TY - JOUR
T1 - Coronal energy release by MHD avalanches: continuous driving
AU - Reid, J.
AU - Hood, A W
AU - Parnell, C. E.
AU - Browning, Philippa
AU - Cargill, PJ
N1 - Funding Information:
Acknowledgements. AWH acknowledges the financial support of STFC through the Consolidated grant, ST/N000609/1, to the University of St Andrews and JR acknowledges the support of the Carnegie Trust for the Universities of Scotland. PKB acknowledges financial support of STFC through consolidated grant ST/P000428/1 at the University of Manchester. This work used the DIRAC 1, UKMHD Consortium machine at the University of St Andrews and the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac. ac.uk). This equipment was funded by a BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/K00087X/1, DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.
Publisher Copyright:
© ESO 2018
PY - 2018/7
Y1 - 2018/7
N2 - Previous work has confirmed the concept of a magnetohydrodynamic (MHD) avalanche in pre-stressed threads within a coronal loop.We undertook a series of full, three-dimensional MHD simulations in order to create three threads by twisting the magnetic field through boundary motions until an instability ensues.We find that, following the original instability, one unstable thread can disrupt itsneighbours with continued driving. A ‘bursty’ heating profile results, with a series of ongoing energy releases, but no evident steady state. For the first time using full MHD, we show that avalanches are a viable mechanism for the storing and release of magnetic energy in the solar corona, as a result of photospheric motions.
AB - Previous work has confirmed the concept of a magnetohydrodynamic (MHD) avalanche in pre-stressed threads within a coronal loop.We undertook a series of full, three-dimensional MHD simulations in order to create three threads by twisting the magnetic field through boundary motions until an instability ensues.We find that, following the original instability, one unstable thread can disrupt itsneighbours with continued driving. A ‘bursty’ heating profile results, with a series of ongoing energy releases, but no evident steady state. For the first time using full MHD, we show that avalanches are a viable mechanism for the storing and release of magnetic energy in the solar corona, as a result of photospheric motions.
KW - Magnetohydrodynamics (MHD)
KW - Methods: numerical
KW - Sun: corona
KW - Sun: magnetic fields
UR - http://www.scopus.com/inward/record.url?scp=85064343830&partnerID=8YFLogxK
UR - http://www.mendeley.com/research/coronal-energy-release-mhd-avalanches-continuous-driving
U2 - 10.1051/0004-6361/201732399
DO - 10.1051/0004-6361/201732399
M3 - Article
SN - 0004-6361
VL - 615
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A84
ER -