Helle Bakke

Doctoral Research Fellow - Rosseland Centre for Solar Physics

Norwegian version of this page

Email helle.bakke@astro.uio.no

Room 213

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Visiting address Sem Sælands vei 13 0371 Oslo

Postal address Postboks 1029 0315 Oslo

Other affiliations Faculty of Mathematics and Natural Sciences (Student)

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Academic interests

Solar corona, solar chromosphere, magnetic reconnection, plasma physics, simulations, observations.

Courses taught

AST3310 – Astrophysical plasma and stellar interiors (teaching assistant)

Background

2013-2017 Physics, astronomy and meteorology (B.Sc., UiO)

2016-2018 Astronomy (M.Sc., UiO)

Tags: Solar Physics, Solar Corona, Solar Chromosphere, Simulations, Observations

Bakke, Helle; Carlsson, Mats; Rouppe van der Voort, Luc; Gudiksen, Boris Vilhelm; Polito, V. & Testa, Paola [Show all 7 contributors for this article] (2022). Chromospheric emission from nanoflare heating in RADYN simulations. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 659. doi: 10.1051/0004-6361/202142842. Full text in Research Archive
Frogner, Lars; Gudiksen, Boris Vilhelm & Bakke, Helle (2020). Accelerated particle beams in a 3D simulation of the quiet Sun. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 643. doi: 10.1051/0004-6361/202038529. Full text in Research Archive Show summary
Context. Observational and theoretical evidence suggest that beams of accelerated particles are produced in flaring events of all sizes in the solar atmosphere, from X-class flares to nanoflares. Current models of these types of particles in flaring loops assume an isolated 1D atmosphere. Aims. A more realistic environment for modelling accelerated particles can be provided by 3D radiative magnetohydrodynamics codes. Here, we present a simple model for particle acceleration and propagation in the context of a 3D simulation of the quiet solar atmosphere, spanning from the convection zone to the corona. We then examine the additional transport of energy introduced by the particle beams. Methods. The locations of particle acceleration associated with magnetic reconnection were identified by detecting changes in magnetic topology. At each location, the parameters of the accelerated particle distribution were estimated from local conditions. The particle distributions were then propagated along the magnetic field, and the energy deposition due to Coulomb collisions with the ambient plasma was computed. Results. We find that particle beams originate in extended acceleration regions that are distributed across the corona. Upon reaching the transition region, they converge and produce strands of intense heating that penetrate the chromosphere. Within these strands, beam heating consistently dominates conductive heating below the bottom of the transition region. This indicates that particle beams qualitatively alter the energy transport even outside of active regions.
Bakke, Helle; Frogner, Lars & Gudiksen, Boris Vilhelm (2018). Non-thermal electrons from solar nanoflares In a 3D radiative MHD simulation. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 620. doi: 10.1051/0004-6361/201834129. Full text in Research Archive

View all works in Cristin

Gudiksen, Boris Vilhelm; Frogner, Lars; Bakke, Helle & Clemmensen, Frederik (2020). Accelerated particles in the solar atmosphere .
Gudiksen, Boris Vilhelm; Frogner, Lars & Bakke, Helle (2020). Accelerated particles in the solar atmosphere.