602 research outputs found
Seasonal and site-specific variation in vapour and aerosol phase PAHs over Flanders (Belgium) and their relation with anthropogenic activities
Peer reviewe
Time delays in quasi-periodic pulsations observed during the X2.2 solar flare on 2011 February 15
We report observations of quasi-periodic pulsations (QPPs) during the X2.2
flare of 2011 February 15, observed simultaneously in several wavebands. We
focus on fluctuations on time scale 1-30 s and find different time lags between
different wavebands. During the impulsive phase, the Reuven Ramaty High Energy
Solar Spectroscopic Imager (RHESSI) channels in the range 25-100 keV lead all
the other channels. They are followed by the Nobeyama RadioPolarimeters at 9
and 17 GHz and the Extreme Ultra-Violet (EUV) channels of the Euv
SpectroPhotometer (ESP) onboard the Solar Dynamic Observatory (SDO). The
Zirconium and Aluminum filter channels of the Large Yield Radiometer (LYRA)
onboard the Project for On-Board Autonomy (PROBA2) satellite and the SXR
channel of ESP follow. The largest lags occur in observations from the
Geostationary Operational Environmental Satellite (GOES), where the channel at
1-8 {\AA} leads the 0.5-4 {\AA} channel by several seconds. The time lags
between the first and last channels is up to 9 s. We identified at least two
distinct time intervals during the flare impulsive phase, during which the QPPs
were associated with two different sources in the Nobeyama RadioHeliograph at
17 GHz. The radio as well as the hard X-ray channels showed different lags
during these two intervals. To our knowledge, this is the first time that time
lags are reported between EUV and SXR fluctuations on these time scales. We
discuss possible emission mechanisms and interpretations, including flare
electron trapping
Transverse oscillations in solar coronal loops induced by propagating Alfvenic pulses
The propagation and the evolution of Alfvenic pulses in the solar coronal
arcades is investigated by means of MHD numerical simulations. Significant
transverse oscillations in coronal loops, triggered by nearby flare events, are
often measured in EUV lines and are generally interpreted as standing kink
modes. However, the damping times of these oscillations are typically very
short (from one to a few periods) and the physical mechanism responsible for
the decay is still a matter of debate. Moreover, the majority of the observed
cases actually appears to be better modeled by propagating, rather than
standing, modes. Here we perform 2.5-D compressible MHD simulations of
impulsively generated Alfven waves propagating in a potential magnetic arcade
(assumed as a simplified 2-D loop model), taking into account the
stratification of the solar atmosphere with height from the photosphere to the
corona. The results show a strong spreading of the initially localized pulses
along the loop, due to the variations in the Alfven velocity with height, and
correspondingly an efficient damping of the amplitude of the oscillations. We
believe that simple explanations based on the effects of wave propagation in
highly inhomogeneous media may apply to the majority of the reported cases, and
that variations of the background density and Alfven speed along the loop
should be considered as key ingredients in future models.Comment: Accepted for publication in A&A on 26 October 2004; 10 pages, 8
figure
Multistage Reconnection Powering a Solar Coronal Jet
Coronal jets are short-lived eruptive features commonly observed in polar coronal holes and are thought to play a key role in the transfer of mass and energy into the solar corona. We describe unique contemporaneous observations of a coronal blowout jet seen by the Extreme Ultraviolet Imager (EUI) on board the Solar Orbiter (SO) spacecraft and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The coronal jet erupted from the south polar coronal hole, and was observed with high spatial and temporal resolution by both instruments. This enabled identification of the different stages of a breakout reconnection process producing the observed jet. We find bulk plasma flow kinematics of ∼100-200 km s−1 across the lifetime of its observed propagation, with a distinct kink in the jet where it impacted and was subsequently guided by a nearby polar plume. We also identify a faint faster feature ahead of the bulk plasma motion propagating with a velocity of ∼715 km s−1, which we attribute to untwisting of newly reconnected field lines during the eruption. A differential emission measure (DEM) analysis using the SDO/AIA observations revealed a very weak jet signal, indicating that the erupting material was likely much cooler than the coronal passbands used to derive the DEM. This is consistent with the very bright appearance of the jet in the Lyα passband observed by SO/EUI. The DEM was used to estimate the radiative thermal energy of the source region of the coronal jet, finding a value of ∼2 × 1024 erg, comparable to the energy of a nanoflare
