text:
\section{Introduction} \label{sec:intro}

Solar flares are explosive phenomena occurring in the solar atmosphere, which indicate a rapid conversion of magnetic energy into other forms of energy (kinetic, radiative, particle acceleration, etc.). This process, which is believed to result from magnetic reconnection within a region with highly unstable magnetic field configurations, can produce emission of electromagnetic radiation in almost the entire electromagnetic spectrum (depending on the energy involved, which can span from 10$^{28}$ to 10$^{32}$ erg) and is associated with an increase in brightness of the corona, chromosphere and, occasionally, the  photosphere (see, e.g. \cite{fletcher} and references therein, for a review).

Several mechanisms are involved in such a broad range of electromagnetic radiation emission at various atmospheric heights. Flares are often contextualized in the well-known CSHKP flare geometry (named for \citealt{carmi,sturr,hira} and \citealt{kopp}) which suggests that when an instability sets in, magnetic reconnection takes place (usually at the coronal level) resulting in electrons and protons being accelerated. But models dealing with coronal processes have little to say about the details of the generation of flare chromospheric emission, particularly in the lower atmosphere. Initial models of atmospheric emission lines were based on empirical models of flaring atmospheres or, assuming an electron-beam plasma heating mechanism, radiative transfer simulations \citep{canfield}. However more recently we have started to turn to radiation-hydrodynamic (RHD) flare simulations (\citealt{Abbet,allred} and \citealt{kaspa09}) which model the effect of accelerated particles traveling through the lower atmospheric layers, impulsively heating the local plasma, and causing an expansion of the chromosphere in a process termed chromospheric evaporation.

To test and constrain the electron-beam energy transport model we need to identify sensitive diagnostic radiation signatures, observations of which can be compared to the output of targeted numerical simulations. In this regard, the chromosphere presents an ideal test-bed for analyzing the release and redistribution of energy from accelerated particles in this region. In particular, observation and modeling of spectral lines emergent from different layers of the chromosphere can be used to understand how the chromosphere responds to energy input at different heights, and thereby to constrain the beam properties. But such investigations also serve an additional, exploratory, purpose by helping us to identify the best ways - e.g. choices of wavelength, temporal and spectral resolution - to get the maximum diagnostic power from flare optical observations, which can be very challenging to plan and execute.

In this paper we present flare observations at high temporal and spatial resolution in the H$\alpha$ and H$\beta$ lines, with accompanying RHD simulations. Though among the strongest spectral lines emitted by flares, simultaneous observations in these two lines are very rare. This flare is therefore of interest, as we can probe the behavior of H$\alpha$ and H$\beta$ to obtain insight into flare chromospheric excitation at their different formation heights. The H$\alpha$, H$\beta$ and H$\gamma$ lines were investigated theoretically by \citet{kaspa09} who used 1-D radiation hydrodynamics and test particle modelling to simulate the propagation, scattering and collisional energy loss of an electron beam (including direct collisional excitation of the hydrogen lines by beam particles), and calculate the emergent Balmer-line radiation. They demonstrated that Balmer line intensities are expected to be correlated on sub-second timescales, and that the intensity variations in line centres and line wings are dependent on the atmospheric heating, and the parameters of the electron beams.

It is worthwhile to stress that simultaneous H$\alpha$ and H$\beta$ observations of a flare is very rare, therefore, the results obtained from the present investigation could provide new and important insights in the comprehension of flare emission mechanisms in the relevant wavelengths and atmospheric heights.

In this paper, we study the flare SOL2014-04-22, that occurred close to the western limb of the Sun and compare observational data acquired from ground-based and satellite instruments with the results obtained from the Radiative hydrodynamic (RADYN) code (\citealt{carlsson97}, and \citealt{allred,AllredKowalskiCarlsson:2015}) in order to investigate the behavior of H${\alpha}$ and H${\beta}$, in response to the energy injected into the chromosphere during flaring. From observations and RADYN models of energy injection by an electron beam, we obtain and compare the absolute H${\alpha}$ and H${\beta}$ intensities, and their ratio, at high temporal resolution. We find that variations of this ratio between footpoints might be due to variations of the injected energy flux between models, suggesting that a well-calibrated H${\alpha}$/H${\beta}$ ratio, and sufficiently high temporal and spatial resolution could provide information on flare energy injection. We also examine the observed and simulated H${\alpha}$ line profile; the comparison allows us to constrain the filling factor of H${\alpha}$-emitting material.

We believe that this study is useful for planned future observations with the next generation of large aperture solar telescopes, such as the Daniel K. Inouye Solar Telescope (formerly the Advanced Technology Solar Telescope, \cite{Keil2010})  and the European Solar Telescope \citep{Collados2010}.

This paper is organized as follows: in Sect. 2 we describe the observational data and in Sect. 3 the data analysis is reported. In Sect. 4 the results obtained from the RADYN models are reported and discussed. In Sect. 5 we draw our conclusions.

\begin{figure*}[ht]
\centering
\includegraphics[width=0.9\textwidth]{cont_magn_FOV}
\caption{\textit{Left}: HMI/SDO magnetogram showing AR 12035 on 2014 Apr 22: white (black) regions indicate sites of positive (negative) longitudinal magnetic field; \textit{right}: HMI/SDO continuum image showing the photospheric configuration of AR 12035 on the same day. The red circle, with a diameter of $90''$, displays the IBIS field of view; the blue box, with a size of $ \sim 59''$, indicates the ROSA field of view. In this and in the following images, if not otherwise specified, North is on the top, West is at the right.}
\label{fig1}
\end{figure*}

\section{Observations}

An observing campaign was carried out on 2014-April-22 at the Dunn Solar Telescope (DST) at the US National Solar Observatory in New Mexico, using two different instruments: the Interferometric Bi-dimensional Spectrometer \citep[IBIS,][]{caval06} and the Rapid Oscillations in the Solar Atmosphere \citep[ROSA,][]{jess10}. The target of the observations was AR 12035, 67.7W 12.4S, characterized by a $\beta\gamma$ configuration (see Figure \ref{fig1}).

The aim of the campaign was to determine: a) the source location, sizes and the eventual offset between flare sources at different wavelengths, including any offset between the H$\alpha$ emission in the core and in the wings, in order to investigate whether it is possible to deduce any spatial dependence of energy deposition; b) the time evolution of flare energy input by examining intensity variations on the shortest possible timescales; c) any evidence for continuum enhancement, although we don't pursue this avenue in the following.

\subsection{Ground-based observations}
The IBIS instrument acquired data in two consecutive time intervals: the first dataset was acquired during the pre-flare phase, while the second one covered all the C3.3 flare (flare B) evolution. More precisely,
the first dataset includes 1000 scans of the H${\alpha}$ line centered at 6563 \AA~ from 14:22 UT to 15:05 UT; each spectral profile was sampled with a total of 17 wavelength points (average step = 0.2 \AA) in about 2.61 s.
The second dataset consists of 900 scans of the H${\alpha}$ line from 15:08 UT to 15:44 UT, with the same spectral sampling used to acquire the first dataset. In both cases the H$\alpha$
line has been acquired in spectral mode without polarimetric measurements, with a pixel size of about $0.09''$ pixel$^{-1}$.

For each narrow-band filtergram, a simultaneous broadband image (6610 $\pm$ 50 \AA )  was
acquired, with the same exposure time and the same field of view (FOV), characterized by a circular shape, with a diameter of $90''$.
To reduce the seeing degradation and obtain a homogeneous resolution across the whole FOV of 1000 $\times$ 1000 pixels,
the broadband images have been restored using the Multi-Object Multi-Frame Blind Deconvolution (MOMFBD, \cite{momfb}) technique.
We computed the global and local shifts necessary to align and destretch the broadband images with respect to the
MOMFBD restored broadband images. The same shifts have been applied to the narrow-band images.

Figure \ref{fig1} (\textit{right panel}) highlights the IBIS field of view with a red circle on SDO/HMI continuum, while Figure \ref{ibis_con} shows an example of the IBIS data in the continuum and in the core of the H${\alpha}$ line.

\begin{figure}
\centering
\includegraphics[width=0.23\textwidth]{bb_370}
\includegraphics[width=0.23\textwidth]{halpha_370}
\caption{IBIS FOV after the flare peak. ($a$) Continuum, ($b$) H$\alpha$ line core.}
\label{ibis_con}
\end{figure}

Co-spatial and co-temporal observations of the same active region were undertaken between 15:10:33 and 15:46:00 UT
with the Rapid Oscillations in the Solar Atmosphere (ROSA; \citet{jess10})
imaging system installed at the DST.
The dataset includes simultaneous imaging in the Ca {\sc{ii}} K core at 3933.7 {\AA} (bandpass 1.0 {\AA}), the G band at 4305.5 {\AA},
(bandpass 9.2 {\AA}), continuum 4170 {\AA} (bandpass 52.0 {\AA}) and H$\beta$ core at 4861 {\AA} (bandpass 0.1 {\AA})
which was obtained through the Universal Birefringent Filter (UBF). The G band and continuum observations were obtained with a spatial sampling of $0.069''$ pixel$^{-1}$ whereas the Ca {\sc{ii}} K and H$\beta$ observations have a spatial sampling of $0.138''$ pixel$^{-1}$. The total field of view of ROSA images is $69''\times69''$, centered at S12.4 W67.3 in heliographic coordinates. High-order adaptive optics \citep{rim} were applied throughout the observations to compensate for local seeing fluctuations.

The images were reconstructed by implementing the speckle algorithms of \cite{wog} followed by de-stretching.
These algorithms have removed the effects of atmospheric distortion from the data. The effective cadence after
reconstruction is reduced to about 9.238 s for H$\beta$, 2.3 s for Ca {\sc{ii}} K and 2.112 s for G band and continuum.
Moreover, the FOV is reduced as a result of the Speckle reconstruction algorithm, as an apodisation windowing function is applied to the images to reduce artefacts introduced by Fourier transforms. The FOV of the reconstructed images is subsequently reduced to $58.65''$ $\times$ $58.65''$.

\begin{figure}
\centering
\includegraphics[width=0.45\textwidth]{fig_goes_esp}
\includegraphics[width=0.45\textwidth]{fig_goes_esp_flare}
\caption{Upper panel: Emission recorded by GOES 1-8 \AA~ and SDO/EVE ESP quad detector 1--7 \AA~ on April 22, 2014. It should be noted that between 14:10 UT and 17:00 UT GOES data are missing.  Bottom panel: enlargement of the above panel, showing the details of the emission recorded by SDO/EVE ESP. In both panels the light blue and pink bands indicate the times of IBIS acquisition. The red and violet curves show the AIA 131 \AA~ emission of flares A and B, see Figure \ref{aialight}.}
\label{eve}
\end{figure}

\subsection{Space-based Observations}

Context images acquired with the Helioseismic and Magnetic Imager \citep[HMI,][]{Scherrer12} and the Atmospheric Imaging Assembly \citep[AIA,][]{Lemen12} instruments on-board the Solar Dynamics Observatory \citep[SDO,][]{Pesnell12} were used to provide general information on the magnetic field configuration and the morphology of the AR. Data from the quadrant diodes at 1--7 \AA~ of Euv SpectroPhotometer (ESP), part of the Extreme ultraviolet Variability Experiment \citep[EVE,][]{Woods12} on board of SDO were used to estimate the GOES classification of the flare.

