While Florida may not seem like the first state to come to mind when thinking about cannabis, they have been working hard to meet the demands of the statewide cannabis need. Although they have not yet moved into the recreational weed industry, they have been working to create new laws to allow for easier access to the substance as well as different social laws to consume it.
Many have been working to figure out what smoking weed will look like in a state that has long had conservative motives regarding the substance. Now that medicinal cannabis is legal in 33 states around the U.S., it seems more reasonable than ever to assume that Florida would work on changing their laws.
In big news, the governor of Florida, Ron DeSantis signed a bill into law that would allow smokable medical marijuana within the state borders. This has been quite a priority not only for the state but for the Governor for some time now. Previously there had been a smoking ban in place that was put into law in 2017. The new bill effectively repeals this to allow smoking the substance which makes a large amount of sense given the industry in the state.
The new law is going into place immediately which means that the constituents will be able to directly benefit from the bill's passing. Although there are still some needed health department regulations in place in regard to how doctors prescribe the substance, it will remain legal throughout the state. Despite this, there has still yet to be a way to legally purchase smokeable cannabis in the state, but this does look like it has to change now that this newest law is in place.
The law that could go into place in regard to who can receive cannabis takes into consideration the various ailments that could benefit from using the substance. These illnesses vary from person to person, but one of the most popular is chronic pain. There are still a large number of uses for the substance, but only time will tell how the market is able to shift to allow for legal weed to then be legally smoked throughout Florida.


text:
For which we give thanks
Barack Obama pardoned "Cheese" and his alternate Mac (not shown) this week. Getty Images
The first Thanksgiving in the New World was celebrated in 1621, nearly a year after the Pilgrims landed at Plymouth in the Massachusetts Bay Colony.
In 1789, George Washington became the first of many US presidents to formally proclaim a day of "public thanksgiving and prayer":
I do recommend and assign Thursday, the 26th day of November next, to be devoted by the people of these States to the service of that great and glorious Being who is the beneficent author of all the good that was, that is, or that will be; that we may then all unite in rendering unto Him our sincere and humble thanks for His kind care and protection of the people of this country previous to their becoming a nation; for the signal and manifold mercies and the favorable interpositions of His providence in the course and conclusion of the late war; for the great degree of tranquillity, union, and plenty which we have since enjoyed; for the peaceable and rational manner in which we have been enabled to establish constitutions of government for our safety and happiness, and particularly the national one now lately instituted; for the civil and religious liberty with which we are blessed, and the means we have of acquiring and diffusing useful knowledge; and, in general, for all the great and various favors which He has been pleased to confer upon us.
In 1863, in the midst of the civil war, Abraham Lincoln likewise called for a day of Thanksgiving in November:
I do therefore invite my fellow citizens in every part of the United States, and also those who are at sea and those who are sojourning in foreign lands, to set apart and observe the last Thursday of November next, as a day of Thanksgiving and Praise to our beneficent Father who dwelleth in the Heavens.
And so it was until President Franklin Roosevelt, in 1939, temporarily moved the celebration back to the third Thursday in November to stimulate Depression-era Christmas sales.
President Obama on Wednesday issued his own Thanksgiving proclamation:
Thanksgiving Day invites us to reflect on the blessings we enjoy and the freedoms we cherish.
As we gather with family and friends to take part in this uniquely American celebration, we give thanks for the extraordinary opportunities we have . . .
Nearly 400 years ago, a group of Pilgrims left their homeland and sailed across an ocean in pursuit of liberty and prosperity. With the friendship and kindness of the Wampanoag people, they learned to harvest the rich bounty of a new world.
Together, they shared a successful crop, celebrating bonds of community during a time of great hardship. Through times of war and of peace, the example of a Native tribe who extended a hand to a new people has endured . . .
With God's grace, this holiday season we carry forward the legacy of our forebears.
In the company of our loved ones, we give thanks for the people we care about and the joy we share, and we remember those who are less fortunate.
At shelters and soup kitchens, Americans give meaning to the simple truth that binds us together: We are our brother's and our sister's keepers.
We remember how a determined people set out for a better world — how through faith and the charity of others, they forged a new life built on freedom and opportunity.
The spirit of Thanksgiving is universal. It is found in small moments between strangers, reunions shared with friends and loved ones, and in quiet prayers for others.
Within the heart of America's promise burns the inextinguishable belief that together we can advance our common prosperity — that we can build a more hopeful, more just, and more unified Nation.
This Thanksgiving, let us recall the values that unite our diverse country, and let us resolve to strengthen these lasting ties.
NOW, THEREFORE, I, BARACK OBAMA, President of the United States of America, by virtue of the authority vested in me by the Constitution and the laws of the United States, do hereby proclaim Thursday, November 27, 2014, as a National Day of Thanksgiving.
I encourage the people of the United States to join together — whether in our homes, places of worship, community centers, or any place of fellowship for friends and neighbors — and give thanks for all we have received in the past year, express appreciation to those whose lives enrich our own, and share our bounty with others.
IN WITNESS WHEREOF, I have hereunto set my hand this twenty-sixth day of November, in the year of our Lord two thousand fourteen, and of the Independence of the United States of America the two hundred and thirty-ninth.
Read Next The inconvenient (and tragic) truths