The SWAP EUV Imaging Telescope Part I: Instrument Overview and Pre-Flight Testing
The Sun Watcher with Active Pixels and Image Processing (SWAP) is an EUV
solar telescope on board ESA's Project for Onboard Autonomy 2 (PROBA2) mission
launched on 2 November 2009. SWAP has a spectral bandpass centered on 17.4 nm
and provides images of the low solar corona over a 54x54 arcmin field-of-view
with 3.2 arcsec pixels and an imaging cadence of about two minutes. SWAP is
designed to monitor all space-weather-relevant events and features in the low
solar corona. Given the limited resources of the PROBA2 microsatellite, the
SWAP telescope is designed with various innovative technologies, including an
off-axis optical design and a CMOS-APS detector. This article provides
reference documentation for users of the SWAP image data.Comment: 26 pages, 9 figures, 1 movi
Hinode/EIS observations of propagating low-frequency slow magnetoacoustic waves in fan-like coronal loops
We report the first observation of multiple-periodic propagating disturbances
along a fan-like coronal structure simultaneously detected in both intensity
and Doppler shift in the Fe XII 195 A line with the EUV Imaging Spectrometer
(EIS) onboard Hinode. A new application of coronal seismology is provided based
on this observation. We analyzed the EIS sit-and-stare mode observation of
oscillations using the running difference and wavelet techniques. Two harmonics
with periods of 12 and 25 min are detected. We measured the Doppler shift
amplitude of 1-2 km/s, the relative intensity amplitude of 3%-5% and the
apparent propagation speed of 100-120 km/s. The amplitude relationship between
intensity and Doppler shift oscillations provides convincing evidence that
these propagating features are a manifestation of slow magnetoacoustic waves.
Detection lengths (over which the waves are visible) of the 25 min wave are
about 70-90 Mm, much longer than those of the 5 min wave previously detected by
TRACE. This difference may be explained by the dependence of damping length on
the wave period for thermal conduction. Based on a linear wave theory, we
derive an inclination of the magnetic field to the line-of-sight about 598
deg, a true propagation speed of 12825 km/s and a temperature of
0.70.3 MK near the loop's footpoint from our measurements.Comment: 4 pages and 4 figures, with 3 online figures and 1 online table;
Astron & Astrophys Letter, in pres
Energy Distribution of Micro-events in the Quiet Solar Corona
Recent imaging observations of EUV line emissions have shown evidence for
frequent flare-like events in a majority of the pixels in quiet regions of the
solar corona. The changes in coronal emission measure indicate impulsive
heating of new material to coronal temperatures. These heating or evaporation
events are candidate signatures of "nanoflares" or "microflares" proposed to
interpret the high temperature and the very existence of the corona. The energy
distribution of these micro-events reported in the literature differ widely,
and so do the estimates of their total energy input into the corona. Here we
analyze the assumptions of the different methods, compare them by using the
same data set and discuss their results.
We also estimate the different forms of energy input and output, keeping in
mind that the observed brightenings are most likely secondary phenomena. A
rough estimate of the energy input observed by EIT on the SoHO satellite is of
the order of 10% of the total radiative output in the same region. It is
considerably smaller for the two reported TRACE observations. The discrepancy
can be explained partially by different thresholds for flare detection. There
is agreement on the slope and the absolute value of the distribution if the
same method were used and a numerical error corrected. The extrapolation of the
power law to unobserved energies that are many orders of magnitude smaller
remains questionable. Nevertheless, these micro-events and unresolved smaller
events are currently the best source of information on the heating process of
the corona
Characterization of the heme pocket structure and ligand binding kinetics of non-symbiotic hemoglobins from the model legume lotus japonicus