In order to have information on the high energy flare emission we also used data acquired by the Reuven Ramaty High Energy Solar Spectrometer Imager (RHESSI; \cite{lin02}).

As described in the following section, a solar flare occurred in NOAA 12035, starting at 15:17 UT, peaking at 15:21 UT and ending at 15:30 UT. GOES data was not available for this event, however EVE/ESP data, represents a good proxy for GOES data and allows us to classify it as a C3.3 flare \citep{hock13}. It is important to hightlight that few minutes before, another flare occurred at the solar limb very close to NOAA 12035. To differentiate these events, we indicate with the letter B the C3.3 flare under analysis, while the letter A indicates the flare which occurred previously.

Full-disk continuum images and longitudinal magnetograms taken by HMI on board the SDO in the Fe I line at 6173 \AA~ with a resolution of $1''$ were used to complement the high-resolution data set of the ground-based instruments.

The SDO/HMI images were aligned, taking into account the solar differential rotation, by using the IDL SolarSoft package \citep{Freeland98}.

Data taken by the Atmospheric Imaging Assembly (AIA; \cite{Lemen12}) aboard the SDO mission were used to study in detail the temporal evolution of the flare in the coronal and upper
chromospheric layers. The AIA full Sun images were processed with the usual SSW \verb!aia_prep! routines \citep{BoernerEdwardsLemen:2012,BoernerTestaWarren:2014}. EUV and UV (1600 and 1700 \AA) images have a cadence of 12 and 24 seconds, respectively.

We reconstructed RHESSI CLEAN images using front detectors 3 to 8, for the energy ranges 6--9 and 12--25 keV\citep{HurfordSchmahlSchwartz:2002}. A sequence of 6--9 keV images with integration time of 32 seconds, stepping every 8 seconds, were constructed to obtain the light curves of flares A and B, as described in Section \ref{sect:data}.

\section{Data analysis} \label{sect:data}

\subsection{The flare evolution}
The first IBIS dataset (from 14:22 to 15:05 UT) shows many small brightenings in the wings of the H$\alpha$ line, probably Ellerman bombs occurring in a region of magnetic flux emergence \citep{ellerman,kurakowa,nindos}.
During the acquisition of the second data set (from 15:08 UT to 15:44 UT) in the south-west quadrant of the Sun two flaring regions were observed: a limb flare (flare A) in AR 12036 (start time 15:11:34 UT, end time 15:30:22 UT, peak time 15:16 UT) and a flare event (flare B) in AR 12035 (start time 15:17 UT, end time 15:30 UT, peak time 15:21 UT).

\begin{figure}[!b]
\centering
\includegraphics[scale=.53]{flareab}
\caption{AIA 131 \AA~ image (reverse color) overlapped with the RHESSI contours in the 6-9 keV range, showing the location of flares A and B (see text).}
\label{aialight}
\end{figure}

\begin{figure}[!t]
\centering
\includegraphics[width=0.48\textwidth]{rhessiaia}
\caption{From top to bottom: RHESSI counts (full Sun), AIA 131 \AA~ emission of flares A and B along with RHESSI emission derived from images; AIA emission from each EUV and UV channel for flare B.}
\label{aialight1}
\end{figure}

\begin{figure}[!b]
\centering
\includegraphics[scale=.45]{fig_source1.pdf}
\caption{AIA 1600 \AA~ image acquired at 15:22:40 UT overlapped with the HMI line-of-sight magnetic field (red: negative field, -2000, -1000, -500, -200, -100 G, blue: positive field, 100, 200, 500, 1000, 2000 G).}
\label{ab}
\end{figure}

\begin{figure}[!h]
\centering
\includegraphics[scale=.5]{fig_rhessi_map_12_25}
\caption{AIA 94 \AA~ image (reverse color) overlapped with the RHESSI emission contours in the 12--25 keV range. The purple dashed circle indicates the region of interest (ROI).}
\label{ab1}
\end{figure}

These two flares, therefore, overlap in time, making it difficult to use full Sun data, like, for instance, the RHESSI full Sun spectral analysis or the SDO/EVE. However, using AIA and RHESSI's imaging capabilities, it is possible to infer the contributions from each flare and retrieve some information. GOES data are not available, therefore, we used the EVE/ESP quadrant diode 1--7 \AA~ as proxy (see Figure \ref{eve}).

We used the AIA 131 \AA~ channel as a reference to distinguish the two flares, because this AIA channel has a temperature response close to the plasma temperatures that can be observed by RHESSI at low energies. We were able to image each flare independently with RHESSI, as shown in Figure \ref{aialight}. To evaluate how each flare evolves, we defined a box around the location of each flare (dotted-boxes in Figure \ref{aialight}) and obtained the average emission in the AIA 131 \AA~ channel (in DN s$^{-1}$ pixel$^{-1}$).

In Figure \ref{aialight1} we show, from top to bottom: RHESSI counts (full Sun), AIA 131 \AA~ emission of flares A and B along with RHESSI emission at 6-9 keV derived from the images; AIA emission from each EUV and UV channel for flare B. The peak in the AIA 131 \AA~ channel occurs at 15:16:20 UT and 15:21:44 UT for flares A and B, respectively. From the AIA 131 \AA~ emission in the second panel of Figure \ref{aialight1} it is clear that the gradual phase of flare A extends during the impulsive phase of flare B. Therefore, we cannot use RHESSI full Sun spectroscopic analysis to study flare B.

The analysis of the IBIS and ROSA dataset allows us to follow the flare evolution in the chromosphere, which is mainly characterized by a loop-like structure with a cusp at its top (see, e.g., the right panel of Figure \ref{ibis_con}) oriented towards the south-west. The distance between the two footpoints, as determined from the IBIS H$\alpha$ image acquired at 15:24 UT (see Figure \ref{ibis_con} \textit{right} panel), is 11500 km and, assuming a semi-circular shape for the loop-like structure, this has a length of $\sim$ 18000 km.

\begin{figure*}
\centering
\subfigure{\includegraphics[trim=80 90 90 90, clip,width=0.28\textwidth]{map_cont2}}
\subfigure{\includegraphics[trim=80 90 90 90, clip,width=0.28\textwidth]{map_ibis2}}
\subfigure{\includegraphics[trim=80 110 110 110, clip,width=0.28\textwidth]{map_rosa2}}
\caption{(a) Image acquired in the IBIS continuum at 6610 \AA; (b) IBIS H${\alpha}$ image of the same FOV (reversed color); (c) ROSA H${\beta}$ image (inverted color) after the alignment procedure with the IBIS corresponding image. The boxes in (b) and (c) indicate the regions A, B, C and D that are used to determine the intensity evolution (see Figs. \ref{abcd} and \ref{ratio}).}
\label{align}
\end{figure*}

Comparing with continuum images (see Figure \ref{ibis_con}, \textit{left} panel), it is possible to establish that the flare developed between the large (western) sunspot and a small pore located at the center of the FOV. The large arch filament system (AFS) connecting the other two main sunspots does not seem to show any variation during the flare.

In Figure \ref{ab} we show an AIA 1600 \AA~ image acquired at the peak of the flare, with the overlapped contours (levels indicated in the figure caption) denoting the longitudinal magnetic field deduced from the HMI instrument. We notice that the cusp region, also observed at 6563 \AA~ (compare with Figure \ref{ibis_con}, \textit{right} panel), is quite evident, while the bright footpoints seem to be both located in regions of positive magnetic field, which is due to projection effects due to the proximity of the AR to the western limb.

The comparison between the AIA 94 \AA~ image acquired $\sim 1$ minute before the flare peak (see Figure \ref{ab1}) and the RHESSI 12--25 keV contours indicate that there are two main sources of hard X-ray emission: the location of one corresponds to the flaring loop-like structure, the other is superimposed on another bright structure to the east of the flaring loop. It is worth noting that this feature was not in the IBIS and ROSA FOVs.

\subsection{H${\alpha}$ - H${\beta}$ comparison}

We further investigate the flare event through the comparison between H${\alpha}$ and H${\beta}$ images acquired by IBIS and ROSA, respectively. In fact, although this event is not very energetic and it is very close to the limb, the combined dataset is unique because it has both H${\alpha}$ and H${\beta}$ imaging.

Due to the fact that the images obtained by the two instruments have different size and spatial resolution, we first need to align the H${\alpha}$ and H${\beta}$ images. To this aim, we use the USAF target images and dot grid images (see, e.g., \citealt{kleint}), because the sample is the same during the observing campaign and, furthermore, they were simultaneously acquired in the two channels.
Through them it was possible to calculate the parameters to rotate, rescale and shift
the images in order to obtain the correct alignment between H${\alpha}$ and H${\beta}$ images. Once obtained these parameters they have been applied
to the IBIS dataset, i.e., the H${\alpha}$ images. Figure \ref{align} shows the result of the alignment procedure: the images have the same orientation, size (456 $\times$ 478 pixels) and
spatial sampling ($0.138''$ pixel$^{-1}$).

After the alignment we compared the lightcurves of these two chromospheric lines in four boxes inside the field of view indicated in Figure \ref{align} ((b) and (c) panels). Three of these boxes (A, B and C) are
on the bright areas of the flare, while the last one (box D) is on a bright patch outside the flaring region. The boxes have the same size, i.e., 40 $\times$ 40 pixels ($\approx$ $5.5''$ $\times$ $5.5''$). We choose a box of this size to avoid to lose information during the flare brightness evolution. We note that the locations of the flare emission inside the boxes are not fixed in space but they moved during the evolution of the event. We obtained the lightcurves of H${\alpha}$ and H${\beta}$ by taking the average intensity values calculated over all pixels inside each box. Moreover, to better compare the intensities acquired with the IBIS and ROSA instruments, we calibrated the intensity obtained by the different cameras from DN to erg s$^{-1}$ cm$^{-2}$ \AA$^{-1}$ sr$^{-1}$ units as follows: we determined the flat-field image intensity acquired on the day of observation with both IBIS and ROSA cameras and, assuming that this flat-field intensity was equal to the values provided in the Brault \& Neckel Atlas \citep{brault}, we converted the measured intensity in DN to fundamental units. We reiterate here that the cadences for the reduced H${\alpha}$ and H${\beta}$ datasets are around 2.6 s and 9.2 s, respectively.

