages of stellar evolution en_US
dc.type Electronic Thesis or Dissertation en
dc.degree.name Doctor of Philosophy - PhD en_US
dc.degree.discipline Physics en_US
dc.degree.grantor University of British Columbia en
dc.date.graduation 2012-11 en_US
dc.degree.campus UBCV en_US
dc.description.scholarlevel Graduate en


Files in this item

Files Size Format Description   View
ubc_2012_fall_thirumalai_anand.pdf 4.095Mb Adobe Portable Document Format   View/Open
 

This item appears in the following Collection(s)

Show simple item record

All items in cIRcle are protected by copyright, with all rights reserved.

UBC Library
1961 East Mall
Vancouver, B.C.
Canada V6T 1Z1
Tel: 604-822-6375
Fax: 604-822-3893