We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

Global Coronal Equilibria with Solar Wind Outflow

Rice, Oliver E. K. and Yeates, Anthony R. (2021) 'Global Coronal Equilibria with Solar Wind Outflow.', The Astrophysical Journal, 923 (1). p. 57.


Given a known radial magnetic field distribution on the Sun’s photospheric surface, there exist wellestablished methods for computing a potential magnetic field in the corona above. Such potential fields are routinely used as input to solar wind models, and to initialize magneto-frictional or full magnetohydrodynamic simulations of the coronal and heliospheric magnetic fields. We describe an improved magnetic field model which calculates a magneto-frictional equilibrium with an imposed solar wind profile (which can be Parker’s solar wind solution, or any reasonable equivalent). These ‘outflow fields’ appear to approximate the real coronal magnetic field more closely than a potential field, take a similar time to compute, and avoid the need to impose an artificial source surface. Thus they provide a practical alternative to the potential field model for initializing time-evolving simulations or modeling the heliospheric magnetic field. We give an open-source Python implementation in spherical coordinates and apply the model to data from Solar Cycle 24. The outflow tends to increase the open magnetic flux compared to the potential field model, reducing the well known discrepancy with in situ observations.

Item Type:Article
Full text:Publisher-imposed embargo
(AM) Accepted Manuscript
File format - PDF
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:© 2021. The American Astronomical Society. All rights reserved.
Date accepted:30 September 2021
Date deposited:04 October 2021
Date of first online publication:10 December 2021
Date first made open access:18 January 2022

Save or Share this output

Look up in GoogleScholar