Figure \ref{abcd} shows the intensity as a function of time deduced from H$\alpha$ (black) and H$\beta$ (orange) images for the four boxes. In particular, the intensity relative to the H$\alpha$ line, has been determined by averaging the intensity at the center of the line (6562.8 \AA) and in an adjacent point along the line profile (6562.9 \AA) covering a total $\Delta \lambda = 0.1$ \AA, comparable to the bandwidth of the H$\beta$ filter employed with the ROSA instrument. However, because the cadence of H${\alpha}$ images was higher than H${\beta}$ data, the sampling to determine the H${\alpha}$ intensity was greater. To highlight the energy released during the flare, the intensity of all the lightcurves were obtained by subtracting the pre-flare intensity calculated by averaging the intensity in each box during 2 minutes in a time interval before the flare, i.e., from 15:10:00 UT to 15:12:00 UT.

\begin{figure}
\centering
\includegraphics[width=0.47\textwidth]{box_multi_last2
\caption{Average intensity (after subtraction of the pre-flare intensity, see text) as a function of time deduced from H$\alpha$ (black) and H$\beta$ (orange) data in the three boxes located into the flare location (A, B and C) and in a box outside the flaring region (D). The vertical black lines show the estimated start (dashed) and peak (solid) times of the flare. The co-temporal drops in the end of sequence are related to the bad seeing conditions.}
\label{abcd}
\end{figure}

The analysis of these plots indicates that the intensity excess of the H$\beta$ line is generally higher than the H$\alpha$ intensity during the impulsive phase of the flare, in particular the former can reach values up to $\sim 0.3 \times 10^{6}$ (box A), $\sim 1.8 \times 10^{6}$ (box B) and $\sim 1.1 \times 10^{6}$ (box C) erg s$^{-1}$ cm$^{-2}$ \AA$^{-1}$ sr$^{-1}$, while the latter reaches value of $\sim 0.2 \times 10^{6}$ (box A),  $\sim 0.7 \times 10^{6}$ (box B) and $\sim 0.5 \times 10^{6}$ (box C) erg s$^{-1}$ cm$^{-2}$ \AA$^{-1}$ sr$^{-1}$ (see the first three panels of Figure \ref{abcd}).
The lightcurves obtained in the box D appear flat for both the lines during all time of analysis (see the bottom panel of Figure \ref{abcd}). In the same plot the vertical black lines show the estimated start (dashed) and peak (solid) flare times deduced by EVE/ESP.

The ratio of the two core spectra intensities has potential diagnostic importance for the comprehension of chromospheric flares \citep{kaspa09}. In order to detect any possible signature of different emission among the two wavelengths, we calculated the ratio between the H$\alpha$ and the H$\beta$ intensity for all the boxes in which we applied an 11-point smoothing function in order to remove the excess noise. The values of ratio have been calculated on the common acquisition time of the two instruments, namely from 15:10 UT to 15:45 UT. The bottom panel in Figure \ref{ratio} presents the temporal evolution of this ratio, where the different colours indicate the intensity ratio obtained for each box (see legend). In the same figure the intensity of the H$\alpha$ (top panel) and H$\beta$ (middle panel) lines as a function of time for each box is reported. Figure \ref{ratio} shows that the two chromospheric lines respond to the flare energy input in the same way, highlighting a similar shift between peaks in intensity and an energy distribution comparable with the corresponding box. Specifically, the H$\alpha$ lightcurves of boxes A, B and C have similar behaviour, with a similar peak in intensity and similar decay phases. Similar behaviour, albeit with different values of intensity is seen in the corresponding H$\beta$ lightcurves.

\begin{figure}
\centering
\includegraphics[width=0.47\textwidth]{ratio_multi_last1
\caption{Temporal evolution of the H$\alpha$ excess intensity (top panel) and the H$\beta$ excess intensity (middle panel) in boxes A, B, C and D indicated in Figure \ref{align} (b)-(c)). The bottom panel shows the temporal evolution of the ratio H$\alpha$/H$\beta$. Different colours indicate different boxes (see the legend in the plot). The vertical black lines show the estimated start (dashed) and peak (solid) flare times.}
\label{ratio}
\end{figure}

The bottom panel in Figure \ref{ratio} shows that the H$\alpha$/H$\beta$ intensity ratios during the flare tends to a constant value for the boxes inside the flaring region (approximately around 0.4 for the boxes B and C and around 0.8 for the box A), while before and after the flare the values are generally higher, with a variable trend for all the boxes. Outside the flaring region (box D) the ratio is highly unstable with large oscillations before, during and after the energy input, due to the low values of the intensity that cause large errors.

\subsection{Spatial offset}

Following the aim of the observing campaign, to evidence a possible spatial offset among each chromospheric sources, we looked at the maximum intensity value inside the corresponding box (note, it is possible that this location will not occur exactly in the same pixels for both H$\alpha$ and H$\beta$ channels). In Figure \ref{distance} we report the spatial offset as a function of time between the brightest points in the H$\alpha$ and H$\beta$ line cores for boxes A and B and the offset between the brightest points in the H$\alpha$ core and H$\alpha$ continuum wing. We display the results only for boxes A and B because they are more relevant as they are located in the footpoints of the flare loop. The analysis of this plot shows a spatial offset in the range of $2''$--$3''$ between the sources imaged in the H$\alpha$ and H$\beta$ line cores, but in the box A this offset decreases to $0.2''$ after the impulsive phase of the flare, while remains constant for the Box B. The distance between the brightest points observed in the H$\alpha$ core and H$\alpha$ wing is constant for box A around a value of $3''$, while it varies in a range of $1''$--$5''$ for box B.

\begin{figure}
\centering
\includegraphics[width=0.4\textwidth]{distance_last1
\caption{Temporal evolution of the offset of the brightest points imaged in the H$\alpha$ and H$\beta$ line cores inside boxes A, B (solid lines). The dashed lines indicate the same, but for H$\alpha$ core line and H$\alpha$ wing.}
\label{distance}
\end{figure}

\subsection{Evolution of H$\alpha$ line profile}

In order to investigate the temporal evolution of the H$\alpha$ line profile and to compare it with the simulations shown in Section 4, we selected a time interval of 10 minutes during the flare evolution, starting at 15:15:50 UT and calculated the average intensity in each point of the line acquired by IBIS (it should be noted that a similar analysis for the ROSA H$\beta$ dataset could not be performed because in this case we only have images in the line center). Again, this analysis was only carried out for boxes A and B.

Figure \ref{haprof} (\textit{left} panel) displays that in box A the H$\alpha$ line shows a stronger increase in the red wing, compared to the blue wing, and that the line core is shifted blueward. In box B, the line exhibits both red and blue wing enhancements (see Figure \ref{haprof}, \textit{right} panel). The core is more enhanced than in box A but it does not go into emission. In box B the core shows a very small red-shift during the rise phase (up to 200 seconds, see Figure \ref{haprof}, \textit{right} panel), shifting to shorter wavelengths afterwards.
In both boxes A and B, the line does not show a central reversal. \citealt{Deng} reports similar observations, in contrast to typical observations of the H$\alpha$ line profile \citep{Canfield90,delab,KuridzeMathioudakisSimoes:2015}.

\begin{figure*}[htb]
\centering
\includegraphics[width=0.90\textwidth]{profile_multi_box_last
\caption{Temporal evolution of the observed H$\alpha$ profile in box A (left) and box B (right). The intensities are reported in absolute units. Different colours indicate different times (from black, through blue and green to dark red). The dashed profile results from the average intensity in each box at the beginning of the observing sequence.}
\label{haprof}
\end{figure*}

\section{RADYN Simulations}

We used the radiative hydrodynamic code RADYN to compute the H$\alpha$ and H$\beta$ line profiles and to calculate the intensity ratio of the line cores for comparison with the observations.
Our idea is to adopt a model closest to observations features, whereby we used the RHESSI imaging spectroscopy integrating over 2 minutes during the main impulsive phase (15:20:00 -- 15:22:00 UT). Figure \ref{rhessi_spec} shows RHESSI photon spectra for the HXR source spatially integrated over the region of interest (ROI) displayed in Figure \ref{ab1}. The spectra were fitted with an isothermal plus thick-target model, shown in Figure \ref{rhessi_spec} with orange line, and the resulting parameters are: emission measure EM=1.3$\times$10$^{46}$ cm$^{-3}$; plasma temperature $T$=13 MK; number of electrons per second injected F=2$\times$10$^{35}$ electrons s$^{-1}$ above E=E$_c$=7 keV; spectral index $\delta$=6.4; total non-thermal power P$_{nth}$=2.7$\times$10$^{27}$ erg s$^{-1}$ and the total non-thermal energy E$^{tot}_{nth}$=3$\times$10$^{29}$ erg. From these parameters, two RADYN simulations were employed here, the first one, marked by F9.5, with a peak of energy flux of F$^{max}_{F9.5}$ = 3$\times$$10^{9}$ erg cm$^{-2}$ s$^{-1}$ and a total amount of energy F$^{tot}_{F9.5}$ = 0.3$\times$$10^{11}$ erg cm$^{-2}$; the second one, indicated by F10, with a peak of F$^{max}_{F10}$ = $10^{10}$ erg cm$^{-2}$ s$^{-1}$ and a total amount of energy  F$^{tot}_{F10}$ = $10^{11}$ erg cm$^{-2}$. For both the runs a beam with an isotropic pitch angle distribution in the forward hemisphere was used with the Fokker-Planck solution to the non-thermal electron distribution \citep{AllredKowalskiCarlsson:2015}. A triangular pulse shape heating flux was applied for 20 seconds (with peak after 10 s), and the atmosphere was allowed to relax for 15 additional seconds. The initial atmosphere before the switch-on of the beam was the VAL3C semi-empirical atmosphere \citep{Vernazza}. The electron beam energy distribution is defined as a power-law with a spectral index of $\delta$ = 6 and a low energy cut-off E$_{c}$ = 10 keV. Considering the location of the flare on the solar disk, to simulate the projection effect we used $\mu$=0.23 in both F9.5 and F10 runs.

\begin{figure}[ht]
\centering
\includegraphics[width=0.47\textwidth]{figspex.pdf}
\caption{RHESSI photon spectra for the HXR over the ROI indicated by purple dashed circle in the Figure \ref{ab1} and integrated for the interval 15:20:00 -- 15:22:00 UT. The orange line is the isothermal plus thick-target model. The isothermal model is the green line, defined by two parameters: emission measure EM and temperature $T$ (see text). The non-thermal thick-target model is the blue line, defined by three parameters: low energy cut-off E$_c$, spectral index $\delta$ and total number of electrons per second above E$_c$.}
\label{rhessi_spec}
\end{figure}

Using the H$\alpha$ and H$\beta$ lines profiles calculated with RADYN, we computed the ratio of the line core intensities, $\lambda=6563$ \AA~ for H$\alpha$ and $\lambda=4861$ \AA~ for H$\beta$, for both models F9.5 and F10, the results of which are shown in Figure \ref{ratiohahb1}. In both models, for the duration of the energy input, the ratio of H$\alpha$ to H$\beta$ is smaller than 1. In F10 the ratio starts around 0.6--0.7 then settles at 0.4 after 10 s, very similar to observed ratios of boxes B and C, while in F9.5 the ratio swings between 0.6--0.8, closer to the observed ratios of box A which is the weakest flare kernel.

\begin{figure}[htb]
\centering
\includegraphics[width=0.5\textwidth]{hahb_fchroma_grid_ratios}
\caption{Time evolution of the intensity and the ratio of the core in the H$\alpha$ and H$\beta$ lines, for the F9.5 and F10 models (see legend). The black dotted lines show the shape of the energy input.}
\label{ratiohahb1}
\end{figure}

Figure \ref{simhahb1} shows the temporal evolution of the synthesised H$\alpha$ line profile for both F10 and F9.5 flare models. In the F9.5 model, the line, initially in absorption, goes into emission with a clear presence of a central reversal. Through the duration of the energy input, the line wings around $\Delta \lambda \approx -0.5$ are much more pronounced than the line core. During the first 15 seconds of the energy input, the entire line profile is shifted towards longer wavelengths, with the blue wing being stronger than the red wing. From then until the end of the energy input at $t=20$ s, the line shifts slightly redward from the rest wavelength and the wings are more symmetric. When the energy input stops, the intensity of the wings and core decrease substantially, a red-wing asymmetry appears and the core is shifted $\Delta \lambda > 0$.