Plant hemoglobins (Hbs) are found in nodules of legumes and actinorhizal plants but also in non-symbiotic organs of monocots and dicots. Non-symbiotic Hbs (nsHbs) have been classified into two phylogenetic groups. Class 1 nsHbs show an extremely high O2 affinity and are induced by hypoxia and nitric oxide (NO), whereas class 2 nsHbs have moderate O2 affinity and are induced by cold and cytokinins. The functions of nsHbs are still unclear, but some of them rely on the capacity of hemes to bind diatomic ligands and catalyze the NO dioxygenase (NOD) reaction (oxyferrous Hb + NO ? ferric Hb + nitrate). Moreover, NO may nitrosylate Cys residues of proteins. It is therefore important to determine the ligand binding properties of the hemes and the role of Cys residues. Here, we have addressed these issues with the two class 1 nsHbs (LjGlb1-1 and LjGlb1-2) and the single class 2 nsHb (LjGlb2) of Lotus japonicus, which is a model legume used to facilitate the transfer of genetic and biochemical information into crops. We have employed carbon monoxide (CO) as a model ligand and resonance Raman, laser flash photolysis, and stopped-flow spectroscopies to unveil major differences in the heme environments and ligand binding kinetics of the three proteins, which suggest non-redundant functions. In the deoxyferrous state, LjGlb1-1 is partially hexacoordinate, whereas LjGlb1-2 shows complete hexacoordination (behaving like class 2 nsHbs) and LjGlb2 is mostly pentacoordinate (unlike other class 2 nsHbs). LjGlb1-1 binds CO very strongly by stabilizing it through hydrogen bonding, but LjGlb1-2 and LjGlb2 show lower CO stabilization. The changes in CO stabilization would explain the different affinities of the three proteins for gaseous ligands. These affinities are determined by the dissociation rates and follow the order LjGlb1-1 > LjGlb1-2 > LjGlb2. Mutations LjGlb1-1 C78S and LjGlb1-2 C79S caused important alterations in protein dynamics and stability, indicating a structural role of those Cys residues, whereas mutation LjGlb1-1 C8S had a smaller effect. The three proteins and their mutant derivatives exhibited similarly high rates of NO consumption, which were due to NOD activity of the hemes and not to nitrosylation of Cys residues
LUCI onboard Lagrange, the Next Generation of EUV Space Weather Monitoring
LUCI (Lagrange eUv Coronal Imager) is a solar imager in the Extreme
UltraViolet (EUV) that is being developed as part of the Lagrange mission, a
mission designed to be positioned at the L5 Lagrangian point to monitor space
weather from its source on the Sun, through the heliosphere, to the Earth. LUCI
will use an off-axis two mirror design equipped with an EUV enhanced active
pixel sensor. This type of detector has advantages that promise to be very
beneficial for monitoring the source of space weather in the EUV. LUCI will
also have a novel off-axis wide field-of-view, designed to observe the solar
disk, the lower corona, and the extended solar atmosphere close to the
Sun-Earth line. LUCI will provide solar coronal images at a 2-3 minute cadence
in a pass-band centred on 19.5 nm. Observations made through this pass-band
allow for the detection and monitoring of semi-static coronal structures such
as coronal holes, prominences, and active regions; as well as transient
phenomena such as solar flares, limb Coronal Mass Ejections (CMEs), EUV waves,
and coronal dimmings. The LUCI data will complement EUV solar observations
provided by instruments located along the Sun-Earth line such as PROBA2-SWAP,
SUVI-GOES and SDO-AIA, as well as provide unique observations to improve space
weather forecasts. Together with a suite of other remote-sensing and in-situ
instruments onboard Lagrange, LUCI will provide science quality operational
observations for space weather monitoring
Beyond small-scale transients: a closer look at the diffuse quiet solar corona
Within the quiet Sun corona imaged at 1 MK, much of the field of view
consists of diffuse emission that appears to lack the spatial structuring that
is so evident in coronal loops or bright points. We seek to determine if these
diffuse regions are categorically different in terms of their intensity
fluctuations and spatial configuration from the more well-studied dynamic
coronal features. We analyze a time series of observations from Solar Orbiter's
High Resolution Imager in the Extreme Ultraviolet to quantify the
characterization of the diffuse corona at high spatial and temporal
resolutions. We then compare this to the dynamic features within the field of
view, mainly a coronal bright point. We find that the diffuse corona lacks
visible structuring, such as small embedded loops, and that this is persistent
over the 25 min duration of the observation. The intensity fluctuations of the
diffuse corona, which are within +/-5%, are significantly smaller in comparison
to the coronal bright point. Yet, the total intensity observed in the diffuse
corona is of the same order as the bright point. It seems inconsistent with our
data that the diffuse corona is a composition of small loops or jets or that it
is driven by discrete small heating events that follow a power-law-like
distribution. We speculate that small-scale processes like MHD turbulence might
be energizing the diffuse regions, but at this point we cannot offer a
conclusive explanation for the nature of this feature.Comment: Accepted for publication in A&A. 10 pages, 8 figure
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