TY - JOUR
T1 - Scaling laws for localised states in a nonlocal amplitude equation
AU - Dawes, J.H.P.
AU - Penington, C.J.
PY - 2012
Y1 - 2012
N2 - It is well known that, although a uniform magnetic field inhibits the onset of small amplitude thermal convection in a layer of fluid heated from below, isolated convection cells may persist if the fluid motion within them is sufficiently vigorous to expel magnetic flux. Such fully nonlinear ("convecton") solutions for magnetoconvection have been investigated by several authors. Here we explore a model amplitude equation describing this separation of a fluid layer into a vigorously convecting part and a magnetically-dominated part at rest. Our analysis elucidates the origin of the scaling laws observed numerically to form the boundaries in parameter space of the region of existence of these localised states, and importantly, for the lowest thermal forcing required to sustain them.
AB - It is well known that, although a uniform magnetic field inhibits the onset of small amplitude thermal convection in a layer of fluid heated from below, isolated convection cells may persist if the fluid motion within them is sufficiently vigorous to expel magnetic flux. Such fully nonlinear ("convecton") solutions for magnetoconvection have been investigated by several authors. Here we explore a model amplitude equation describing this separation of a fluid layer into a vigorously convecting part and a magnetically-dominated part at rest. Our analysis elucidates the origin of the scaling laws observed numerically to form the boundaries in parameter space of the region of existence of these localised states, and importantly, for the lowest thermal forcing required to sustain them.
UR - http://www.scopus.com/inward/record.url?scp=84863822593&partnerID=8YFLogxK
UR - http://dx.doi.org/10.1080/03091929.2011.652956
U2 - 10.1080/03091929.2011.652956
DO - 10.1080/03091929.2011.652956
M3 - Article
SN - 1029-0419
VL - 106
SP - 372
EP - 391
JO - Geophysical and Astrophysical Fluid Dynamics
JF - Geophysical and Astrophysical Fluid Dynamics
IS - 4-5
ER -