In the F10 model, the line also goes into emission with a central reversal, with a much more pronounced intensity of the line core with respect to the wing intensities, compared to the F9.5 model. As noted by \cite{KuridzeMathioudakisSimoes:2015}, a red wing asymmetry (i.e., the red wing intensity stronger than the blue wing) develops in the first 5 seconds, before reverting to a blue wing asymmetry after that time. The line core shifts to opposite directions: blueward and then redward. The wing asymmetry is created by an excess of absorption by the moving plasma above the height of formation of the H$\alpha$ line, as pointed out by \cite{KuridzeMathioudakisSimoes:2015}, i.e., a red asymmetry does not necessarily indicate the presence of downward moving plasma, nor does a blue asymmetry indicate upwardly moving plasma. When the energy input ends, the line intensity drops rapidly, the wings become much less pronounced (even disappearing) but the line remains in emission until the end of the simulation.

The synthetic H$\alpha$ line profiles obtained from the RADYN simulations are different from the profiles observed with IBIS, as described earlier. The line profiles in both boxes A and B remain mostly in absorption throughout the event, with a stronger increase in the core intensity than the wings intensities.

It is possible that not all the pixels inside the box are activated by the flares, so the ''filling factor'', defined as \textit{ff}=1/$(N+1)$, is smaller than 1. We have tried to simulate this filling factor effect with the RADYN lines by averaging $N$ times the pre-flare line profile with the flaring lines, namely $I_{\textit{ff}} = \textit{ff}  (I_\mathrm{flare} + NI_\mathrm{pre-flare})$. In practical terms, this brings the calculated lines closer to the observed line shape. For both F9.5 and F10 models, we found solutions that qualitatively reproduce the observations: $N_\mathrm{F9.5}$=2 and $N_\mathrm{F10}$=5 with the filling factor values \textit{ff}$_{F9.5}$=0.333 and ff$_{F10}$=0.167. Figure \ref{simhahb2} shows the line profiles using that filling factor. The plots display that the line is in absorption, prior to a small enhancement of the wings around $\Delta \lambda \pm$1.0 \AA. In F10 there is a small enhancement at $\Delta \lambda \pm $1.0 \AA, and in F9.5 the blue-shift of the line core follows closer the observations than F10. In absolute values of $I_\lambda$, F10 gives a better agreement in $I(\Delta \lambda=0)$, with F9.5 being too weak.

\begin{figure}[ht]
\centering
\includegraphics[width=0.5\textwidth]{hahb_fchroma_grid_lineprofile_00}
\caption{Time evolution of the H$\alpha$ line profile calculated with RADYN, for the F9.5 (top) and F10 (bottom) flare models.}
\label{simhahb1}
\end{figure}

\begin{figure}[ht]
\centering
\includegraphics[width=0.5\textwidth]{hahb_fchroma_grid_lineprofile_01}
\caption{Same as Figure \ref{simhahb1}, but simulating a filling factor \textit{ff} smaller than 1 (see text). Top: F9.5 model, \textit{ff}=0.167. Bottom: F10 model, \textit{ff}=0.048.}
\label{simhahb2}
\end{figure}

Note that with H$\beta$ we do not have line scans as we do with H$\alpha$. The H$\beta$ images are from the core of the line, and have a relatively broad filter width in comparison to the H$\alpha$ scans. Therefore, RADYN simulation can not be used for a direct comparison for the H$\beta$ images.

We used the F9.5 and F10 to qualitatively explore a weak and a strong case. To determine which of the two runs is closer to observations we have to derive the total amount of energy injected in the two models. RADYN solves equations along one dimension, but the observation results are related to boxes of two dimensions. Our idea is to translate the filling factor discussion in an area value in order to obtain a size for the flaring elements. Comparing the observed and synthetic H$\alpha$ lines profile (see Figure \ref{haprof} and \ref{ratiohahb1}) we obtained a different value of filling factor from F9.5 and F10 runs. Knowing the size of box used in the observations ($5.5''\times5.5''$), we can easily convert them to a simulated flaring area: $\approx 3.2''\times3.2''$ for F9.5 and $\approx 2.2''\times2.2''$ for F10. To estimate the projection effect, from the location of the flare source on the solar disk we obtained $\mu$=0.3 and, using this value, the effective flaring areas are then A$^{eff}_{F9.5}$=17.5$\times$10$^{16}$ cm$^2$ and A$^{eff}_{F10}$=8.8$\times$10$^{16}$ cm$^2$.
From the RHESSI photon spectra fit parameters and using the effecive flaring areas we found F=P$_{nth}$/A$^{eff}_{F9.5}$$\approx$0.15$\times$10$^{11}$ erg s$^{-1}$ cm$^{-2}$ and F=P$_{nth}$/A$^{eff}_{F10}$$\approx$0.31$\times$10$^{11}$ erg s$^{-1}$ cm$^{-2}$. The real problem here is that the RHESSI values are derived from the whole flare (see the ROI in Figure \ref{ab1}), not just one source (box), but anyway the F9.5 model appears closer to the observations.

\section{Conclusions}

The aim of this work was to clarify some aspects related to energy release and redistribution in the chromospheric layer of the solar atmosphere during a solar flare. Therefore, we investigated the chromospheric response to the sudden energy input, locating the sources, the sizes and the eventual offset between flare sources in different wavelengths. Our approach was to look at the features of two chromospheric lines during a C3.3 solar flare, using high resolution ground-based data  acquired during an observing campaign carried out at Dunn Solar Telescope. Although the location of the flare on disk was not ideal and the intensity of the event was relatively low, the uniqueness of this dataset in terms of the resolution (both spatial and temporal), the lines used (both H$\alpha$ scans and H$\beta$ core images) and the fact that all phases of the flare were observed, provides novel insights into the behaviour of the cromosphere during a flare.

In a previous work, \cite{kaspa09} simulated Balmer lines during impulsive flare heating and investigated the correlation between H$\alpha$ and H$\beta$ lines. The authors tried to use H$\alpha$/H$\beta$ ratio to check whether they are sensitive to electron beam presence, i.e., whether they are significantly different if the non-thermal collisional rates are included in the simulations.
In this paper we displayed the lightcurves from observed H$\alpha$ and H$\beta$ lines, where, in the flaring region, the H$\beta$ intensity excess is greater than those of H$\alpha$ during the flare energy input, as noted by \cite{kaspa09}.

We employed the radiative hydrodynamic code RADYN to compute the synthetic H$\alpha$ and H$\beta$ line profiles to compare them with our observations. For both F9.5 and F10 runs the H$\beta$ intensity is greater than H$\alpha$, while the intensity ratio is around 0.4 in the F10 model after the energy peak, which is in agreement with the observed ratios for the different regions of the flare. Similar ratios from different inputs implies that the H$\alpha$ and H$\beta$ lines are affected similarly by the amount of energy and this indicates that this ratio is sensitive to the amount of energy deposited in the chromosphere.

Our results for the line ratios are in agreement with the findings of \citet{kaspa09}. In \cite{kaspa09}, Flarix gives intensities in erg s$^{-1}$ cm$^{-2}$ Hz$^{-1}$ sr$^{-1}$ and also line ratios are computed from those values, while in this paper we used erg s$^{-1}$ cm$^{-2}$ \AA$^{-1}$ sr$^{-1}$ as $I_\lambda$ units. As confirmed by private communication with the authors, the ratio should be around 0.5 after adjusting to the same units of $I_\lambda$ used in this paper, very close to our results.

Furthermore, by comparing the observed and synthetic H$\alpha$ line profile evolutions, there is good agreement using a ''filling factor'' approach. The simulated H$\alpha$ profiles present a clear central reversal, while the observed line profiles were enhanced during the flare, but remained mostly in absorption. We have interpreted the weakly-enhanced H$\alpha$ line profiles as an effect of a low filling-factor, estimated to be \textit{ff} $\approx$ 0.33 or \textit{ff} $\approx$ 0.17, using models F9.5 and F10, respectively. The simulated intensity ratios, with the pre-flare level subtracted, for the low filling factor cases yield values in the range 0.4--0.5. This is simply because the same filling factor was applied for both H$\alpha$ and H$\beta$ line profiles. Furthermore, converting the filling factor in terms of flaring area we obtained values of total energies for F9.5 and F10 models, indicating the F9.5 closer to the observations.

Concerning the analysis related to the spatial offset, because the flare is located close to the limb, we can read the results as diagnostic of the formation heights of the two line-cores. Figure \ref{con_f} displays the line contribution functions \citep{carlsson97} after 10 s of F9.5 flare input, where the H$\alpha$ core formation height is higher of about 40 km with respect to the H$\beta$ core (wings formation heights are the same). The observed spatial separation is in qualitative agreement with the RADYN simulation, the observed spatial offset is much larger but this may be due to one dimensional limit of RADYN code, so it's hard to make an actual comparison with imaging observations. Therefore, a possible suggestion for future observations in both spectral lines would be to search for flaring active regions very close to the solar limb, in order to further investigate the spatial offset.

\begin{figure}[ht]
\centering
\includegraphics[width=0.22\textwidth]{fig_hahb_cf_ha76}
\includegraphics[width=0.22\textwidth]{fig_hahb_cf_hb_76}
\caption{Intensity contribution functions for the H$\alpha$ (left) and H$\beta$ (right) lines after 10 s of F9.5 flare heating. The diagrams are plotted in inverse grayscale so that darker shades indicate higher intensities. The line profile is overplotted as a blue line. Red lines indicate the height at which $\tau$=1. Positive velocity corresponds to plasma upflows.}
\label{con_f}
\end{figure}

\acknowledgments

The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 606862 (F-CHROMA). This research has received funding from the European Commission's Seventh Framework Programme under the grant agreement no. 312495 (SOLARNET project). The IBIS and ROSA data analyzed in this paper were acquired in the framework of SOLARNET service mode. This work was also supported by the Italian MIUR-PRIN grant 2012P2HRCR on The active Sun and its effects on space and Earth climate, by Space Weather Italian COmmunity (SWICO) Research Program, by the Istituto Nazionale di Astrofisica (PRIN INAF 2010/2014), and by the Universit\'a degli Studi di Catania.

