Transition from axi to nonaxisymmetric dynamo modes in spherical convection models of solarlike stars 

Axel Brandenburg Submitted: 20181226 02:55
We seek to understand the transition from nearly axisymmetric configurations at solar rotation rates to nonaxisymmetric configurations for rapid rotation using 3D numerical simulations of turbulent convection and considering rotation rates between 1 and 30 times the solar value. We find a transition from axi to nonaxisymmetric solutions at around 1.8 times the solar rotation rate. This transition coincides with a change in the rotation profile from antisolar to solarlike differential rotation with a faster equator and slow poles. In the solarlike rotation regime, the field configuration consists of an axisymmetric oscillatory field accompanied by an m=1 azimuthal mode (two active longitudes), which also shows temporal variability. At slow (rapid) rotation, the axisymmetric (nonaxisymmetric) mode dominates. The axisymmetric mode produces latitudinal dynamo waves with polarity reversals, while the nonaxisymmetric mode often exhibits a drift in the rotating reference frame and the strength of the active longitudes changes cyclically over time between the different hemispheres. Most of the obtained dynamo solutions exhibit cyclic variability either caused by latitudinal or azimuthal dynamo waves. In an activityperiod diagram, the cycle lengths normalized by the rotation period form two different populations as a function of rotation rate or magnetic activity level. The slowly rotating axisymmetric population lies close to what is called the inactive branch in observations, while the rapidly rotating models are close to the superactive branch with a declining cycle to rotation frequency ratio with increasing rotation rate. We can successfully reproduce the transition from axi to nonaxisymmetric dynamo solutions for high rotation rates, but highresolution simulations are required to limit the effect of rotational quenching of convection at rotation rates above 20 times the solar value.
Authors: Viviani, M., Warnecke, J., Käpylä, M. J., Käpylä, P. J., Olspert, N., ColeKodikara, E. M., Lehtinen, J. J., & Brandenburg, A.
Projects: None

Publication Status: A&A 616, A160 (2018)
Last Modified: 20181226 12:06



Turbulent transport coefficients in spherical wedge dynamo simulations of solarlike stars 

Axel Brandenburg Submitted: 20180311 23:22
Aims: We investigate dynamo action in global compressible solarlike convective dynamos in the framework of meanfield theory.
Methods: We simulate a solartype star in a wedgeshaped spherical shell, where the interplay between convection and rotation selfconsistently drives a largescale dynamo. To analyze the dynamo mechanism we apply the testfield method for azimuthally (φ) averaged fields to determine the 27 turbulent transport coefficients of the electromotive force, of which six are related to the α tensor. This method has previously been used either in simulations in Cartesian coordinates or in the geodynamo context and is applied here for the first time to fully compressible simulations of solarlike dynamos.
Results: We find that the φφcomponent of the α tensor does not follow the profile expected from that of kinetic helicity. The turbulent pumping velocities significantly alter the effective mean flows acting on the magnetic field and therefore challenge the flux transport dynamo concept. All coefficients are significantly affected by dynamically important magnetic fields. Quenching as well as enhancement are being observed. This leads to a modulation of the coefficients with the activity cycle. The temporal variations are found to be comparable to the timeaveraged values and seem to be responsible for a nonlinear feedback on the magnetic field generation. Furthermore, we quantify the validity of the ParkerYoshimura rule for the equatorward propagation of the mean magnetic field in the present case.
Authors: Warnecke, J., Rheinhardt, M., Käpylä, P. J., Käpylä, M. J., & Brandenburg, A.
Projects: None

Publication Status: Astron. Astrophys. 609, A51 (2018)
Last Modified: 20180312 09:45



Spontaneous flux concentrations from the negative effective magnetic pressure instability beneath a radiative stellar surface 

Axel Brandenburg Submitted: 20180203 05:30
Abstract: The formation of sunspots requires the concentration of magnetic flux near the surface. The negative magnetic pressure instability (NEMPI) might be a possible mechanism for accomplishing this, but it has mainly been studied in simple systems using an isothermal equation of state without a natural free surface. We study NEMPI in a stratified Cartesian meanfield model where turbulence effects are parameterized. We use an ideal equation of state and include radiation transport, which establishes selfconsistently a free surface. We use a Kramerstype opacity with adjustable exponents chosen such that the deeper layers are approximately isentropic. No convection is therefore possible in this model, allowing us to study NEMPI with radiation in isolation. We restrict ourselves to twodimensional models. We use artificially enhanced meanfield coefficients to allow NEMPI to develop, making it therefore possible to study the reason why it is much harder to excite in the presence of radiation. NEMPI yields moderately strong magnetic flux concentrations a certain distance beneath the surface where optical depth is unity. The instability is oscillatory and in the form of upward travelling waves. This seems to be a new effect that has not been found in earlier models without radiative transport. The horizontal wavelength is about ten times smaller than what has been found previously in more idealized isothermal models. In our models, NEMPI saturates at field strengths too low to explain sunspots. Furthermore, the structures appear too narrow and too far beneath the surface to cause significant brightness variations at the radiative surface. We speculate that the failure to reproduce effects resembling sunspots may be related to the neglect of convection.
Authors: Perri, B., & Brandenburg, A.
Projects: None

