795 research outputs found
Kinematics and Fine Structure of An Unwinding Polar Jet Observed by SDO/AIA
We present an observational study of the kinematics and fine structure of an
unwinding polar jet, with high temporal and spatial observations taken by the
Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO)
and the Solar Magnetic Activity Research Telescope (SMART). During the rising
period, the shape of the jet resembled a cylinder with helical structures on
the surface, while the mass of the jet was mainly distributed on the cylinder's
shell. In the radial direction, the jet expanded successively at its western
side. The radial expansion presented three distinct phases: the gradually
expanding phase, the fast expanding phase, and the steady phase. Each phase
lasted for about 12 minutes. The angular speed of the unwinding jet and the
twist transferred into the outer corona during the eruption are estimated to be
11.1 \times 10{-3} rad/s (period = 564 s) and 1.17 to 2.55 turns (or 2.34 to
5.1{\pi}) respectively. On the other hand, by calculating the azimuthal
component of the magnetic field in the jet and comparing the free energy stored
in the non-potential magnetic field with the jet's total energy, we find that
the non-potential magnetic field in the jet is enough to supply the energy for
the ejection. These new observational results strongly support the scenario
that the jets are driven by the magnetic twist, which is stored in the twisted
closed field of a bipole, and released through magnetic reconnection between
the bipole and its ambient open field
Accuracy of magnetic energy computations
For magnetically driven events, the magnetic energy of the system is the
prime energy reservoir that fuels the dynamical evolution. In the solar
context, the free energy is one of the main indicators used in space weather
forecasts to predict the eruptivity of active regions. A trustworthy estimation
of the magnetic energy is therefore needed in three-dimensional models of the
solar atmosphere, eg in coronal fields reconstructions or numerical
simulations. The expression of the energy of a system as the sum of its
potential energy and its free energy (Thomson's theorem) is strictly valid when
the magnetic field is exactly solenoidal. For numerical realizations on a
discrete grid, this property may be only approximately fulfilled. We show that
the imperfect solenoidality induces terms in the energy that can lead to
misinterpreting the amount of free energy present in a magnetic configuration.
We consider a decomposition of the energy in solenoidal and nonsolenoidal parts
which allows the unambiguous estimation of the nonsolenoidal contribution to
the energy. We apply this decomposition to six typical cases broadly used in
solar physics. We quantify to what extent the Thomson theorem is not satisfied
when approximately solenoidal fields are used. The quantified errors on energy
vary from negligible to significant errors, depending on the extent of the
nonsolenoidal component. We identify the main source of errors and analyze the
implications of adding a variable amount of divergence to various solenoidal
fields. Finally, we present pathological unphysical situations where the
estimated free energy would appear to be negative, as found in some previous
works, and we identify the source of this error to be the presence of a finite
divergence. We provide a method of quantifying the effect of a finite
divergence in numerical fields, together with detailed diagnostics of its
sources
Photospheric Injection of Magnetic Helicity: Connectivity--based Flux Density Method
Magnetic helicity quantifies how globally sheared and/or twisted is the
magnetic field in a volume. This quantity is believed to play a key role in
solar activity due to its conservation property. Helicity is continuously
injected into the corona during the evolution of active regions (ARs). To
better understand and quantify the role of magnetic helicity in solar activity,
the distribution of magnetic helicity flux in ARs needs to be studied. The
helicity distribution can be computed from the temporal evolution of
photospheric magnetograms of ARs such as the ones provided by SDO/HMI and
Hinode/SOT. Most recent analyses of photospheric helicity flux derive an
helicity flux density proxy based on the relative rotation rate of photospheric
magnetic footpoints. Although this proxy allows a good estimate of the
photospheric helicity flux, it is still not a true helicity flux density
because it does not take into account the connectivity of the magnetic field
lines. For the first time, we implement a helicity density which takes into
account such connectivity. In order to use it for future observational studies,
we test the method and its precision on several types of models involving
different patterns of helicity injection. We also test it on more complex
configurations - from magnetohydrodynamics (MHD) simulations - containing
quasi-separatrix layers. We demonstrate that this connectivity-based helicity
flux density proxy is the best to map the true distribution of photospheric
helicity injection.Comment: Solar Physics, June 2013 (this is the version of the author, a
definitive version is now available in the online journal
Testing predictors of eruptivity using parametric flux emergence simulations
Solar flares and coronal mass ejections (CMEs) are among the most energetic
events in the solar system, impacting the near-Earth environment. Flare