PJAS and LF acknowledge support from grant ST/L000741/1 made by the UK's Science and Technology Facilities Council.

This research was supported by the Research Council of Norway through the grant ''Solar Atmospheric Modelling'' and through grants of computing time from the Programme for Supercomputing.

The RADYN models used in this work are part of the F-CHROMA database of solar flare models, available at \url{www.fchroma.org}, under "data access". We would also like to thank Jana K\v{a}sparov\'{a} for discussing their 2009 results in detail.

redpajama_set_name: RedPajamaArXiv


This class prepares Java™ programmers to develop interoperable Java Web services and using SOAP, WSDL, and XML Schema. Students get an overview of the interoperable and Java-specific Web services architectures, and then learn the standard APIs for SOAP messaging and WSDL-driven, component-based service development. Both document-style and RPC-style messages and services are covered in depth.
Attendees receive more than 400 pages of comprehensive courseware and a copy of Addison-Wesley's J2EE Web Services.
Java EE application server or servlet/JSP container of the attendees' choice, with web services support. If none has been chosen, we recommend Tomcat [http://tomcat.apache.org] with Axis [http://ws.apache.org/axis/] installed.
The Java IDE of your choice. If none has been chosen, we recommend Eclipse [http://www.eclipse.org] or NetBeans [http://www.netbeans.org].
Expose session beans as web services.


No reviews for Nitro Super Sonic 1/7 Scale Pre-Painted Figure: Super Sonico Cowgirl yet.
the price for Nitro Super Sonic 1/7 Scale Pre-Painted Figure: Super Sonico Cowgirl drops.
Nitro Super Sonic 1/7 Scale Pre-Painted Figure: Super Sonico Cowgirl is available.
there are new images or links available for Nitro Super Sonic 1/7 Scale Pre-Painted Figure: Super Sonico Cowgirl.
Vertex releases a new product.


Poll: Would you change your name after marriage?
I would probably have it double-barreled so I still get to keep my surname.
I got married three years ago and changed my name to my husbands. I also changed the name I work under and the name that I have registered with my professional body. I did spend a lot of time thinking about the options for what to do with my name.
I decided quite quickly against double barrelling mostly because the combination of our two names is really silly. I also considered just keeping my maiden name however I grew up in a family where my married parents each kept their own name and I didn't like the fact that my mum had a different name to me. I also don't have a huge issue with taking my husbands name as I don't have a real attachment to my maiden name (very common).
At the end of the day none of these are huge reasons but they tipped the balance to me choosing to change my name. I haven't regretted it since and it has made things easier since having our son as I have the same surname as him.
I hate my surname so yes. My brother is jealous I'm a girl who can just get married and take a different surname, because, you know, finding someone to marry is soooo easy! That said, if I did a significant amount of work using my maiden name I may keep it for work.
I love silly double barrelled names! My friend suggested me and my ex got married to become the 'Bland-Munton's which is clearly horrific.
Ours would have been colour-type of food!
I quite like the idea of picking an entirely new name. Avoids this issue and symbolises a new part of life beginning.
Thanks for the correction, however, in the bit you quoted you can still see how that applies to only spouse or civil partner. If you're not married you get nothing. If you're unmarried but have children, I suppose it'll go to the children anyway and you can get your share back from them - but what if you don't have kids yet? THen you've got no rights.
Yes, I'm sure there are ways around all these things without marriage, but simply marriage does it all for you. So why not get married, and just do things how you want (keep your name if you want, etc)?
What I meant to express was the fact that marriage does not do it all for you. Whether you are married or not you need to write a will.
Married people, because the rules of intestacy preclude the spouse from inheriting all the estate and of course give no indication of any specific gifts. Unmarried people of course need to write a will to express their wishes. On the other hand marriage may stop you from leaving your estate where you will as a spouse may appeal through the courts if they are excluded.
In monied families assets are often held within trusts which may be there precisely to stop a spouse inheriting the capital and thus alienating it from the family.
In addition nowadays people may have property abroad and marriage, will or no will, may not help you at all as the rules of that country will apply. So, in France, I believe, the property goes to the children. British people often expect that inheritance rules are the same abroad as here and it comes as nasty shock when they discover they are not even in ex colonies.
The point though is that, since most people don't have a will when they get married, the marriage makes a difference. It changes it from your partner gets nothing to your partner gets something. I believe the original post being discussed had said that marriage makes no legal difference to anything.
For me it's not a choice between dad's name or partner's name because my mother wasn't willing to give me my father's surname so I have the surname of my mother, her mother, and her mother. I kind of like that. Four generations.
But yeah, I'll take the name of the man I want to marry.
Hmm, never thought of that before.
Thatn would be quite cool actually.
wait a min.... Does this mean anarchism101 is female?
What's up with the kisses?
The idea is that the couple picks a new name for them both to change to so I don't think it's a suggestion that anarchism101 is female.
I've briefly thought about the idea (the new name), but I really can't think of one that would sound both normal enough and special/meaningful enough for us to change our names for it. It just feels like stealing someone else's name, or picking one randomly that can't possibly be 'the best' out of all the possible names. I think especially that it wouldn't work here in Denmark - we would likely want a Danish name (well, I'm assuming that we would, anyway), and they're mostly patronymic. Let's say my other half's name is Hansen (it's not) - while there hasn't been a 'Hans' in his family in living memory, it would seem weird to change our names to Jespersen or Mathiesen instead - who the **** is this Jesper or Mathias we're naming ourselves after? My dad is called Peter, shall we call ourselves Petersen? (Answer: No, because that would be creepy and my other half's dad is not called Peter, obviously).
I end every post with kisses, it's like part of my signature... Unless I really dislike someone's posts. Partly it's habit. Also, it shows that I don't have a malicious intent with messages that are part of debates or question something, since it's so easy to misread intent on a forum but it would be a bit odd to only add them to posts that were ambiguous and not those which are clearly nice.
Now I'm self conscious about it!!!
I thought I was getting special treatment.
At least it means I don't really dislike your posts!
Is it possible to change your last name to your mums maiden name?
Why do women change their name when they get married?


Metallica performed Lincoln Financial Field in Philadelphia on May 12, and broke out an extended version of "Now That We're Dead" with the whole band on drums! Skip to about 6:20 within the video, where the music breaks down in a giant drum jam, complete with big drums for everybody in the group.
8-Year Olds Prove You Are Never Too Young To Rock With Amazing Cover Of "Enter Sandman"!


Built by racers. Driven by purists.
In 1967, two A10:D65 engineers with a passion for motorsports began fine-tuning engines for Mercedes-Benz racecars in an old mill. Today, as the performance division of Mercedes-Benz, AMG creates some of the most sought-after vehicles in the world. They're the product of skilled craftsmen, designers and engineers who live to test the limits, and one shared conviction: on the road to driving performance, short cuts never win the race.
Whether it's the hand-built craftsmanship of the "One Man – One Engine" philosophy or the ever-advancing technological leadership of the latest biturbos, an AMG engine is developed not just to perform, but to outperform. But it's just one of many high-performance weapons in our engineering arsenal.


text:
6 'New 52' titles cancelled, 6 new titles out this month
By orlouge82,
April 4, 2012 in Community
orlouge82
Seven of DC's "New 52" titles have been cancelled (presumably due to low sales)
Hawk and Dove
Mister Terrific
O.M.A.C.
Static Shock
I think that this news is months old already, but I just discovered this fact this morning when I was checking on my titles.
I'm particularly upset about "Static Shock" and "Mister Terrific," but probably more so about the former. Static was the brainchild of the late Dwayne McDuffie (who also did story work for the DCAU series Justice League and Justice League Unlimited), and it makes me bummed to see Static fail so soon after it started.
On the other hand, "Blackhawks" is one title that I'm not sad to see go. I started reading the title when it first came out, but by issue four or five, I just couldn't read it anymore.
Anyhow, any comic readers out there sad about any of these titles going away?
DarkeSword
It's only six. You have Hawk and Dove listed twice.
Also how can you not like Blackhawks? Blackhawks was awesome. So sad to see it go.
I wasn't reading any of the other books though. Not surprised to see Hawk and Dove go, considering it's Liefeld's art, but the real puzzler is that now that H&D is over, Liefeld's working on three books for DC.
Static's failure as a title had mostly to do with a creative and editorial team that did not get along. A shame, really; Static's a great character.
I'm more excited for the Second Wave of titles that's coming in to fill in the space, like Earth 2, World's Finest, Batman Incorporated and The Ravagers. Dial H for Hero and GI Combat don't sound very interesting to me.
Fix'd
I don't know, I guess Blackhawks started turning me off when it started getting so much into the government bureaucracy stuff. Just starting taking a turn for the formulaic to me. Personal preferences, I suppose. Kind of the same reason I wasn't terribly into JLI at first, but now most of the government guys went kaboom, so I'm curious to see where it goes from there.
Interesting about Static's failure. Do you know what the sales figures were for it compared to the others? I hope that they at least integrate him into the Teen Titans story or something. I don't want him to just fall off of the face of the planet. And though his recent cameo in The Savage Hawkman was kind of neat, he as a character didn't really seem to fit in with the story (i.e. Hawkman's story at the time was much more mystical, whereas Static has always been very centered around science).
As far as the new titles, I just hope that DC can keep their continuity straight with all of this parallel Earth stuff. I'm still trying to straighten out exactly what's different in the New 52 Universe, and now they are already adding parallel Earths.
I was able to pick up the Huntress limited series that leads into Worlds Finest, but I'm still not clear if both Huntress and Power Girl are from Earth 2, or just Power Girl, or how they got on this Earth. Probably will be explained, but I just hope the parallel universes don't spin out of control, necessitating another DC Universe-wide "Crisis" event.
All the cancelled titles had low sales I believe. Don't know the figures. Virgil did show up in Teen Titans as Red Robin's go-to-science-guy.
You can't really do the DC Universe without parallel worlds. The concept of parallel worlds has been such an integral part of the line that it's actually surprising they didn't launch it right away with the New 52.
The benefit of the New 52 as a "reboot" is that it's actually much easier to keep the continuity straight. They've sort of reset things back to square one and can clearly delineate what book takes place in which universe.
Huntress and Power Girl are both from Earth 2. Helena "Bertellini" is one of Helena's aliases.
True enough re: DC's parallel worlds.
I'm actually pretty excited about several of the new titles, and was wondering how they were going to treat Fairchild after she was revealed in Superboy (I couldn't believe that she was only going to be limited to being a tertiary character in his story).
5 bucks says we see the whole "New 52" thing reset again to be the old universe that it was supposed to replace.
I mean, it just comes off as a temporary thing, and they'll hand-wave it away, and go back to how things were before.
EC2151
Please tell me Action 52 is still slated for release this summer.
AngelCityOutlaw
52 titles is....a lot of titles to work on. So kill the weakest links.
If I gambled, I'd take that bet and you'd owe me 5 dollars.
It's hilarious and quite honestly mind-boggling that people keep thinking this. Why on Earth would they go back to how things were before? What about it makes you think that this is all temporary?
The launch of the New 52 was massively successful for them and the entire DC Universe is much fresher and not bogged down by decades of continuity. There's a cohesiveness throughout all of the titles, and the way they've organized their different lines of comics (The Edge, The Dark, Young Justice, etc.) makes everything much easier to keep track of. Let's not even forget the fact that so much of what they're putting out right now is just so incredibly good.
The Phalanx
Let's not even forget the fact that so much of what they're putting out right now is just so incredibly good.
Like motherfucking Animal Man.
Holy damn do I love Animal Man so far.
Brushfire
They bring back Powergirl yet?
Next month.
The Rot is some pretty fucked up shit. I think the Animal Man/Swamp Thing storyline with it are one of the most interesting ones to me right now in DC's New 52 (except, possibly, for the Court of Owls thing going on in the Bat Universe).
I'm very interested to read the full history of the Red, the Green, and the Rot.
For reals. Here I thought they were cutting out games out of an 'Action 52' HD remake.
Dave the Rave
It's a real shame that Static Shock is getting cancelled. The main reason I collect those comics is because I was a fan of the animated series in the early/mid 2000s.
Was it a good title? I wasn't reading it.
Alright so it's may and some of the Second Wave titles are out. I haven't read Dial H for hero but I picked up Earth 2 and World's Finest and I have to say that these are some seriously good books. Earth 2 in particular is absolutely incredible. There's a great twist that sets up the premise of the world and the motivations for many of the characters, and Nicola Scott's art is like just brilliant.
World's Finest is a fun set up for a buddy-book, with Huntress's and Powergirl's contrasting personalities. Really excited about this one.
Yeah, I haven't touched Dial H for Hero, but I did pick up Earth 2 and The World's Finest. Both are pretty great so far. Nice tie-in with Mr. Terrific, too (I'm guessing he'll be coming out more as the series progresses, since his comic ended with him accidentally going to Earth 2).
Earth 2 wasn't exactly what I was expecting based on the cover art, but the alternate super heroes and origins are pretty interesting so far, and I think it'll be a great comic.