Publication Status: A&A 609, A99 (2018)
Last Modified: 20180205 22:07



Highwavenumber solar fmode strengthening prior to active region formation 

Axel Brandenburg Submitted: 20171021 07:56
We report a systematic strengthening of the local solar surface or fundamental fmode 12 days prior to the emergence of an active region (AR) in the same (corotating) location. Except for a possibly related increase in the kurtosis of the magnetic field, no indication can be seen in the magnetograms at that time. Our study is motivated by earlier numerical findings of Singh et al. (2014) which showed that, in the presence of a nonuniform magnetic field that is concentrated a few scale heights below the surface, the fmode fans out in the diagnostic kω diagram at high wavenumbers. Here we explore this possibility using data from the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory and show for six isolated ARs, 11130, 11158, 11242, 11105, 11072, and 11768, that at large latitudinal wavenumbers (corresponding to horizontal scales of around 3000 km), the fmode displays strengthening about two days prior to AR formation and thus provides a new precursor for AR formation. Furthermore, we study two ARs, 12051 and 11678, apart from a magnetically quiet patch lying next to AR~12529, to demonstrate the challenges in extracting such a precursor signal when a newly forming AR emerges in a patch that lies in close proximity of one or several already existing ARs which are expected to pollute neighboring patches. We then discuss plausible procedures for extracting precursor signals from regions with crowded environments. The idea that the fmode is perturbed days before any visible magnetic activity occurs at the surface can be important in constraining dynamo models aimed at understanding the global magnetic activity of the Sun.
Authors: Singh, N. K., Raichur, H., & Brandenburg, A.
Projects: None

Publication Status: Astrophys. J. 832, 120 (2017)
Last Modified: 20171021 18:40



Stellar mixing length theory with entropy rain 

Axel Brandenburg Submitted: 20161224 07:54
The effects of a nongradient flux term originating from the motion of convective elements with entropy perturbations of either sign are investigated and incorporated into a modified version of stellar mixing length theory (MLT). Such a term, first studied by Deardorff in the meteorological context, might represent the effects of cold intense downdrafts caused by the rapid cooling in the granulation layer at the top of the convection zone of latetype stars. Such intense downdrafts were first seen in the strongly stratified simulations of Stein & Nordlund in the late 1980s. These downdrafts transport heat nonlocally, a phenomenon referred to as entropy rain. Moreover, the Deardorff term can cause upward enthalpy transport even in a weakly Schwarzschildstably stratified layer. In that case, no giant cell convection would be excited. This is interest in view of recent observations, which could be explained if the dominant flow structures were of small scale even at larger depths. To study this possibility, three distinct flow structures are examined: one in which convective structures have similar size and mutual separation at all depths, one in which the separation increases with depth, but their size is still unchanged, and one in which both size and separation increase with depth, which is the standard flow structure. It is concluded that the third possibility with fewer and thicker downdrafts in deeper layers remains most plausible, but it may be unable to explain the suspected absence of largescale flows with speeds and scales expected from MLT.
Authors: Axel Brandenburg
Projects: None

Publication Status: Astrophys. J. 832, 6 (2016)
Last Modified: 20161228 11:41



Bipolar region formation in stratified twolayer turbulence 

Axel Brandenburg Submitted: 20161031 05:48
This work presents an extensive study of the previously discovered formation of bipolar flux concentrations in a twolayer model. We interpret the formation process in terms of negative effective magnetic pressure instability (NEMPI), which is a possible mechanism to explain the origin of sunspots. In our simulations, we use a Cartesian domain of isothermal stratified gas that is divided into two layers. In the lower layer, turbulence is forced with transverse nonhelical random waves, whereas in the upper layer no flow is induced. A weak uniform magnetic field is imposed in the entire domain at all times. In this study we vary the stratification by changing the gravitational acceleration, magnetic Reynolds number, strength of the imposed magnetic field, and size of the domain to investigate their influence on the formation process. Bipolar magnetic structure formation takes place over a large range of parameters. The magnetic structures become more intense for higher stratification until the density contrast becomes around 100 across the turbulent layer. For the Reynolds numbers considered, magnetic flux concentrations are generated at magnetic Prandtl number between 0.1 and 1. The magnetic field in bipolar regions increases with higher imposed field strength until the field becomes comparable to the equipartition field strength of the turbulence. A larger horizontal extent enables the flux concentrations to become stronger and more coherent. The size of the bipolar structures turns out to be independent of the domain size. In the case of bipolar region formation, we find an exponential growth of the largescale magnetic field, which is indicative of a hydromagnetic instability. Additionally, the flux concentrations are correlated with strong largescale downward and converging flows. These findings imply that NEMPI is responsible for magnetic flux concentrations.
Authors: Jörn Warnecke, Illa R. Losada, Axel Brandenburg, Nathan Kleeorin, Igor Rogachevskii
Projects: None

Publication Status: Astron. Astrophys. 589, A125 (2016)
Last Modified: 20161031 14:12



Hydraulic effects in a radiative atmosphere with ionization 

Axel Brandenburg Submitted: 20160519 23:19
In a paper of 1978, Eugene Parker postulated the need for hydraulic downward motion to explain magnetic flux concentrations at the solar surface. A similar process has recently also been seen in simplified (e.g., isothermal) models of flux concentrations from the negative effective magnetic pressure instability. We study the effects of partial ionization near the radiative surface on the formation of such magnetic flux concentrations. We first obtain onedimensional (1D) equilibrium solutions using either a Kramerslike opacity or the H opacity. The resulting atmospheres are then used as initial conditions in twodimensional (2D) models where flows are driven by an imposed gradient force resembling a localized negative pressure in the form of a blob. To isolate the effects of partial ionization and radiation, we ignore turbulence and convection. In 1D models, due to partial ionization, an unstable stratification forms always near the surface. We show that the extrema in the specific entropy profiles correspond to the extrema in degree of ionization. In the 2D models without partial ionization, flux concentrations form close to the height where the blob is placed. In models with partial ionization, such flux concentrations form at the surface much above the blob. This is due to the corresponding unstable layer in specific entropy. With H opacity, flux concentrations are weaker due to the stably stratified deeper parts. We demonstrate that, together with density stratification, the imposed source of negative pressure drives the formation of flux concentrations. We find that the inclusion of partial ionization affects entropy profiles causing the strong flux concentrations to form closer to the surface. We speculate that turbulence is needed to limit the strength of flux concentrations and homogenize the specific entropy to a more nearly marginal stratification.
Authors: Pallavi Bhat, Axel Brandenburg
Projects: None

Publication Status: Astron. Astrophys. 587, A90 (2016)
Last Modified: 20160520 22:55



Magnetic helicity and energy spectra of a solar active region 

Axel Brandenburg Submitted: 20160313 06:49
We adopt an isotropic representation of the Fouriertransformed twopoint correlation tensor of the magnetic field to estimate the magnetic energy and helicity spectra as well as current helicity spectra of two individual active regions (NOAA 11158 and NOAA 11515) and the change of the spectral indices during their development as well as during the solar cycle. The departure of the spectral indices of magnetic energy and current helicity from 5/3 are analyzed, and it is found that it is lower than the spectral index of the magnetic energy spectrum. Furthermore, the fractional magnetic helicity tends to increase when the scale of the energycarrying magnetic structures increases. The magnetic helicity of NOAA 11515 violates the expected hemispheric sign rule, which is interpreted as an effect of enhanced field strengths at scales larger than 3060Mm with opposite signs of helicity. This is consistent with the general cycle dependence, which shows that around the solar maximum the magnetic energy and helicity spectra are steeper, emphasizing the largescale field.
Authors: Zhang, H., Brandenburg, A., & Sokoloff, D. D.
Projects: None

Publication Status: Astrophys. J. 819, 146 (2016)
Last Modified: 20160315 11:25



Intense bipolar structures from stratified helical dynamos 

Axel Brandenburg Submitted: 20160116 06:38
We perform direct numerical simulations of the equations of magnetohydrodynamics with external random forcing and in the presence of gravity. The domain is divided into two parts: a lower layer where the forcing is helical and an upper layer where the helicity of the forcing is zero with a smooth transition in between. At early times, a largescale helical dynamo develops in the bottom layer. At later times the dynamo saturates, but the vertical magnetic field continues to develop and rises to form dynamic bipolar structures at the top, which later disappear and reappear. Some of the structures look similar to δ spots observed in the Sun. This is the first example of magnetic flux concentrations, owing to strong density stratification, from selfconsistent dynamo simulations that generate bipolar, superequipartition strength, magnetic structures whose energy density can exceeds the turbulent kinetic energy by even a factor of ten.
Authors: Dhrubaditya Mitra, A. Brandenburg, N. Kleeorin, I. Rogachevskii
Projects: None

Publication Status: Mon. Not. Roy. Astron. Soc. 445, 761769 (2014)
Last Modified: 20160120 12:26



Magnetic flux concentrations from dynamogenerated fields 

Axel Brandenburg Submitted: 20150727 14:45
The meanfield theory of magnetized stellar convection gives rise to the two possibility of distinct instabilities: the largescale dynamo instability, operating in the bulk of the convection zone, and a negative effective magnetic pressure instability (NEMPI) operating in the strongly stratified surface layers. The latter might be important in connection with magnetic spot formation, but the growth rate of NEMPI is suppressed with increasing rotation rates, although recent direct numerical simulations (DNS) have shown a subsequent increase in the growth rate. We examine quantitatively whether this increase in the growth rate of NEMPI can be explained by an α squared meanfield dynamo, and whether both NEMPI and the dynamo instability can operate at the same time. We use both DNS and meanfield simulations (MFS) to solve the underlying equations numerically either with or without an imposed horizontal field. We use the testfield method to compute relevant dynamo coefficients. DNS show that magnetic flux concentrations are still possible up to rotation rates above which the largescale dynamo effect produces mean magnetic fields. The resulting DNS growth rates are quantitatively well reproduced with MFS. As expected, for weak or vanishing rotation, the growth rate of NEMPI increases with increasing gravity, but there is a correction term for strong gravity and large turbulent magnetic diffusivity. Magnetic flux concentrations are still possible for rotation rates above which dynamo action takes over. For the solar rotation rate, the corresponding turbulent turnover time is about 5 hours, with dynamo action commencing in the layers beneath.
Authors: Sarah Jabbari, Axel Brandenburg, Illa R. Losada, Nathan Kleeorin, Igor Rogachevskii
Projects: EUNIS

Publication Status: Astron. Astrophys. 568, A112 (2014)
Last Modified: 20150729 13:00



Nearpolytropic stellar simulations with a radiative surface 

Axel Brandenburg Submitted: 20141213 13:52
Studies of solar and stellar convection often employ simple polytropic setups using the diffusion approximation instead of solving the proper radiative transfer equation. This allows one to control separately the polytropic index of the hydrostatic reference solution, the temperature contrast between top and bottom, and the Rayleigh and Peclet numbers. We extend such studies by including radiative transfer in the gray approximation using a Kramerslike opacity with freely adjustable coefficients. We study the properties of such models and compare them with results from the diffusion approximation. We use the Pencil Code, which is a highorder finite difference code where radiation is treated using the method of long characteristics. The source function is given by the Planck function. The opacity is written as kappa=kappa_0 rho^a T^b, where b is varied from 3.5 to +5, and kappa_0 is varied by four orders of magnitude. We consider sets of one dimensional models and perform a comparison with the diffusion approximation. Except for the case where b=5, we find onedimensional hydrostatic equilibria with a nearly polytropic stratification and a polytropic index close to n=(3b)/(1+a), covering both convectively stable (n>3/2) and unstable (n<3/2) cases. For b=3 and a=1, the value of n is undefined a priori and the actual value of n depends then on the depth of the domain. For large values of \kappa_0, the thermal adjustment time becomes long, the Peclet and Rayleigh numbers become large, and the temperature contrast increases and is thus no longer an independent input parameter, unless the Stefan Boltzmann constant is considered adjustable. Proper radiative transfer with Kramerslike opacities provides a useful tool for studying stratified layers with a radiative surface in ways that are more physical than what is possible with polytropic models using the diffusion approximation.
Authors: Barekat, A., & Brandenburg, A.
Projects: None

Publication Status: Astron. Astrophys. 571, A68 (2014)
Last Modified: 20141215 14:00



