Research highlights and influential papers

→ recent research highlights

	Distributed Solar Dynamo Solar dynamo may not be located in the tachocline Equatorward migration from negative near-surface shear Non-resistively limited saturation through helicity fluxes Bipolar regions formed locally near the surface Tilt depends just on shear, not on helicity Large-scale fields even without helicity, just shear				Brandenburg, A.: 2005, ``The case for a distributed solar dynamo shaped by near-surface shear,'' Astrophys. J. 625, 539-547 (astro-ph/0502275, ADS , PDF) citations 215 on ADS
	Dynamo Review Reviews small scale and large scale dynamos Saturation through magnetic helicity conservation Detailed calculation of transport coefficiens using minimal tau approximation (MTA)				Brandenburg, A., & Subramanian, K.: 2005, ``Astrophysical magnetic fields and nonlinear dynamo theory,'' Phys. Rep. 417, 1-209 (astro-ph/0405052, ADS , PDF) citations 676 on ADS
	Accretion disc turbulence first simulation showing that turbulence can be driven by the Balbus-Hawley (or magnetorotational) instability by a magnetic field that in turn is generated by this very same turbulence establishes self-consistent value for disc viscosity with Shakura-Sunyaev alpha of about 0.01				Brandenburg, A., Nordlund, Å., Stein, R. F., & Torkelsson, U.: 1995, ``Dynamo-generated turbulence and large-scale magnetic fields in a Keplerian shear flow,'' Astrophys. J. 446, 741-754 (ADS , PDF) citations 567 on ADS
	Inverse cascade: resistively slow establishes fundamental connection between inverse cascade in hydromagnetic turbulence and alpha effect in dynamo theory unexpected: inverse cascade operates on resistive timescale has to do with magnetic helicity conservation				Brandenburg, A.: 2001, ``The inverse cascade and nonlinear alpha-effect in simulations of isotropic helical hydromagnetic turbulence,'' Astrophys. J. 550, 824-840 (astro-ph/0006186, ADS , PDF) citations 336 on ADS
	Mixed parity dynamo solutions first simulation showing stable mixed parity solutions of nonlinear dynamo equations relevant for Maunder minima type variations of solar/stellar activity				Brandenburg, A., Krause, F., Meinel, R., Moss, D., & Tuominen, I.: 1989, ``The stability of nonlinear dynamos and the limited role of kinematic growth rates,'' Astron. Astrophys. 213, 411-422 (ADS , PDF) citations 154 on ADS
	Convective Dynamo Simulations with Overshoot it was previously though that magnetic buoyancy removes magnetic flux before the dynamo has a chance to work we find that downward pumping is at least equally strong the dynamo works in the entire convection zone, but pumping concentrates magnetic flux at the bottom of the convection zone relevant to the sun				Nordlund, Å., Brandenburg, A., Jennings, R. L., Rieutord, M., Ruokolainen, J., Stein, R. F., & Tuominen, I.: 1992, ``Dynamo action in stratified convection with overshoot,'' Astrophys. J. 392, 647-692 (ADS , PDF) citations 190 on ADS Brandenburg, A., Jennings, R. L., Nordlund, Å., Rieutord, M., Stein, R. F., & Tuominen, I.: 1996, ``Magnetic structures in a dynamo simulation,'' J. Fluid Mech. 306, 325-352 (ADS , PDF) citations 165 on ADS
	Galactic Magnetism Review reviews observations and theory has now become standard reference				Beck, R., Brandenburg, A., Moss, D., Shukurov, A., & Sokoloff, D.: 1996, ``Galactic Magnetism: Recent Developments and Perspectives,'' Ann. Rev. Astron. Astrophys. 34, 155-206 (ADS , PDF) citations 654 on ADS
	Early Universe magnetic fields First to point out possibility of inverse cascade in early Universe Magnetic fields from electroweak phase transition otherwise small scale Horizon scale ~3 cm, corresponding to ~AU after cosmological expansion Would become ~kpc with inverse cascade				Brandenburg, A., Enqvist, K., & Olesen, P.: 1996, ``Large-scale magnetic fields from hydromagnetic turbulence in the very early universe,'' Phys. Rev. D 54, 1291-1300 (astro-ph/9602031, ADS , PDF) citations 154 on ADS Christensson, M., Hindmarsh, M., & Brandenburg, A.: 2001, ``Inverse cascade in decaying 3D magnetohydrodynamic turbulence,'' Phys. Rev. E 64, 056405, 1-6 (astro-ph/0011321, ADS , PDF) citations 99 on ADS
	SN-driven turbulence first realistic 3-D simulation of supernova-driven multi-phase interstellar medium find segregation into 2 phases: warm/denser and hot/dilute and gives filling factors demonstrates different rms velocities in warm (~10 km/s) and hot (~40 km/s) components				Korpi, M. J., Brandenburg, A., Shukurov, A., Tuominen, I., & Nordlund, Å.: 1999, ``A supernova regulated interstellar medium: simulations of the turbulent multiphase medium,'' Astrophys. J. Lett. 514, L99-L102 (ADS , PDF) citations 132 on ADS
	Nonhelical MHD turbulence Demonstrates Rm^1/2 scaling of growth rate Establishes a k^+3/2 spectrum during kinematic stage Inertial range with k^−3/2 magnetic and kinetic energy spectrum during saturated stage				Haugen, N. E. L., Brandenburg, A., & Dobler, W.: 2004, ``Simulations of nonhelical hydromagnetic turbulence,'' Phys. Rev. E 70, 016308, 1-14 (astro-ph/0307059, ADS , PDF) citations 179 on ADS
	Global simulation of fully convective star 3-D simulation of sphere in a box Demonstrates dynamo action in fully convective star Large scale field dipolar Anti-solar rotation, constant along cylinders				Dobler, W., Stix, M., & Brandenburg, A.: 2006, ``Convection and magnetic field generation in fully convective spheres,'' Astrophys. J. 638, 336-347 (astro-ph/0410645, ADS , PDF) citations 129 on ADS