redpajama_set_name: RedPajamaCommonCrawl


My studio is based in the creative hotspot of Chippendale in Sydney, Australia.
Yes, absolutely! Shipping is free within Australia and for all other countries there is a flat rate per order that will appear on the checkout page before your payment is processed. All orders are trackable and require a signature on delivery.
Yes. If you see an image belonging to me either in my blog The Journal on any of my social media channels, I am more than happy to arrange a custom print for you.
Not at the moment as framing is such a personal decision and should be based on your individual and interior aesthetic. I personally love a natural timber frame with a white matt board.
If you purchase a standard frame from a shop I strongly recommend investing in a framer to matt/mount the image with an acid free matt board. Matting is essential to keep the print away from the glass and to allow the image to breathe, ensuring the longevity of your artwork.
As a guide for your custom mat, allow 3 inches extra white to the left, right and top side. For the bottom side, however, you may wish to add extra weight and allow 5 inches, however there is no set rule for framing and this is where you may wish to seek the guidance of your local professional framer.
Here are some examples of what a print looks like framed with and without a mat. In both cases the white border of the print is visible, allowing the image to breathe and providing space for my signature.
I am happy to print your favourite artwork in a custom size for you. Please contact me at milton@miltongan.com if you would like a quote.
Thanks, I'm glad you like them! Sharing via social media is fine but all images must be credited to Milton Gan Editions (@miltonganeditions on Facebook and Instagram) and linked to www.miltonganeditions.com. Please do not reproduce, edit or submit my images to third parties without my consent otherwise it is a breach of copyright.
Please visit the Shipping & Returns page for more information.


Emission components could be covered under warranty for up to 8 yrs or 80,000 miles, whichever occurs first, under federal law. See EPA Emission Warranty Information.
To renew the registration each year, you must complete the Odometer Certification for Emission Exemption (EC 18) to certify that you have driven the vehicle 5,000 miles or less.
Bring the completed application, the EC 18, any existing license plates and your Nevada Evidence of Insurance card to a DMV office. If you wish to keep the old plates, you must bring the rear plate and surrender the decal in person.