productivity is empirically known to be correlated with the size and complexity
of active regions. Several indicators, based on magnetic-field data from active
regions, have been tested for flare forecasting in recent years. None of these
indicators, or combinations thereof, have yet demonstrated an unambiguous
eruption or flare criterion. Furthermore, numerical simulations have been only
barely used to test the predictability of these parameters. In this context, we
used the 3D parametric MHD numerical simulations of the self-consistent
formation of the flux emergence of a twisted flux tube, inducing the formation
of stable and unstable magnetic flux ropes of Leake (2013, 2014). We use these
numerical simulations to investigate the eruptive signatures observable in
various magnetic scalar parameters and provide highlights on data analysis
processing. Time series of 2D photospheric-like magnetograms are used from
parametric simulations of stable and unstable flux emergence, to compute a list
of about 100 different indicators. This list includes parameters previously
used for operational forecasting, physical parameters used for the first time,
as well as new quantities specifically developed for this purpose. Our results
indicate that only parameters measuring the total non-potentiality of active
regions associated with magnetic inversion line properties, such as the
Falconer parameters , , and , as well as the
new current integral and length parameters, present a
significant ability to distinguish the eruptive cases of the model from the
non-eruptive cases, possibly indicating that they are promising flare and
eruption predictors.Comment: 46 pages, 16 figures, accepted for publication in Space Weather and
Space Climate on June, 8t
X-ray and UV investigation into the magnetic connectivity of a solar flare
We investigate the X-ray and UV emission detected by RHESSI and TRACE in the
context of a solar flare on the 16th November 2002 with the goal of better
understanding the evolution of the flare. We analysed the characteristics of
the X-ray emission in the 12-25 and 25-50 keV energy range while we looked at
the UV emission at 1600 {\AA}. The flare appears to have two distinct phases of
emission separated by a 25-second time delay, with the first phase being
energetically more important. We found good temporal and spatial agreement
between the 25-50 keV X-rays and the most intense areas of the 1600 {\AA} UV
emission. We also observed an extended 100-arcsecond < 25 keV source that
appears coronal in nature and connects two separated UV ribbons later in the
flare. Using the observational properties in X-ray and UV wavelengths, we
propose two explanations for the flare evolution in relation to the spine/fan
magnetic field topology and the accelerated electrons. We find that a
combination of quasi separatrix layer reconnection and null-point reconnection
is required to account for the observed properties of the X-ray and UV
emission.Comment: 8 pages, 8 figures, published in Astronomy and Astrophysic
Temporal Evolution of the Magnetic Topology of the NOAA Active Region 11158
We studied the temporal evolution of the magnetic topology of the active
region (AR) 11158 based on the reconstructed three-dimensional magnetic fields
in the corona. The \nlfff\ extrapolation method was applied to the 12 minutes
cadence data obtained with the \hmi\ (HMI) onboard the \sdo\ (SDO) during five
days. By calculating the squashing degree factor Q in the volume, the derived
quasi-separatrix layers (QSLs) show that this AR has an overall topology,
resulting from a magnetic quadrupole, including an hyperbolic flux tube (HFT)
configuration which is relatively stable at the time scale of the flare ( hours). A strong QSL, which corresponds to some highly sheared arcades
that might be related to the formation of a flux rope, is prominent just before
the M6.6 and X2.2 flares, respectively. These facts indicate the close
relationship between the strong QSL and the high flare productivity of AR
11158. In addition, with a close inspection of the topology, we found a
small-scale HFT which has an inverse tear-drop structure above the
aforementioned QSL before the X2.2 flare. It indicates the existence of
magnetic flux rope at this place. Even though a global configuration (HFT) is
recognized in this AR, it turns out that the large-scale HFT only plays a
secondary role during the eruption. In final, we dismiss a trigger based on the
breakout model and highlight the central role of the flux rope in the related
eruption.Comment: Accepted by Ap
Electric current in flares ribbons: observations and 3D standard model
We present for the first time the evolution of the photospheric electric
currents during an eruptive X-class flare, accurately predicted by the standard
3D flare model. We analyze this evolution for the February 15, 2011 flare using
HMI/SDO magnetic observations and find that localized currents in \J-shaped
ribbons increase to double their pre-flare intensity. Our 3D flare model,
developed with the OHM code, suggests that these current ribbons, which develop
at the location of EUV brightenings seen with AIA imagery, are driven by the
collapse of the flare's coronal current layer. These findings of increased
currents restricted in localized ribbons are consistent with the overall free
energy decrease during a flare, and the shape of these ribbons also give an
indication on how much twisted the erupting flux rope is. Finally, this study
