Models of magnetic field generation in partly stable planetary cores: Applications to Mercury and Saturn

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The Magnetic Field of Mercury (2010, background): “…dynamos can also yield a weak field, and a stable but conductive layer at the top of the core could suppress higher-order terms, so such models are generally consistent with an axisymmetric dipolar field at spacecraft altitudes (Christensen 2006; Wicht et al. 2007; Christensen and Wicht 2008).”
Low‐degree structure in Mercury's planetary magnetic field (2012, background): “[45] One mechanism that appears to account for the observed field invokes a non-convecting layer above a deep dynamo [Christensen, 2006; Christensen and Wicht, 2008].”
The curious case of Mercury's internal structure (2013, background): “…region below a solid or stably strati ﬁ ed layer is that the inner core must be relatively small in order that the convecting region between the inner core and the nonconvecting shallowmost portion of the core will be of suf ﬁ cient thickness [ Christensen , 2006; Christensen and Wicht , 2008].”
MESSENGER Observations of Mercury's Magnetic Field Structure (2012, background): “, 2005; Takahashi and Matsushima, 2006], the presence of stably stratified layer(s) [Christensen, 2006; Christensen and Wicht, 2008; Manglik et al., 2010], or the precipitation of solid iron [Vilim et al.”