209 research outputs found
Limb Event Brightenings and Fast Ejection Using IRIS Mission Observations
The Interface Region Imaging Spectrograph (IRIS) of the NASA small explorer
mission provides significantly more complete and higher resolution spectral
coverage of the dynamical conditions inside the chromosphere and transition
region (TR) than has heretofore been available. Near the solar limb high
temporal, spatial (0.3") and spectral resolution observations from the
ultraviolet IRIS spectra reveal high-energy limb event brightenings (LEBs) at
low chromospheric heights, around 1 Mm above the limb. They can be
characterized as explosive events producing jets. We selected two events
showing spectra of a confined eruption just off or near the quiet Sun limb, the
jet part showing obvious moving material with short duration large Doppler
shifts in three directions identified as macrospicules on slit-jaw (SJ) images
in Si IV and He II 304 A. The events are analyzed from a sequence of very close
rasters taken near the central meridian and the South pole limb. The processed
SJ images and the simultaneously observed fast spectral sequences having large
Doppler shifts, with a pair of red shifted elements together with a faster blue
shifted element from almost the same position, are analyzed. Shifts correspond
to velocities of up to 100 km/s in projection on the plane of the sky. The
occurrence of erupting spicules and macrospicules from these regions is noticed
from images taken before and after the spectra. The cool low first ionization
potential (FIP) element simultaneous line emissions of the MgII h and k
resonance lines do not clearly show a similar signature due to optical
thickness effects but the Si IV broad-band SJ images do. The bidirectional
plasma jets ejected from a small reconnection site are interpreted as the
result of coronal loop-loop interactions leading to reconnection in nearby
sites.Comment: 24 pages, 16 figures., Accepted in Sol. Phy
Polar Coronal Plumes as Tornado-Like Jets
We examine the dynamical behavior of white light polar plume structures in
the inner corona that are observed from the ground during total solar eclipses,
based on their EUV hot and cool emission line counterparts observed from space.
EUV observations from SDO/AIA of a sequence of rapidly varying coronal hole
structures are analyzed. Evidence of events showing acceleration in the 1.25 Mk
line of Fe XII at 193 A is given. The structures along the plume show an
outward velocity of about 140 kms-1 that can be interpreted as an upwards
propagating wave in the 304 A and 171 A lines; higher speeds are seen in 193 A
(up to 1000 km/s). The ejection of the cold He II plasma is delayed by about 4
min in the lowest layer and more than 12 min in the highest level compared to
the hot 193 A behavior. A study of the dynamics using time-slice diagrams
reveals that a large amount of fast ejected material originates from below the
plume, at the footpoints. The release of plasma material appears to come from a
cylinder with quasi-parallel edge-enhanced walls. After the initial phase of a
longitudinal acceleration, the speed substantially reduces and the ejecta
disperse into the environment. Finally, the detailed temporal and spatial
relationships between the cool and hot components were studied with
simultaneous multi-wavelength observations, using more AIA data. The
outward-propagating perturbation of the presumably magnetic walls of polar
plumes supports the suggestion that Alfven waves propagate outwardly along
these radially extended walls.Comment: 17 pages, 10 figures, accepted in Ap
About the directional properties of Solar Spicules from Hough Transform analysis
Spicules are intermittently rising above the surface of the Sun eruptions;
EUV jets are now also reported in immediately above layers. The variation of
spicule orientation with respect to the solar latitude, presumably reflecting
the confinement and the focusing of ejecta by the surrounding global coronal
magnetic field, is an important parameter to understand their dynamical
properties. A wealth of high resolution images of limb spicules are made
available in H CaII emission from the SOT Hinode mission. Furthermore, the
Hough transform is applied to the resulting images for making a statistical
analysis of spicule orientations in different regions around the solar limb,
from the pole to the equator. Results show a large difference of spicule
apparent tilt angles in: (i) the solar pole regions, (ii) the equatorial
regions, (iii) the active regions and (iv) the coronal hole regions. Spicules
are visible in a radial direction in the polar regions with a tilt angle (less
than 200). The tilt angle is even reduced to 10 degrees inside the coronal hole
with open magnetic field lines and at the lower latitude the tilt angle reaches
values in excess of 50 degree. Usually, which is in close resemblance to the
rosettes made of dark mottles and fibrils in projection on the solar disk. The
inference of these results for explaining the so-called chromospheric
prolateness observed at solar minimum of activity in cool chromospheric lines
is considered.Comment: 13 pages, 6 figure
Improved SOT (Hinode mission) high resolution solar imaging observations
We consider the best today available observations of the Sun free of
turbulent Earth atmospheric effects, taken with the Solar Optical Telescope
(SOT) onboard the Hinode spacecraft. Both the instrumental smearing and the
observed stray light are analyzed in order to improve the resolution. The Point
Spread Function (PSF) corresponding to the blue continuum Broadband Filter
Imager (BFI) near 450 nm is deduced by analyzing i/ the limb of the Sun and ii/
images taken during the transit of the planet Venus in 2012. A combination of
Gaussian and Lorentzian functions is selected to construct a PSF in order to
remove both smearing due to the instrumental diffraction effects (PSF core) and
the large-angle stray light due to the spiders and central obscuration (wings
of the PSF) that are responsible for the parasitic stray light. A
Max-likelihood deconvolution procedure based on an optimum number of iterations
is discussed. It is applied to several solar field images, including the
granulation near the limb. The normal non-magnetic granulation is compared to
the abnormal granulation which we call magnetic. A new feature appearing for
the first time at the extreme- limb of the disk (the last 100 km) is discussed
in the context of the definition of the solar edge and of the solar diameter. A
single sunspot is considered in order to illustrate how effectively the
restoration works on the sunspot core. A set of 125 consecutive deconvolved
images is assembled in a 45 min long movie illustrating the complexity of the
dynamical behavior inside and around the sunspot.Comment: 15 pages, 22 figures, 1 movi
Alfvenic waves in polar spicules
Context. For investigating spicules from the photosphere to coronal heights,
the new Hinode/SOT long series of high resolution observations from Space taken
in CaII H line emission offers an improved way to look at their remarkable
dynamical behavior using images free of seeing effects. They should be put in
the context of the huge amount of already accumulated material from
ground-based instruments, including high- resolution spectra of off-limb
spicules. Results. The surge-like behavior of solar polar region spicules
supports the untwisting multi-component interpretation of spicules exhibiting
helical dynamics. Several tall spicules are found with (i) upward and downward
flows similar at lower and middle-levels, the rate of upward motion being
slightly higher at high levels; (ii) the left and right-hand velocities are
also increasing with height; (iii) a large number of multi-component spicules
show shearing motion of both left-handed and right-handed senses occurring
simultaneously, which might be understood as twisting (or untwisting) threads.
