138 research outputs found
Towards a Realistic, Data-Driven Thermodynamic MHD Model of the Global Solar Corona
In this work we describe our implementation of a thermodynamic energy
equation into the global corona model of the Space Weather Modeling Framework
(SWMF), and its development into the new Lower Corona (LC) model. This work
includes the integration of the additional energy transport terms of coronal
heating, electron heat conduction, and optically thin radiative cooling into
the governing magnetohydrodynamic (MHD) energy equation. We examine two
different boundary conditions using this model; one set in the upper transition
region (the Radiative Energy Balance model), as well as a uniform chromospheric
condition where the transition region can be modeled in its entirety. Via
observation synthesis from model results and the subsequent comparison to full
sun extreme ultraviolet (EUV) and soft X-Ray observations of Carrington
Rotation (CR) 1913 centered on Aug 27, 1996, we demonstrate the need for these
additional considerations when using global MHD models to describe the unique
conditions in the low corona. Through multiple simulations we examine ability
of the LC model to asses and discriminate between coronal heating models, and
find that a relative simple empirical heating model is adequate in reproducing
structures observed in the low corona. We show that the interplay between
coronal heating and electron heat conduction provides significant feedback onto
the 3D magnetic topology in the low corona as compared to a potential field
extrapolation, and that this feedback is largely dependent on the amount of
mechanical energy introduced into the corona.Comment: 17 pages, 11 figures, Submitted to ApJ on 12/08/200
The August 24, 2002 Coronal Mass Ejection: When a Western Limb Event Connects to Earth
We discuss how some coronal mass ejections (CMEs) originating from the
western limb of the Sun are associated with space weather effects such as solar
energetic particles (SEPs), shock or geo-effective ejecta at Earth. We focus on
the August 24, 2002 coronal mass ejection, a fast (~ 2000 km/s) eruption
originating from W81. Using a three-dimensional magneto-hydrodynamic simulation
of this ejection with the Space Weather Modeling Framework (SWMF), we show how
a realistic initiation mechanism enables us to study the deflection of the CME
in the corona and the heliosphere. Reconnection of the erupting magnetic field
with that of neighboring streamers and active regions modify the solar
connectivity of the field lines connecting to Earth and can also partly explain
the deflection of the eruption during the first tens of minutes. Comparing the
results at 1 AU of our simulation with observations by the ACE spacecraft, we
find that the simulated shock does not reach Earth, but has a maximum angular
span of about 120, and reaches 35 West of Earth in 58 hours. We
find no significant deflection of the CME and its associated shock wave in the
heliosphere, and we discuss the consequences for the shock angular span.Comment: 7 pages, 4 figures, IAU 257 Symposium Proceeding
Solar-Terrestrial Simulations of CMEs with a Realistic Initiation Mechanism: Case Study for Active Region 10069
Most simulations of coronal mass ejections (CMEs) to date either focus on the
interplanetary propagation of a giant plasma "blob" without paying too much
attention to its origin and to the formation process or they focus on the
complex evolution of the coronal magnetic field due to (sub-)photospheric
motions which result in an eruption. Here, we present global simulations of
CMEs where coronal motions are used to produce a realistic evolution of the
coronal magnetic field and cause an eruption. We focus on active region 10069,
which produced a number of eruptions in late August 2002, including the August
24, 2002 CME - a fast (~2000 km/s) eruption originating from W81-, as well as a
slower eruption on August 22, 2002 (originating from W62). Using a
three-dimensional magneto-hydrodynamic (MHD) simulation of these ejections with
the Space Weather Modeling Framework (SWMF), we show how a realistic initiation
mechanism enables us to study the deflection of the CME in the corona and in
the heliosphere. Reconnection of the erupting magnetic field with that of
neighboring streamers and active regions modify the solar connectivity of the
field lines connecting to Earth and change the expected solar energetic
particle fluxes. Comparing the results at 1 AU of our simulations with in situ
observations by the ACE spacecraft, we propose an alternate solar origin for
the shock wave observed at L1 on August 26.Comment: 4 pages, 2 figures, refereed proceedings for Solar Wind 1
Self-similar solution of fast magnetic reconnection: Semi-analytic study of inflow region
An evolutionary process of the fast magnetic reconnection in ``free space''
which is free from any influence of outer circumstance has been studied
semi-analytically, and a self-similarly expanding solution has been obtained.
The semi-analytic solution is consistent with the results of our numerical
simulations performed in our previous paper (see Nitta et al. 2001). This
semi-analytic study confirms the existence of self-similar growth. On the other
hand, the numerical study by time dependent computer simulation clarifies the
stability of the self-similar growth with respect to any MHD mode. These
results confirm the stable self-similar evolution of the fast magnetic
reconnection system.Comment: 15 pages, 7 figure
Resistive Anomalies at Ferromagnetic Transitions Revisited: the case of SrRuO_3
We show that recent resistivity data on SrRuO_3 for T->T_c are consistent
with conventional theory when corrections to scaling are included and a small
shift in T_c is allowed.Comment: 2 pages, 1 figure; revte
Ideal kink instability of a magnetic loop equilibrium
The force-free coronal loop model by Titov & D\'emoulin (1999} is found to be
unstable with respect to the ideal kink mode, which suggests this instability
as a mechanism for the initiation of flares. The long-wavelength () mode
grows for average twists \Phi\ga3.5\pi (at a loop aspect ratio of
5). The threshold of instability increases with increasing major loop radius,
primarily because the aspect ratio then also increases. Numerically obtained
equilibria at subcritical twist are very close to the approximate analytical
equilibrium; they do not show indications of sigmoidal shape. The growth of
kink perturbations is eventually slowed down by the surrounding potential
field, which varies only slowly with radius in the model. With this field a
global eruption is not obtained in the ideal MHD limit. Kink perturbations with
a rising loop apex lead to the formation of a vertical current sheet below the
apex, which does not occur in the cylindrical approximation.Comment: Astron. Astrophys. Lett., accepte
Numerical Studies of the Solar Energetic Particle Transport and Acceleration
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/76215/1/AIAA-2005-4928-462.pd
Superconductivity in ferromagnetic metals and in compounds without inversion centre
The symmetry properties and the general overview of the superconductivity
theory in the itinerant ferromagnets and in materials without space parity are
presented. The basic notions of unconventional superconductivity are introduced
in broad context of multiband superconductivity which is inherent property of
ferromagnetic metals or metals without centre of inversion.Comment: 38 pages, no figure
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