Change search
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf
Magnetic Fields of Massive Stars
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy.
2010 (English)Independent thesis Basic level (degree of Bachelor), 15 credits / 22,5 HE creditsStudent thesis
Abstract [en]

This paper is an introduction to the subject of magnetic fields on stars, with a focus on hotter stars. Basic astrophysical concepts are explained, including: spectroscopy, stellar classification, general structure and evolution of stars. The Zeeman effect and how absorption line splitting  is used to detect and measure magnetic fields is explained. The properties of a prominent type of magnetic massive star, Ap-stars, are delved into. These stars have very stable, global, roughly dipolar magnetic fields theorized to have been captured during star formation and maintained  throughout their lifetime. Different approaches to making models of the magnetic field of massive stars are explained, in particular the oblique rotator model. Finally, the use of the oblique rotator model is illustrated by finding possible field structures that would reproduce magnetic field observations of the star HD 37776.This paper is an introduction to the subject of magnetic fields on stars, with a focus on hotter stars. Basic astrophysical concepts are explained, including: spectroscopy, stellar classification, general structure and evolution of stars. The Zeeman effect and how absorption line splitting  is used to detect and measure magnetic fields is explained. The properties of a prominent type of magnetic massive star, Ap-stars, are delved into. These stars have very stable, global, roughly dipolar magnetic fields theorized to have been captured during star formation and maintained  throughout their lifetime. Different approaches to making models of the magnetic field of massive stars are explained, in particular the oblique rotator model. Finally, the use of the oblique rotator model is illustrated by finding possible field structures that would reproduce magnetic field observations of the star HD 37776.

Place, publisher, year, edition, pages
2010. , 24 p.
Series
FYSAST
Identifiers
URN: urn:nbn:se:uu:diva-126242OAI: oai:DiVA.org:uu-126242DiVA: diva2:322514
Educational program
Bachelor Programme in Physics
Uppsok
Physics, Chemistry, Mathematics
Supervisors
Examiners
Available from: 2011-07-06 Created: 2010-06-07 Last updated: 2011-07-06Bibliographically approved

Open Access in DiVA

fulltext(1906 kB)537 downloads
File information
File name FULLTEXT01.pdfFile size 1906 kBChecksum SHA-512
3b33d375af25778680596ae0cada28bc9c61b5729dda9e15b02b55a27243f40d3af2e83ba4d9698f34985fb04ca1f545a997e8c29c978937c97430bfe306aef9
Type fulltextMimetype application/pdf

By organisation
Department of Physics and Astronomy

Search outside of DiVA

GoogleGoogle Scholar
Total: 537 downloads
The number of downloads is the sum of all downloads of full texts. It may include eg previous versions that are now no longer available

urn-nbn

Altmetric score

urn-nbn
Total: 479 hits
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf