122 research outputs found
Nonlinear Alpha Effect in Dynamo Theory
We extend the standard two-scale theory of the turbulent dynamo coefficient
to include the nonlinear back reaction of the mean field on
the turbulence. We calculate the turbulent emf as a power series in ,
assuming that the base state of the turbulence () is isotropic, and,
for simplicity, that the magnetic diffusivity equals the kinematic viscosity.
The power series converges for all , and for the special case that the
spectrum of the turbulence is sharply peaked in , our result is proportional
to a tabulated function of the magnetic Reynolds number and the ratio
of (in velocity units) to the rms turbulent velocity .
For (linear regime) we recover the results of Steenbeck et al.
(1966) as modified by Pouquet et al. (1976). For , the usual
astrophysical case, starts to decrease at , dropping
like as . Hence for large ,
saturates at , as estimated by Kraichnan (1979), rather than at
, as inferred by Cattaneo and Hughes (1996) from
their numerical simulations at =100. We plan to carry out simulations with
various values of to investigate the discrepency.Comment: 41 pages, 1 Postscript figure, accepted for publication to Ap
Evolution of helicity in NOAA 10923 over three consecutive solar rotations
We have studied the evolution of magnetic helicity and chirality in an active
region over three consecutive solar rotations. The region when it first
appeared was named NOAA10923 and in subsequent rotations it was numbered NOAA
10930, 10935 and 10941. We compare the chirality of these regions at
photospheric, chromospheric and coronal heights. The observations used for
photospheric and chromospheric heights are taken from Solar Vector Magnetograph
(SVM) and H_alpha imaging telescope of Udaipur Solar Observatory (USO),
respectively. We discuss the chirality of the sunspots and associated H_alpha
filaments in these regions. We find that the twistedness of superpenumbral
filaments is maintained in the photospheric transverse field vectors also. We
also compare the chirality at photospheric and chromospheric heights with the
chirality of the associated coronal loops, as observed from the HINODE X-Ray
Telescope.Comment: 8 pages, 4 figure
Current Helicity and Twist as Two Indicators of The Mirror Asymmetry of solar Magnetic Fields
A comparison between the two tracers of magnetic field mirror asymmetry in
solar active regions, twist and current helicity, is presented. It is shown
that for individual active regions these tracers do not possess visible
similarity while averaging by time over the solar cycle, or by latitude,
reveals similarities in their behaviour. The main property of the dataset is
anti-symmetry over the solar equator. Considering the evolution of helical
properties over the solar cycle we find signatures of a possible sign change at
the beginning of the cycle, though more systematic observational data are
required for a definite confirmation. We discuss the role of both tracers in
the context of the solar dynamo theory.Comment: 14 pages, 6 figure
Segmentation of Loops from Coronal EUV Images
We present a procedure which extracts bright loop features from solar EUV
images. In terms of image intensities, these features are elongated ridge-like
intensity maxima. To discriminate the maxima, we need information about the
spatial derivatives of the image intensity. Commonly, the derivative estimates
are strongly affected by image noise. We therefore use a regularized estimation
of the derivative which is then used to interpolate a discrete vector field of
ridge points ``ridgels'' which are positioned on the ridge center and have the
intrinsic orientation of the local ridge direction. A scheme is proposed to
connect ridgels to smooth, spline-represented curves which fit the observed
loops. Finally, a half-automated user interface allows one to merge or split,
eliminate or select loop fits obtained form the above procedure. In this paper
we apply our tool to one of the first EUV images observed by the SECCHI
instrument onboard the recently launched STEREO spacecraft. We compare the
extracted loops with projected field lines computed from
almost-simultaneously-taken magnetograms measured by the SOHO/MDI Doppler
imager. The field lines were calculated using a linear force-free field model.