text:
View from the donkey's saddle
Category Archives: Asel Asleh
February 8, 2017 · 6:27 am
Stand proud. Fearlessly. Together.
Dear friends and supporters,
During these first weeks of the Trump presidency I am reminded, more than ever, of the importance of resistance that is grounded in the values I hold most dear. Community. Equity. Love. Human Dignity. Freedom. Justice.
This short video embodies those values:
The video shows scenes from my play about the police killing of a Palestinian teenager interspersed with the reactions of audience members at Historically Black Colleges and Universities, drawing parallels between structures of oppression in Israel and here in the U.S.–and linking the struggles for liberation and equality.
The connections revealed in the video are profound. The sense of possibility expressed in communal joint struggle is deeply inspiring. This inspiration is reflected in the words that audience members called out after post-play discussions:
"Stand Proud."
"Fearlessly."
Participants in a community residency in Gainesville, FL rehearse for a staged reading of There Is A Field
I hope you will take a moment to watch–and share! I would love to hear your responses if you do!
In solidarity, in struggle, and in community,
Jen Marlowe
Playwright/Producer, There Is A Field
Founder, Donkeysaddle Projects
donkeysaddle@gmail.com
[Donkeysaddle Projects is a sponsored project of Fractured Atlas, a non-profit arts service organization. Contributions for the charitable purposes of Donkeysaddle Projects must be made payable to Fractured Atlas only and are tax-deductible to the extent permitted by law.}
Filed under Asel Asleh, Black Palestinian solidarity, Human Rights, Palestine/Israel
Tagged as Arab Israelis, Aseel Asleh, Asel Asleh, Black Palestinian solidarity, donkeysaddle projects, Dream Defenders, Gainesville, Intersectionality, Israel, Palestine, Palestinian citizens of Israel, solidarity, There Is A Field
Activism, movement building, and fighting structural inequality
Below, please find a blog post that I wrote for Hedgebrook, a phenomenal women's writing residency and community of women writers that I have been a part of since 2010.
The play ended and my colleague Carlton Mackey (founder of 50 Shades of Black) invited the audience to share one-word reflections on their experiences. The students at Bowie State University, an historically Black institution in Bowie, MD sat in silence for several moments before their words came pouring out:
"Discrimination."
"Baltimore."
"Relatable."
"Ferguson."
"Reality."
The play, called There Is A Field, tells the story of a 17-year old boy who had been killed by the police.
But it was not situated in America. The play was about Aseel Asleh, a Palestinian citizen of Israel who was killed by Israeli police on October 2, 2000, one of 12 unarmed Palestinian citizens of Israel killed by Israeli security forces at the start of the Second Intifada.
Students at Bowie State University watching There Is A Field
Filed under Asel Asleh, Black Palestinian solidarity, Palestine/Israel
Tagged as Aseel Asleh, Asel Asleh, Black Lives Matter, Bowie State University, Ferguson, From Ferguson to Palestine, Israel, Movement for Black Lives, Palestine, There Is A Field
"Ideals are our north stars:" Reflections on THERE IS A FIELD from death row
(Dear friends,
I sent a copy of my play "There Is A Field" to my friend George Wilkerson, who is on North Carolina's death row. George is part of a drama group that is considering performing the play. With his permission, I am posting here his reflections upon reading the play, which are both on the play itself and the larger Palestinian/Israeli conflict. If anyone has comments or responses for George, please post and I will send them to him!)
Hey Jen,
I finished reading There Is A Field. It's very poignant. You have a gift of making people relatable–of finding the common humanity in everyone. I thought it was clever of you to begin the play with the emails. It allowed me to view their intimate exchanges without asking anything of me, without arguing for/against anything. It had the effect of drawing me in, of investing emotionally with the sibling relationship; I have 3 brothers and one sister. That shared experience gave me a framework for understanding.
I identify with Aseel, in that people tell me I'm an idealist. The way it's said is as if idealism is disconnected from reality. Like I'm just a dreamer. However, to me, idealism is what shapes reality. Ideals are our north stars. They guide us, give us direction, provide a point of reference. Ideals have practical applications. They are governing principles…
One thing I see [in the world] is reactionism. There's a temptation to demonize the oppressors and lionize the oppressed, but the issue isn't so clearly defined. Just to be clear, oppression is wrong. Period. However, it doesn't justify the reverse racism or prejudice that is common amongst the oppressed. I believe Gandhi said it well: "An eye for an eye makes the whole world blind." Think: If I allow your treatment of me to determine my behavior and beliefs and how I treat you (and others of your race), then I don't stand for anything. I am a puppet in your hands. Then, if you allow my treatment of you to determine your behavior, etc, then where are we? We are trapped in a vicious feedback loop. Dr King recognized this, so did Gandhi, which is why they advocated nonviolence. They said, stand firm, adhere to our beliefs. Do not compromise your integrity. Someone must break the cycle. Someone must take the first step. Someone must set the example. It says, "Do unto others as you want done unto you," not "Do unto others as is done to you." You know?
I won't pretend to know a lot about the Palestinian/Israeli conflict. As I read your play, and now your book, having connected with your real-life characters, I see a temptation within me to only see their side of the story. However, I recognize that there are more sides to every story. I sympathize and am moved to compassion for their (the Palestinians') struggles. But if their roles were reversed, would they do the Jews any differently? I see Christians persecuted and martyred in Muslim-controlled countries, run out of their homes, their families slaughtered. None of it is okay. None of it is justifiable. Killing Jews because they killed Palestinians because they killed Jews because they killed Palestinians is not okay.
I know it's not politically correct to speak like this, but every party involved is in violation. Christians persecute Muslims; Muslims kill Christians; Jews kill Muslims; Gays hate Christians, saying they are "intolerant" even while they themselves are being intolerant of Christians, as if Christians' intolerance justifies their own. It's madness. Where does it end?
Picking sides only furthers it. I am a Christian, but I believe Christianity is about LOVE. I may disagree with others' beliefs and behaviors, but I love/accept them nevertheless. I'm not anyone's judge.
I believe this is the place Aseel had reached. Beyond the rights or wrongs of any one religion, there is a field. We are that field: humanity. Without the religions, the biases, the prejudices, there is a law written in every heart which tells us how we ought to treat one another. It is woven into the very nature of us. This begs the question of why we hurt each other, then, if it is within our nature to love. This is a question, the answer to which determines everything that follows. Sin. The entrance of sin corrupted our nature. But I'm not here to preach. I'm here to tear down the veils, and to demonstrate humanity as God designed us, ie, to live a life governed by love.
The way I give people my friendship immediately is because I believe in love. Sure, people have hurt me and no doubt will again. But I heal, and quickly, because I forgive. Refusal to forgive is what keeps wounds open. The more people hurt me and I forgive, the stronger I get.
–George T. Wilkerson
Filed under Asel Asleh, Black Palestinian solidarity, Criminal Justice, Death Penalty, Palestine/Israel
Tagged as Black Palestinian solidarity, death row, George Wilkerson, There Is A Field
Coming soon: THERE IS A FIELD
It is with great excitement that I announce:
the Land Day Tour of my new play There Is A Field!
There Is A Field is a play about Aseel Asleh, a 17-year old Palestinian citizen of Israel killed by police in October 2000. Based on interviews and primary sources collected over 15 years, the play offers a uniquely personal lens for understanding inequality as the root of state violence and impunity. Audiences throughout the United States will find particular resonance with themes raised by Aseel's life and murder, and post-play discussions and actions will create space to further explore connections and build solidarity across universal struggles for liberation and equality.
The play emerges at a critical juncture of unprecedented mobilization for the rights of Palestinians, for Black-Palestinian solidarity, and for transnational movement-building against supremacy and state-sanctioned violence. Aseel's life and murder, which highlights both entrenched inequality and the impunity of the State of Israel, contributes to the vital and growing national conversation around the systematic devaluation of Black life in the United States.
The Land Day Tour of There Is A Field is a professional production of the play, cast and rehearsed out of NYC, that will travel to 20 schools across ten states in March and April! The tour coincides with the 40th anniversary of Land Day, an annual commemoration of land dispossessions and the killings of Palestinian citizens of Israel in 1976.
Check out the tour schedule here, and make plans to attend a performance at a university near you! If you don't live near a city hosting the tour, you can still participate in the Land Day Tour by organizing your own reading of the play!
And, please consider supporting the Land Day Tour with a contribution today!
Towards justice!
on behalf of the Land Day Tour partner organizations:
50 Shades of Black, Adalah, Code Pink, Donkeysaddle Projects, Dream Defenders, Hands Up United, Jewish Voice for Peace, Students for Justice in Palestine-National, and the U.S. Campaign to End the Israeli Occupation.
[Donkeysaddle Projects is a sponsored project of Fractured Atlas, a non-profit arts service organization. Contributions for the charitable purposes of Donkeysaddle Projects must be made payable to Fractured Atlas and are tax-deductible to the extent permitted by law.}
Reading of an earlier version of There Is A Field in Derry, Northern Ireland
Tagged as 50 Shades of Black, Adalah, Aseel Asleh, Black Palestinian solidarity, Hands Up United, Jewish Voice for Peace, Palestine, Students for Justice in Palestine, There Is A Field, U.S. Campaign to End the Israeli Occupation
Call to Action: Witness Bahrain and There Is A Field
The coming months bring two important anniversaries.
February 14 is the 5-year anniversary of Bahrain's uprising, when hundreds of thousands of Bahrainis took to the streets calling for democracy and human rights in Bahrain–and were met by violent repression from the Bahraini regime, repression which continues until today.
March 30 is the 40-year anniversary of Land Day, an annual commemoration of land dispossession and the killings of Palestinian citizens of Israel in 1976.
Donkeysaddle Projects is inviting you to participate in global actions to mark both events!
FEBRUARY: Host a screening of our new award-winning film, WITNESS BAHRAIN!
MARCH: Participate in the Land Day Tour of our new play, THERE IS A FIELD, by organizing a performance, rehearsed reading, or "living room reading" of the play!
More information on WITNESS BAHRAIN can be found here, and information about organizing a screening can be found here.
More information on THERE IS A FIELD can be found here, and information on organizing a performance or reading can be found here.
Or–email Jen Marlowe for more information on both initiatives!
Looking forward to your participation in marking these two significant anniversaries, and in organizing events that support human rights and equality!
And–ways to help support both initiatives, along with all our work at Donkeysaddle Projects, can be found here!
In solidarity,
Director, Witness Bahrain
Filed under Asel Asleh, Bahrain, Palestine/Israel
Tagged as Aseel Aslih, Asel Asleh, Bahrain, Israel, Land Day, Palestine, Palestinian Citizen of Israel, There Is A Field, Witness Bahrain
Set the Stage for Justice!
You make possible all that we do at Donkeysaddle Projects—and we cannot thank you enough.
In 2015, you supported the premiere of our documentary film Witness Bahrain at the Seattle Transmedia & Independent Film Festival (where it won the Audience Award, with later screenings on Capitol Hill in DC and at Seattle's Arab Festival); you helped us report from the ground in Palestine/Israel, producing several short videos and feature pieces in The Nation, AlJazeera America, TomDispatch, +972Mag, Mondoweiss, and Yes! Magazine; and you supported our ongoing efforts to expose the violence of the death penalty and its connection to all forms of state violence, including police killings.
Witness Bahrain won the Audience Award at the Seattle Transmedia & Independent Film Festival
The past year has brought into stark relief the interconnection between universal struggles for liberation and equality–in Palestine, in the U.S. and beyond.
For that reason, we are asking your support to set the stage for justice in 2016, as we produce a college/university tour of our new documentary-style play, There Is A Field.
Based on interviews and primary sources collected over fourteen years, There Is A Field is a story of how a Palestinian family journeys through grief after the Israeli police killed their teenage son, Aseel. While offering an intimate view into the racism and violence faced by Palestinian citizens of Israel, the play transcends any particular time or place to reflect on oppressions in Israel/Palestine, the United States, and around the world.
We are working with a growing coalition of organizations to steer the tour of the play; including Adalah, 50 Shades of Black, Students for Justice in Palestine, Dream Defenders, Jewish Voice for Peace, the U.S. Campaign to End the Israeli Occupation, and Code Pink.
The play emerges at a critical juncture of not only escalating state violence, but also unprecedented mobilization for the rights of Palestinians, for Black-Palestinian solidarity, and for transnational movement-building.
The story of Aseel's life and murder accentuates the stark similarities between entrenched inequality and impunity, both in the State of Israel and in the U.S., and contributes to the vital and growing national conversation around the systematic devaluation of Black life in the United States. Through the performance and post-play discussions, audience members will grapple with unequal systems of justice, and together consider ways to strengthen intersectional movements for social transformation.
Your donation today will allow There Is A Field to travel to 20 universities in the United States this spring (including several Historically Black Colleges and Universities) and will enable us to end the tour with three days of performances and workshops in the St Louis area, culminating in a performance in Ferguson, MO.
Please support donkeysaddle projects with a contribution that feels meaningful to you this year. Just click here to make a tax-deductible one-time (or monthly) donation, or click here for information on sending a check!
In doing so, you will be supporting a vision of the world in which every person's humanity and rights is equally respected and equally protected.
Towards justice, freedom and equality,
Jen Marlowe & Amer Shurrab
Donkeysaddle Projects
www.donkeysaddle.org
Filed under Asel Asleh, Human Rights, Palestine/Israel, Uncategorized
Tagged as Black Lives Matter, Israel, Palestine, solidarity, state violence, supremacy
Fifteen years ago today, I got an early morning phone call. It was Adam Shapiro, my boss at the Seeds of Peace Center in Jerusalem.
"Aseel was killed this morning."
Aseel. Aseel Asleh, 17-years old, Palestinian citizen of Israel, star participant of Seeds of Peace. What happened? I almost didn't ask, it felt like a stupid question. The Second Intifada had just erupted, the whole region was engulfed in violence, what did I think happened? But was he at a demonstration? Was he shot accidentally? What were the specifics? Aseel was dead? Impossible. How? Aseel?
Adam didn't know the details yet. He didn't yet know that Aseel had been standing on the outskirts of a demonstration outside his village of Arrabeh in the Galilee, when two police officers chased him for no discernible reason. Adam hadn't yet learned that one of the officers hit our young friend in the back with a rifle butt, and that Aseel stumbled and fell face first in the olive grove. He couldn't yet tell me that Aseel's parents (who had gone to the demonstration to bring him home) saw all this, but then could see no more because the olive trees were blocking their view. They could, however, hear the shot. The doctor who later examined his body said the bullet wound suggested that Aseel had been shot point blank in the back of his neck.
But Adam didn't know any of that yet. All he knew–all he could tell me–was that Aseel had been shot and killed.
I hung up the phone and sat on my couch. I didn't know what to do. What do you do when you find out that a kid you love was killed? What's the proper thing to do? I had just made coffee and it was sitting on the table in front of me. All I remember thinking: Do I still drink the coffee? What do I do?
I realize now that I was in deep shock that morning. Yet, the question of "What do I do?" has stayed with me the past 15 years. It took root as I watched Aseel's family and friends deal with their grief and traumatic loss. It grew as I realized that the events of October 2000, in which 12 Palestinian citizens of Israel were killed, were a collective trauma that sent deep and reverberating shock waves through the entire community. It pushed me when it became evident that there would be no justice for Aseel, or for the other martyrs of October 2000.
Making sure that Aseel's story is told, impacting and educating others: This is what I can do.
And I invite you to do it with me.
For the past six months, I have been further developing There Is A Field, a documentary-style play I wrote, based on years of interviews with Aseel's family, emails that Aseel left behind, court transcripts, and other sources.
In March 2016, There Is A Field will tour to up to 15 U.S. colleges and universities, culminating in a short run in New York City. In each campus we visit, the play will be a tool of advocacy and activism. If we're able to raise enough funds, we will expand the tour even further.
As we confront brutality, state violence, systemic injustice and oppression here in the U.S. and in many parts of the world, I know many of us continue to struggle with the question of "what do I do?"
I hope you will choose, as part of your response, to support There Is A Field, so that Aseel's story can continue to impact, to educate, and to challenge. So that Aseel's story can support efforts to build a world where inequality, racism, state murder and injustice have no place.
Please click here to learn more about There Is A Field, and how to support the play.
With love for my friend, and for every young person we have collectively lost,
Aseel Asleh, age 16
Filed under Asel Asleh, Palestine/Israel
Tagged as Adalah, Arab Israeli, Aseel Asleh, Asel Asleh, Black October, Israel, October events, Palestine, Palestinian Citizen of Israel
View from the donkey's saddle · wanderings in the world of social justice/human rights activism


