Join the disputation
The PhD defence and trial lecture will be 100% in-person. The room opens for participation just before the disputation starts, and closes for new participants approximately 15 minutes after the defence has begun.
Join the trial lecture - 17th of October at 10:15 (Aud. 209, Svein Rosselands Hus)
"Coronal heating"
Conferral summary
P.h.d-graden var en co-tutelle mellom universitetet i Oslo og University of St Andrews i Skottland. I avhandlingen sin har hun studert en metode for å identifisere magnetohydrodynamiske bølger i solatmosfæren. Hun presenterer styrker og svakheter med metoden ved bruk i numeriske simuleringer, og introduserer et konsept for hvordan den kan brukes i observasjoner.
Main research findings:
The Sun has been the object of study and admiration for millennia. Still, to this day, we continue to try to understand its mysteries.
The Sun’s atmosphere is a dynamic and complex system, subject to a range of electromagnetic phenomena. Disturbances in the solar atmosphere creates waves. These waves are called magnetohydrodynamic (MHD) waves and can be found almost everywhere in the solar atmosphere. These play an important part in our aim to better understand the sun.
For example, MHD waves can be used in seismological studies of the sun, helping us to deduce information which we cannot figure out directly from observations. They are also thought to play a key role in solving one of the longest unanswered mysteries in modern astrophysics: The coronal heating problem.
There exist different types of MHD waves, called wave modes, but it is not necessarily clear which wave mode we are looking at. Identifying the wave mode would serve as a valuable tool in both coronal seismology and in solving the coronal heating problem. In my thesis, I investigate one such scheme. I investigate its strength and limitation, and provide a proof-of-concept for how the scheme can be used in observations.