252 research outputs found
Coronal mass ejections from the same active region cluster: Two different perspectives
The cluster formed by active regions (ARs) NOAA 11121 and 11123,
approximately located on the solar central meridian on 11 November 2010, is of
great scientific interest. This complex was the site of violent flux emergence
and the source of a series of Earth-directed events on the same day. The onset
of the events was nearly simultaneously observed by the Atmospheric Imaging
Assembly (AIA) telescope aboard the Solar Dynamics Observatory (SDO) and the
Extreme-Ultraviolet Imagers (EUVI) on the Sun-Earth Connection Coronal and
Heliospheric Investigation (SECCHI) suite of telescopes onboard the
Solar-Terrestrial Relations Observatory (STEREO) twin spacecraft. The
progression of these events in the low corona was tracked by the Large Angle
Spectroscopic Coronagraphs (LASCO) onboard the Solar and Heliospheric
Observatory (SOHO) and the SECCHI/COR coronagraphs on STEREO. SDO and SOHO
imagers provided data from the Earth's perspective, whilst the STEREO twin
instruments procured images from the orthogonal directions. This spatial
configuration of spacecraft allowed optimum simultaneous observations of the AR
cluster and the coronal mass ejections that originated in it. Quadrature
coronal observations provided by STEREO revealed a notably large amount of
ejective events compared to those detected from Earth's perspective.
Furthermore, joint observations by SDO/AIA and STEREO/SECCHI EUVI of the source
region indicate that all events classified by GOES as X-ray flares had an
ejective coronal counterpart in quadrature observations. These results have
direct impact on current space weather forecasting because of the probable
missing alarms when there is a lack of solar observations in a view direction
perpendicular to the Sun-Earth line.Comment: Solar Physics - Accepted for publication 2015-Apr-25 v2: Corrected
metadat
Topological Analysis of Emerging Bipole Clusters Producing Violent Solar Events
During the rising phase of Solar Cycle 24 tremendous activity occurred on the
Sun with fast and compact emergence of magnetic flux leading to bursts of
flares (C to M and even X-class). We investigate the violent events occurring
in the cluster of two active regions (ARs), NOAA numbers 11121 and 11123,
observed in November 2010 with instruments onboard the {\it Solar Dynamics
Observatory} and from Earth. Within one day the total magnetic flux increased
by with the emergence of new groups of bipoles in AR 11123. From all the
events on 11 November, we study, in particular, the ones starting at around
07:16 UT in GOES soft X-ray data and the brightenings preceding them. A
magnetic-field topological analysis indicates the presence of null points,
associated separatrices and quasi-separatrix layers (QSLs) where magnetic
reconnection is prone to occur. The presence of null points is confirmed by a
linear and a non-linear force-free magnetic-field model. Their locations and
general characteristics are similar in both modelling approaches, which
supports their robustness. However, in order to explain the full extension of
the analysed event brightenings, which are not restricted to the photospheric
traces of the null separatrices, we compute the locations of QSLs. Based on
this more complete topological analysis, we propose a scenario to explain the
origin of a low-energy event preceding a filament eruption, which is
accompanied by a two-ribbon flare, and a consecutive confined flare in AR
11123. The results of our topology computation can also explain the locations
of flare ribbons in two other events, one preceding and one following the ones
at 07:16 UT. Finally, this study provides further examples where flare-ribbon
locations can be explained when compared to QSLs and only, partially, when
using separatrices.Comment: 42 pages, 15 figure
How are Emerging Flux, Flares and CMEs Related to Magnetic Polarity Imbalance in MDI Data?
In order to understand whether major flares or coronal mass ejections (CMEs)
can be related to changes in the longitudinal photospheric magnetic field, we
study 4 young active regions during seven days of their disc passage. This time
period precludes any biases which may be introduced in studies that look at the
field evolution during the short-term flare or CME period only. Data from the
Michelson Doppler Imager (MDI) with a time cadence of 96 minutes are used.
Corrections are made to the data to account for area foreshortening and angle
between line of sight and field direction, and also the underestimation of the
flux densities. We make a systematic study of the evolution of the longitudinal
magnetic field, and analyze flare and CME occurrence in the magnetic evolution.
