Starting in 1995 numerical modeling of the Earth's dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).

The principal dancer of the Montreal-based company La La La Human Steps from 1981 to 1999, Louise Lecavalier was the single most iconic dancer of her generation, elevating the punk ballet art form to new heights. From a distinctly feminist angle, this critical study looks broadly at the figure of the dancer and their contributions to dance aesthetics and cultural politics. Importantly, this book prioritizes the dancer's voice and shines light on the generally unseen labour of (often women) dancers in producing the historical movements of the discipline. From a close examination of La La La Human Steps' and Lecavalier's evolving aesthetic, to a consideration of Lecavalier's public persona as rebel, conduit and saint, this study charts her growth as a dancer and as an icon. With analysis given to her appearance as bodyguard in Kathryn Bigelow's film Strange Days (1995), and her solo piece No No No I'm Not Mary Poppins (1982), Lecavalier’s work and legacy unfurls before the reader, highlighting the often-unrecognised presence of Africanist aesthetics in her company's repertoire. With extra materials, such as images of performance and street photography as well as a letter from the renowned dancer herself, Louise Lecavalier: Labour, Fandom and Cultural Politics is a celebratory and much-needed insight into the artistic motive and dancer's perspective.

Starting in 1995 numerical modeling of the Earth's dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).

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