Astek is seeking talented V&V Engineers with extensive experience across the Australian Defence Sector to join a global leader.
The Verification and Validation (V&V) Engineer will be engaged in verifying product designs according to requirements and internal quality standards. The V&V Engineer plans, implements, tests, documents, and maintains enterprise-wide solutions to total systems or subsystems using internally created and/or off the shelf products.This position provides support to systems engineering team to meet project deliverables in the completion of development testing. Project deliverables may include producing and/or reviewing verification and/or validation plans, protocols, and reports, execution of the plans and protocols, and resolving deviations.
Responsible for working with system engineers, developers, end users and organisations to create test plans and test scripts.
Coordinate with client and other team participants to plan test events. Participate in a team of testing professionals in creating reports, tracks problems and reporting on errors that are identified.
Participate in the configuring necessary hardware and operating environments as needed to complete assigned testing.
The role will be exposed to a comprehensive array of IT products, operating systems, software, hardware, systems and networks and specialised environments.
In addition to the above, you will have relevant industry qualifications or certifications in communications and/or electronics. Defence project experience, excellent communication skills (both written and verbal) and a solution-oriented, collaborative personality are key competencies of the role.
Applicants are required to be Australian Citizens and hold at minimum a baseline security clearance. NV1 security clearance preferred.


text:
The COVID-19 Crisis Will Change Policymaking and Business
Commentary - 27/03/2020
By Soňa Muzikárová.
The COVID-19 outbreak has highlighted systemic weak points across business and supply chains.
Last week, I looked at some real economy and financial channels that the coronavirus pandemic has disrupted across the world. A global recession is now a foregone conclusion, and it will have emanated from the harsh impact on the economy.
On the one hand is the supply side, with production capacities cut back or stopped altogether as per the instructions of authorities. Volkswagen Slovakia, the largest Slovak employer, has suspended production in all three plants. Other large manufacturers are likely to follow suit. On the other hand is the demand side as consumers have been told to stay at home and have limited access to goods and services.
Both of these factors are putting pressure on domestic economies and international trade. Added to that, transnational supply chains are severely disrupted and tumbling stock markets are wiping away wealth. The uncertainty about the extent, severity and future trajectory of the coronavirus — known as COVID-19 — further impairs the confidence channel.
These effects have struck the real economy at superspeed and affected our daily lives. People are stockpiling to reduce the frequency of grocery shopping trips as well as panic buying in the expectation of shortages. Food chains offering home delivery services are overwhelmed by the number of orders. Many companies are forced to cancel online orders due to high demand, citing "technical issues." Despite calls for social distancing by governments, hardware stores are facing perpetual lines, and their half-empty shelves trigger painful memories of the golden era of socialism.
Meanwhile, in Slovakia, some individuals have not grasped the sense of urgency in managing the outbreak. Troubling social media posts have surfaced of citizens seeing this emergency as an opportunity to let off some steam skiing.
The economics of the COVID-19 outbreak is an interesting one. The behavior of individuals has a significant impact on the public health and economic outcomes of an entire country. The behavior exemplified by some in Slovakia will inevitably lead to a scenario like Italy, which is currently the European epicenter of the coronavirus pandemic. On the other hand, the combination of prudent, top-down decision-making, coupled with bottom-up responsibility, could lead to a more managed outcome — both socially and economically.
As the pandemic sheds light on the classic dichotomy between individualism and collective interest, it begs the question of what globalization and supranational cooperation can do for us these days. With the world at unease, central banks continue running the course of synchronized monetary easing. On March 15, the US Federal Reserve delivered another emergency interest rate cut that is now nearly zero. This was accompanied by the launch of a massive $700 billion quantitative easing program. The European Central Bank announced its own set of measures on March 12, including immediate liquidity support and its own asset-purchase program. Moreover, world leaders have pledged to take concerted fiscal action.
The economic response is critical. The objectives include helping the economy to continue functioning, preventing the hardest-hit sectors and businesses from going bust, and ensuring that public health care is sufficiently funded. National policy measures are a vital part of a comprehensive response strategy, as each economy has been affected differently by the coronavirus pandemic and they each have different resources at hand.
An intense global downturn will, additionally, demand heavy lifting on the part of international institutions. This response must be comprehensive, multi-disciplinary and fast-moving. This is not a time for interstate bickering. Multilateralism may be in a dire state, but it is now the time to stick to the basics and synchronize across policy domains that are mutually agreeable.
Bringing Change
The COVID-19-induced crisis will lead to a broader paradigm shift in policymaking. One-sided policymaking will no longer suffice. A balanced and diversified approach across toolkits (monetary-fiscal-structural), actors (national, international) and time (short-term versus long-term impacts) is the global economy's best bet in addressing the fallout that will ensue. Policy dominated by a strategic foresight and a targeted, potential-enhancing and resilience-strengthening approach is long overdue.
The health of the economy is also bolstered from the bottom up, and the COVID-19 outbreak has highlighted systemic weak points across business and supply chains. It is Schumpeterian creative destruction at its best. Supply shortages across "winning sectors," such as food and medical supplies, indicate poor inventory management and analytics. Long lines outside stores and canceled online orders suggest a lack of digital presence and associated infrastructure.
The disruption of supply chains means different things to different sectors. Some industries should rethink their excessive reliance on one country or region, such as China, while others should consider diversifying their sources. The current situation with supply chains highlights the need for business contingency plans geared toward being operational with minimal workers physically present. In any case, harnessing existing technologies, coupled with the constant reframing of business efforts seem to be the suitable foundation for a makeover in business.
It is only March and we are at an inflection point in 2020. The extent of change in our daily routines and the tyranny of uncertainty we are not accustomed to will be carved in our collective memory for many years to come. But as the saying goes, never let a good crisis go to waste. The global health crisis may be the catalyst for much-needed change across policymaking domains and business. This is a change that, in normal times, would slowly unfold for perhaps an entire decade.
This article was originally published on the Fair Observer website on 23 March 2020.
Soňa Muzikárová
Soňa Muzikárová is the Chief Economist at GLOBSEC Policy Institute


text:
Q: Why does app go to the create.html.erb view after post submission instead of show.html.erb view? rails 4 Right now in my rails 4 app after the user submits a post I want the app to redirect/render the show view, but right now it just goes to the create view.  Here is my Posts controller:
class PostsController < ApplicationController

  def show
    @post = Post.find(params[:id]) # show
  end
end

def new
  @post = Post.new
end

def create
  @post = Post.new(post_params)

  private

  def post_params
    params.require(:post).permit(:Title, :Body) #whatsoever your post has
  end

#redirect_to post_path(@post)

  if @post.save
    redirect_to @post.find(params[:id])
  else
    render :new
  end
end

Here are my routes:
Rails.application.routes.draw do

root :to => "pages#index"
devise_for :users
resources :users
resources :pages
resources :posts
end

Thanks for your help.

A: Looks like there's a few bits of code in wrong places - end statements, and your final if statement at the bottom, which doesn't seem to be in any method.
Something like this should work:
class PostsController < ApplicationController

  def show
    @post = Post.find(params[:id]) # show
  end

  def new
    @post = Post.new
  end

  def create
    @post = Post.new(post_params)

    if @post.save
      redirect_to @post.find(params[:id])
    else
      render :new
    end
  end

  private

  def post_params
    params.require(:post).permit(:title, :body) #whatsoever your post has
  end

end

A: First, the redirect is wrong. It should be simply:
redirect_to @post

After fixing that, it could be re-rendering because there was an error validating the @post. If @post.save fails the form will be re-rendered, but the URL will stay pointed at the create action.

redpajama_set_name: RedPajamaStackExchange


Sometimes in the summer you just need something sweet and this incredibly easy cobbler will do the trick! With limited ingredients, you can make an immensely satisfying, guilt-free, paleo dessert in no time at all. The berries are your choice, but I find it easier to go with a premixed bag to take even more though out of this recipe. If you are using fresh fruit, make sure to add the honey a couple hours before and let the berries sit at room temperature. This will help pull some of the juices out of the berries making the end result much sweeter. If you don't really care for the whole paleo thing, adding some vanilla ice cream on top makes this even better.
5 cups mixed, frozen berries. Your choice!
Add frozen berries to bowl and let thaw. Add chia seeds and honey. Stir to combine.
Add berries to the base of a 9 inch cast iron skillet (or any oven proof dish will work).
In a food processor/blender, add the almond flour, coconut flour and salt. Mix just to combine the dry ingredients.
Add the cold butter to the food processor/blender. Pulse just until the butter is combined. The batter will be lumpy. Then add the honey and mix just to combine.
Using your fingers. Break the dough apart into small pieces and "crumble" on to the top of the berry mixture.
Bake for 35-45 minutes or until the crumble turns golden brown. Best served hot!


text:
Definitions of 'egoism'
Egoism's treatment of altruism
Arguments for and against
An ancient form of egoism
Egoism and altruism
Kraut, Richard
Retrieved January 18, 2020, from https://www.rep.routledge.com/articles/thematic/egoism-and-altruism/v-1
Henry Sidgwick conceived of egoism as an ethical theory parallel to utilitarianism: the utilitarian holds that one should maximize the good of all beings in the universe; the egoist holds instead that the good one is ultimately to aim at is only one's own. This form of egoism (often called 'ethical egoism') is to be distinguished from the empirical hypothesis ('psychological egoism') that human beings seek to maximize their own good. Ethical egoism can approve of behaviour that benefits others, for often the best way to promote one's good is to form cooperative relationships. But the egoist cannot approve of an altruistic justification for such cooperation: altruism requires benefiting others merely for their sake, whereas the egoist insists that one's ultimate goal must be solely one's own good.
One way to defend ethical egoism is to affirm psychological egoism and then to propose that our obligations cannot outstrip our capacities; if we cannot help seeking to maximize our own well being, we should not hold ourselves to a less selfish standard. But this defence is widely rejected, because psychological egoism seems too simple a conception of human behaviour. Moreover, egoism violates our sense of impartiality; there is no fact about oneself that justifies excluding others from one's ultimate end.
There is, however, a different form of egoism, which flourished in the ancient world, and is not vulnerable to this criticism. It holds that one's good consists largely or exclusively in acting virtuously, and that self-interest properly understood is therefore our best guide.
Kraut, Richard. Egoism and altruism, 1998, doi:10.4324/9780415249126-L126-1. Routledge Encyclopedia of Philosophy, Taylor and Francis, https://www.rep.routledge.com/articles/thematic/egoism-and-altruism/v-1.
Buddhist concept of emptiness By Williams, Paul
Moral motivation By Wallace, R. Jay
Moral scepticism By Nelson, Mark T.
Morality and identity By Singer, Ira
Prudence By Hughes, Gerard J.
Reasons for action By Wiland, Eric
Self-interest By Oneill, John