This comparison allows one to verify faint and spurious loop connections
produced by our segmentation tool and it also helps to prove the quality of the
magnetic-field model where well-identified loop structures comply with
field-line projections. We also discuss further potential applications of our
tool such as loop oscillations and stereoscopy.Comment: 13 pages, 9 figures, Solar Physics, online firs
Cross helicity and turbulent magnetic diffusivity in the solar convection zone
In a density-stratified turbulent medium the cross helicity is
considered as a result of the interaction of the velocity fluctuations and a
large-scale magnetic field. By means of a quasilinear theory and by numerical
simulations we find the cross helicity and the mean vertical magnetic field
anti-correlated. In the high-conductivity limit the ratio of the helicity and
the mean magnetic field equals the ratio of the magnetic eddy diffusivity and
the (known) density scale height. The result can be used to predict that the
cross helicity at the solar surface exceeds the value of 1 Gauss km/s. Its sign
is anti-correlated with that of the radial mean magnetic field. Alternatively,
we can use our result to determine the value of the turbulent magnetic
diffusivity from observations of the cross helicity.Comment: 9 pages, 2 figures, submitted to Solar Physic
Helicity at Photospheric and Chromospheric Heights
In the solar atmosphere the twist parameter has the same sign as
magnetic helicity. It has been observed using photospheric vector magnetograms
that negative/positive helicity is dominant in the northern/southern hemisphere
of the Sun. Chromospheric features show dextral/sinistral dominance in the
northern/southern hemisphere and sigmoids observed in X-rays also have a
dominant sense of reverse-S/forward-S in the northern/southern hemisphere. It
is of interest whether individual features have one-to-one correspondence in
terms of helicity at different atmospheric heights. We use UBF \Halpha images
from the Dunn Solar Telescope (DST) and other \Halpha data from Udaipur Solar
Observatory and Big Bear Solar Observatory. Near-simultaneous vector
magnetograms from the DST are used to establish one-to-one correspondence of
helicity at photospheric and chromospheric heights. We plan to extend this
investigation with more data including coronal intensities.Comment: 5 pages, 1 figure, 1 table To appear in "Magnetic Coupling between
the Interior and the Atmosphere of the Sun", eds. S.S. Hasan and R.J. Rutten,
Astrophysics and Space Science Proceedings, Springer-Verlag, Heidelberg,
Berlin, 200
Constraints on the magnitude of alpha in dynamo theory
We consider the backreaction of the magnetic field on the magnetic dynamo
coefficients and the role of boundary conditions in interpreting whether
numerical evidence for suppression is dynamical. If a uniform field in a
periodic box serves as the initial condition for modeling the backreaction on
the turbulent EMF, then the magnitude of the turbulent EMF and thus the dynamo
coefficient \a, have a stringent upper limit that depends on the magnetic
Reynolds number to a power of order -1. This is not a dynamic suppression
but results just because of the imposed boundary conditions. In contrast, when
mean field gradients are allowed within the simulation region, or non-periodic
boundary are used, the upper limit is independent of and takes its
kinematic value. Thus only for simulations of the latter types could a measured
suppression be the result of a dynamic backreaction. This is fundamental for
understanding a long-standing controversy surrounding suppression.
Numerical simulations which do not allow any field gradients and invoke
periodic boundary conditions appear to show a strong suppression (e.g.
Cattaneo & Hughes 1996). Simulations of accretion discs which allow field
gradients and allow free boundary conditions (Brandenburg & Donner 1997)
suggest a dynamo which is not suppressed by a power of . Our
results are consistent with both types of simulations.Comment: LaTex, version in press, Ap
Evolution of turbulent spots in a parallel shear flow
The evolution of turbulent spots in a parallel shear flow is studied by means
of full three-dimensional numerical simulations. The flow is bounded by free
surfaces and driven by a volume force. Three regions in the spanwise spot
cross-section can be identified: a turbulent interior, an interface layer with
prominent streamwise streaks and vortices and a laminar exterior region with a
large scale flow induced by the presence of the spot. The lift-up of streamwise
streaks which is caused by non-normal amplification is clearly detected in the
region adjacent to the spot interface. The spot can be characterized by an
exponentially decaying front that moves with a speed different from that of the
cross-stream outflow or the spanwise phase velocity of the streamwise roll
pattern. Growth of the spots seems to be intimately connected to the large
scale outside flow, for a turbulent ribbon extending across the box in
downstream direction does not show the large scale flow and does not grow.
Quantitatively, the large scale flow induces a linear instability in the
neighborhood of the spot, but the associated front velocity is too small to
explain the spot spreading.Comment: 10 pages, 10 Postscript figure
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