Superflare occurrence and energies on G, K and Mtype dwarfs 

Axel Brandenburg Submitted: 20140925 21:24
Kepler data from G, K and Mtype stars are used to study conditions that lead to superflares with energies above 10^{34} { erg}. From the 117,661 stars included, 380 show superflares with a total of 1690 such events. We study whether parameters, like effective temperature or the rotation rate, have any effect on the superflare occurrence rate or energy. With increasing effective temperature we observe a decrease in the superflare rate, which is analogous to the previous findings of a decrease in dynamo activity with increasing effective temperature. For slowly rotating stars, we find a quadratic increase of the mean occurrence rate with the rotation rate up to a critical point, after which the rate decreases linearly. Motivated by standard dynamo theory, we study the behavior of the relative starspot coverage, approximated as the relative brightness variation. For faster rotating stars, an increased fraction of stars shows higher spot coverage, which leads to higher superflare rates. A turbulent dynamo is used to study the dependence of the Ohmic dissipation as a proxy of the flare energy on the differential rotation or shear rate. The resulting statistics of the dissipation energy as a function of dynamo number is similar to the observed flare statistics as a function of the inverse Rossby number and shows similarly strong fluctuations. This supports the idea that superflares might well be possible for solartype G stars.
Authors: Candelaresi, S., Hillier, A., Maehara, H., Brandenburg, A., & Shibata, K.
Projects: None

Publication Status: Astrophys. J. 792, 67 (2014)
Last Modified: 20140926 10:14



Magnetic Prandtl number dependence of the kinetictomagnetic dissipation ratio 

Axel Brandenburg Submitted: 20140730 00:01
Using direct numerical simulations of threedimensional hydromagnetic turbulence, either with helical or nonhelical forcing, we show that the ratio of kinetictomagnetic energy dissipation always increases with the magnetic Prandtl number, i.e., the ratio of kinematic viscosity to magnetic diffusivity. This dependence can always be approximated by a power law, but the exponent is not the same in all cases. For nonhelical turbulence, the exponent is around 1/3, while for helical turbulence it is between 0.6 and 2/3. In the statistically steady state, the rate of the energy conversion from kinetic into magnetic by the dynamo must be equal to the Joule dissipation rate. We emphasize that for both smallscale and largescale dynamos, the efficiency of energy conversion depends sensitively on the magnetic Prandtl number, and thus on the microphysical dissipation process. To understand this behavior, we also study shell models of turbulence and onedimensional passive and active scalar models. We conclude that the magnetic Prandtl number dependence is qualitatively best reproduced in the onedimensional model as a result of dissipation via localized Alfvén kinks.
Authors: Axel Brandenburg
Projects: None

Publication Status: Astrophys. J. 791, 12 (2014)
Last Modified: 20140730 15:22



Meanfield and direct numerical simulations of magnetic flux concentrations from vertical field 

Axel Brandenburg Submitted: 20140705 20:53
Strongly stratified hydromagnetic turbulence has previously been found to produce magnetic flux concentrations if the domain is large enough compared with the size of turbulent eddies. Meanfield simulations (MFS) using parameterizations of the Reynolds and Maxwell stresses show a negative effective magnetic pressure instability and have been able to reproduce many aspects of direct numerical simulations (DNS) regarding the growth rate of this largescale instability, shape of the resulting magnetic structures, and their height as a function of magnetic field strength. Unlike the case of an imposed horizontal field, for a vertical one, magnetic flux concentrations of equipartition strength with the turbulence can be reached. This results in magnetic spots that are reminiscent of sunspots. Here we want to find out under what conditions magnetic flux concentrations with vertical field occur and what their internal structure is. We use a combination of MFS, DNS, and implicit largeeddy simulations to characterize the resulting magnetic flux concentrations in forced isothermal turbulence with an imposed vertical magnetic field. We confirm earlier results that in the kinematic stage of the largescale instability the horizontal wavelength of structures is about 10 times the density scale height. At later times, even larger structures are being produced in a fashion similar to inverse spectral transfer in helically driven turbulence. Using turbulence simulations, we find that magnetic flux concentrations occur for different values of the Mach number between 0.1 and 0.7. DNS and MFS show magnetic flux tubes with meanfield energies comparable to the turbulent kinetic energy. The resulting vertical magnetic flux tubes are being confined by downflows along the tubes and corresponding inflow from the sides, which keep the field concentrated.
Authors: A. Brandenburg, O. Gressel, S. Jabbari, N. Kleeorin, I. Rogachevskii
Projects: None

Publication Status: Astron. Astrophys. 562, A53 (2014)
Last Modified: 20140706 20:34



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