We find that the majority of CMEs and flares occur during or after new flux
emergence. The flux in all four active regions is observed to have deviations
from polarity balance both on the long-term (solar rotation) and on the short
term (few hours). The long-term imbalance is not due to linkage outside the
active region; it is primarily related to the east-west distance from central
meridian, with the sign of polarity closer to the limb dominating. The sequence
of short term imbalances are not closely linked to CMEs and flares and no
permanent imbalance remains after them. We propose that both kinds of imbalance
are due to the presence of a horizontal field component (parallel to the
photospheric surface) in the emerging flux.Comment: 22 pages, 8 figures, Solar Physics (in press
How Can Active Region Plasma Escape into the Solar Wind from below a Closed Helmet Streamer?
Recent studies show that active-region (AR) upflowing plasma, observed by the
EUV-Imaging Spectrometer (EIS), onboard Hinode, can gain access to open
field-lines and be released into the solar wind (SW) via magnetic-interchange
reconnection at magnetic null-points in pseudo-streamer configurations. When
only one bipolar AR is present on the Sun and it is fully covered by the
separatrix of a streamer, such as AR 10978 in December 2007, it seems unlikely
that the upflowing AR plasma can find its way into the slow SW. However,
signatures of plasma with AR composition have been found at 1 AU by Culhane et
al. (2014) apparently originating from the West of AR 10978. We present a
detailed topology analysis of AR 10978 and the surrounding large-scale corona
based on a potential-field source-surface (PFSS) model. Our study shows that it
is possible for the AR plasma to get around the streamer separatrix and be
released into the SW via magnetic reconnection, occurring in at least two main
steps. We analyse data from the Nan\c{c}ay Radioheliograph (NRH) searching for
evidence of the chain of magnetic reconnections proposed. We find a noise storm
above the AR and several varying sources at 150.9 MHz. Their locations suggest
that they could be associated with particles accelerated during the first-step
reconnection process and at a null point well outside of the AR. However, we
find no evidence of the second-step reconnection in the radio data. Our results
demonstrate that even when it appears highly improbable for the AR plasma to
reach the SW, indirect channels involving a sequence of reconnections can make
it possible.Comment: 26 pages, 10 figures. appears in Solar Physics, 201
Parallel Evolution of Quasi-separatrix Layers and Active Region Upflows
Persistent plasma upflows were observed with Hinode's EUV Imaging
Spectrometer (EIS) at the edges of active region (AR) 10978 as it crossed the
solar disk. We analyze the evolution of the photospheric magnetic and velocity
fields of the AR, model its coronal magnetic field, and compute the location of
magnetic null-points and quasi-sepratrix layers (QSLs) searching for the origin
of EIS upflows. Magnetic reconnection at the computed null points cannot
explain all of the observed EIS upflow regions. However, EIS upflows and QSLs
are found to evolve in parallel, both temporarily and spatially. Sections of
two sets of QSLs, called outer and inner, are found associated to EIS upflow
streams having different characteristics. The reconnection process in the outer
QSLs is forced by a large-scale photospheric flow pattern which is present in
the AR for several days. We propose a scenario in which upflows are observed
provided a large enough asymmetry in plasma pressure exists between the
pre-reconnection loops and for as long as a photospheric forcing is at work. A
similar mechanism operates in the inner QSLs, in this case, it is forced by the
emergence and evolution of the bipoles between the two main AR polarities. Our
findings provide strong support to the results from previous individual case
studies investigating the role of magnetic reconnection at QSLs as the origin
of the upflowing plasma. Furthermore, we propose that persistent reconnection
along QSLs does not only drive the EIS upflows, but it is also responsible for
a continuous metric radio noise-storm observed in AR 10978 along its disk
transit by the Nan\c{c}ay Radio Heliograph.Comment: 29 pages, 10 figure
Companion Event and Precursor of the X17 Flare on 28 October 2003
A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Há and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point.Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Deluca, E. E.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Uddin, W.. Aryabhatta Research Institute of Observational Sciences (ARIES); Indi
Energy spectrum of turbulent fluctuations in boundary driven reduced magnetohydrodynamics
The nonlinear dynamics of a bundle of magnetic flux ropes driven by
stationary fluid motions at their endpoints is studied, by performing numerical
simulations of the magnetohydrodynamic (MHD) equations. The development of MHD
turbulence is shown, where the system reaches a state that is characterized by
the ratio between the Alfven time (the time for incompressible MHD waves to
travel along the field lines) and the convective time scale of the driving
motions. This ratio of time scales determines the energy spectra and the
relaxation toward different regimes ranging from weak to strong turbulence. A
connection is made with phenomenological theories for the energy spectra in MHD
turbulence.Comment: Published in Physics of Plasma
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