further enhances the close correspondence obtained between the theoretical
predictions of the standard 3D model and flare observations indicating that the
main key physical elements are incorporated in the model.Comment: 12 pages, 7 figure
The origin of net electric currents in solar active regions
There is a recurring question in solar physics about whether or not electric
currents are neutralized in active regions (ARs). This question was recently
revisited using three-dimensional (3D) magnetohydrodynamic (MHD) numerical
simulations of magnetic flux emergence into the solar atmosphere. Such
simulations showed that flux emergence can generate a substantial net current
in ARs. Another source of AR currents are photospheric horizontal flows. Our
aim is to determine the conditions for the occurrence of net vs. neutralized
currents with this second mechanism. Using 3D MHD simulations, we
systematically impose line-tied, quasi-static, photospheric twisting and
shearing motions to a bipolar potential magnetic field. We find that such
flows: (1) produce both {\it direct} and {\it return} currents, (2) induce very
weak compression currents - not observed in 2.5D - in the ambient field present
in the close vicinity of the current-carrying field, and (3) can generate
force-free magnetic fields with a net current. We demonstrate that neutralized
currents are in general produced only in the absence of magnetic shear at the
photospheric polarity inversion line - a special condition rarely observed. We
conclude that, as magnetic flux emergence, photospheric flows can build up net
currents in the solar atmosphere, in agreement with recent observations. These
results thus provide support for eruption models based on pre-eruption magnetic
fields possessing a net coronal current.Comment: 14 pages and 11 figures (Accepted in The Astrophysical Journal
First observational application of a connectivity--based helicity flux density
Measuring the magnetic helicity distribution in the solar corona can help in
understanding the trigger of solar eruptive events because magnetic helicity is
believed to play a key role in solar activity due to its conservation property.
A new method for computing the photospheric distribution of the helicity flux
was recently developed. This method takes into account the magnetic field
connectivity whereas previous methods were based on photospheric signatures
only. This novel method maps the true injection of magnetic helicity in active
regions. We applied this method for the first time to an observed active
region, NOAA 11158, which was the source of intense flaring activity. We used
high-resolution vector magnetograms from the SDO/HMI instrument to compute the
photospheric flux transport velocities and to perform a nonlinear force-free
magnetic field extrapolation. We determined and compared the magnetic helicity
flux distribution using a purely photospheric as well as a connectivity-based
method. While the new connectivity-based method confirms the mixed pattern of
the helicity flux in NOAA 11158, it also reveals a different, and more correct,
distribution of the helicity injection. This distribution can be important for
explaining the likelihood of an eruption from the active region. The
connectivity-based approach is a robust method for computing the magnetic
helicity flux, which can be used to study the link between magnetic helicity
and eruptivity of observed active regions.Comment: 4 pages, 3 figures; published online in A&A 555, L6 (2013
A model for straight and helical solar jets: II. Parametric study of the plasma beta
Jets are dynamic, impulsive, well-collimated plasma events that develop at
many different scales and in different layers of the solar atmosphere.
Jets are believed to be induced by magnetic reconnection, a process central
to many astrophysical phenomena. Within the solar atmosphere, jet-like events
develop in many different environments, e.g., in the vicinity of active regions
as well as in coronal holes, and at various scales, from small photospheric
spicules to large coronal jets. In all these events, signatures of helical
structure and/or twisting/rotating motions are regularly observed. The present
study aims to establish that a single model can generally reproduce the
observed properties of these jet-like events.
In this study, using our state-of-the-art numerical solver ARMS, we present a
parametric study of a numerical tridimensional magnetohydrodynamic (MHD) model
of solar jet-like events. Within the MHD paradigm, we study the impact of
varying the atmospheric plasma on the generation and properties of
solar-like jets.
The parametric study validates our model of jets for plasma ranging
from to , typical of the different layers and magnetic
environments of the solar atmosphere. Our model of jets can robustly explain
the generation of helical solar jet-like events at various . This
study introduces the new result that the plasma modifies the morphology
of the helical jet, explaining the different observed shapes of jets at
different scales and in different layers of the solar atmosphere.
Our results allow us to understand the energisation, triggering, and driving
processes of jet-like events. Our model allows us to make predictions of the
impulsiveness and energetics of jets as determined by the surrounding
environment, as well as the morphological properties of the resulting jets.Comment: Accepted in Astronomy and Astrophysic
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