Recent research highlights

	Large-scale fields from shear-flow turbulence compatible with incoherent alpha-shear dynamo shear-current dynamo not excited shown with test-field method all components of diffusion tensor obtained				Brandenburg, A., Rädler, K.-H., Rheinhardt, M., & Käpylä, P. J.: 2008, ``Magnetic diffusivity tensor and dynamo effects in rotating and shearing turbulence,'' Astrophys. J. 676, 740-751 (arXiv:0710.4059, ADS, PDF) citations 90 on ADS, 97 on Google Scholar
	Kinematic alpha effect in isotropic turbulence simulations test-field method applied to isotropic turbulence shows that turb. diffusion ηt=⅓τu2rms. and τ=(urmskf)-1 to good approximation				Sur, S., Brandenburg, A., & Subramanian, K.: 2008, ``Kinematic alpha effect in isotropic turbulence simulations,'' Monthly Notices Roy. Astron. Soc. 385, L15-L19 (arXiv:0711.3789, ADS, PDF) citations 59 on ADS, 73 on Google Scholar
	Large-scale dynamos in turbulent convection with shear α-Ω type dynamos from convection Strong horizontally averaged fields Horizontal shear: drives magnetic helicity vertically Vertical shear: drives magnetic helicity horizontally Quenching alleviated by normal-field condition				Käpylä, P. J., Korpi, M. J., & Brandenburg, A.: 2008, ``Large-scale dynamos in turbulent convection with shear,'' Astron. Astrophys. 491, 353-362 (arXiv:0806.0375, ADS, PDF) citations 85 on ADS, 98 on Google Scholar
	Cyclic magnetic activity due to turbulent convection in spherical wedge geometry Convectively driven dynamo in spherical wedge produces long cycle periods (∼33 years) equatorward migration of toroidal flux belts Hossenfelder's blog entry about the Sun's butterfly diagram				Käpylä, P. J., Mantere, M. J., & Brandenburg, A.: 2012, ``Cyclic magnetic activity due to turbulent convection in spherical wedge geometry,'' Astrophys. J. Lett. 755, L22 (arXiv:1205.4719, ADS, DOI, PDF) citations 71 on ADS, 60 on Google Scholar
	Detection of negative effective magnetic pressure instability in simulations Conclusively demonstrates negative effective magnetic pressure instability(NEMPI) is caused by magnetic suppression of turbulent pressure reduction is stronger than added explicit pressure argued to be relevant to formation of active regions				Brandenburg, A., Kemel, K., Kleeorin, N., Mitra, D., & Rogachevskii, I.: 2011, ``Detection of negative effective magnetic pressure instability in turbulence simulations,'' Astrophys. J. Lett. 740, L50 (arXiv:1109.1270, ADS, DOI, HTML, PDF) citations 38 on ADS, 39 on Google Scholar