The number of turns depends on the overall diameter of the structure made of
components and changes from at least one turn for the smallest structure to at
most two or three turns for surge-like broad structures; the curvature along
the spicule corresponds to a low turn number similar to a transverse kink mode
oscillation along the threads.Comment: 8 pages, 10 figures, Accepted in Astronomy and Astrophysic
Chromospheric peculiar off-limb dynamical events from IRIS observations
To study motions and oscillations in the solar chromosphere and at the
transition region (TR) level we analyze some extreme Doppler shifts observed
off-limb with the Interface Region Imaging Spectrograph (IRIS). Raster scans
and slit-jaw imaging observations performed in the near-ultraviolet (NUV)
channels were used. Large transverse oscillations are revealed by the far wings
profiles after accurately removing the bulk average line profiles of each
sequence. Different regions around the Sun are considered. Accordingly, the
cool material of spicules is observed in Mg II lines rather dispersed up to
coronal heights. In the quiet Sun and especially in a polar coronal hole, we
study dynamical properties of the dispersed spicules-material off-limb using a
high spectral, temporal and spatial resolutions IRIS observations. We suggest
that numerous small-scale jet-like spicules show rapid twisting and swaying
motions evidenced by the large distortion and dispersion of the line profiles,
including impressive periodic Doppler shifts. Most of these events repeatedly
appear in red- and blue-shifts above the limb throughout the whole interval of
the observation datasets with an average swaying speed of order +/-35 kms-1
reaching a maximum value of 50 km s-1 in the polar coronal hole region, well
above the 2.2 Mm heights. We identified for the 1st time waves with a short
period of order of 100 sec and less and transverse amplitudes of order of +/-
20 to 30 km s-1 with the definite signature of Alfven waves. No correlation
exists between brightness and Doppler shift variations; the phase speed of the
wave is very large and cannot definitely be determined from the spectral
features seen along the quasi-radial features. Even shorter periods waves are
evidenced, although their contrast is greatly attenuated by the overlapping
effects along the line of sight.Comment: 15 pages, 9 figs. accepted in Ap
Oscillations and waves related to sunspots
In order to study umbral oscillations, running penumbral waves and the relationship between them, we analyzed CCD, high-resolution, sunspot observations obtained at the center and the wings of the Hα line and the Fe I 5576 ˚A
line using a UBF filter. We produced “space/time slice images” which show that there is not a clear relationship between umbral oscillations and running penumbral waves as they observed in upper chromospheric layers. We found that the running penumbral waves are observable at least up to the formation height of the Hα±0.5 ˚A line, but not in the Hα±0.75 ˚A or the Fe I±0.12 ˚A. The correlation between umbral oscillations at various atmospheric heights and running penumbral waves strongly indicates that the latter are excited by photospheric umbral oscillations and not the
chromospheric ones
Evaluation of a method for the resolution improvement of near limb solar images
We present a methodology, based onthe correctionfor the limb
darkening and the use of a directionally sensitive operator the “MadMax”, for the image processing of observations obtained near the solar limb. Our image processing method substantially enhances near-limb observations and permits an insight into the studies of the very fine chromospheric structures, over higher-resolution images. Space/time images produced from filtergrams processed with our method indicate that polar surges and spicules are probably related to different physical mechanisms
A model of the prolate chromosphere formation at the solar minimum
Detailed observations in different chromospheric lines of a solar diameter in polar and equatorial directions showed that the polar chromosphere at the minimum phase of solar cycle looks more extended than the low-latitude chromosphere. We propose a simple geometric model to explainthe effect of the prolateness of the solar chromosphere. A specific dynamical part of the solar atmosphere above the 2 Mm level is assumed to be a mixture of moving up and down jets of chromospheric matter with the coronal plasma between them. Due to the dynamic nature of this layer, the magnetic field is considered to play a very important role in the density distribution with the height, guiding the mass flows along the field lines. The difference of the magnetic-field topology in the polar and the equatorial regions leads to different heights of the chromospheric limb
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