redpajama_set_name: RedPajamaCommonCrawl


Hong Kong-based Spanish illustrator Alexis Bautista is on a mission to bring fun to the city with Kokonuzz.
Barcelona native Alexis Bautista moved to Hong Kong in 2006 to work in marketing. Experiencing the city's busy urban lifestyle, the self-taught designer decided to create something fun for busy urban-dwellers, opening his viral entertainment firm Kokonuzz in 2012.
He started by creating a series of whimsical animal characters, such as a Spanish pig named Kino and a Hong Kong wolf called Luppo. The Hong Kong series, which was inspired by local culture, had Kino dressed up as a popular dim sum dish, Char Siu Bao (barbecued steamed bun).
"It's just our characters going around the city doing fun things," he said. "For example, taxi drivers in Hong Kong carry many phones, so we have our octopus, Otto, driving a taxi with many phones." Other characters, such as Luke & Mary, a pair of adventurous siblings, and Dim Sum Party are tailored for the children's market.
The characters were launched printed on T-shirts, which were sold online and at local farmers' markets. The company later got its big break exhibiting at the 2014 Hong Kong International Licensing Show, where it met its first investor, DNA 1964 Ltd.
"We also sealed deals with several partners, including Hong Kong Magnetic Products Ltd, a big magnet manufacturer from Hong Kong, which was looking for a brand to create its own line of products. After meeting several times, we created many different collections, which are now distributed in the UK, Germany, Japan, US, France, Hong Kong and the Chinese mainland," he said.
Since then, Kokonuzz has expanded its presence in the digital space by developing content on Facebook and YouTube. Such quirky videos as "Are you a true Hong Kongese?" and "Hip Hop Pig," have developed a strong following.
Kokonuzz returned to the Licensing Show last January, where its characters drew an even wider audience. "Lots of people were interested this year, including the team from the gaming application Cut the Rope.
For 2015, Mr Bautista has his eyes set on mobile applications. A story-telling mobile application and several games are now in the works. "Some of our brands' storylines will be developed through mobile games, similar to Angry Birds," he said.


text:
\section{Introduction}

Flares are explosive events that occur in solar and stellar atmospheres. Flares are observed across a wide range of wavelengths, such as radio, visible, X-rays and gamma rays and the emission responsible for these observations originates from many different regions within solar and stellar atmospheres, from photospheres to coronae. It is generally believed that both solar and stellar flares are produced by the same mechanism, namely magnetic reconnection \citep{2011LRSP....8....6S}. However, discrepancies are readily observed, most notably the energy of the flares, which, for stellar flares, can often be several orders of magnitudes larger than even the largest solar flares.

While stellar flares have been studied for decades, it is only recently, through observations made by NASA's \textit{Kepler} mission \citep{2010Sci...327..977B}, that a statistically large sample of flares for a single star has been obtained. \citet{Davenport2014ApJ} detected over 6,000 flares on an M dwarf star in just 11 months of \textit{Kepler} data. Using a subset, containing 885 flares, which were classified as ``classical'' because they contained just a single peak, \citeauthor{Davenport2014ApJ} created an empirical flare template, that was well-represented by a polynomial  in the fast rising phase, and two exponential decays, one each for the impulsive and gradual decay phases respectively. The first decay phase corresponds to radiative cooling losses and the second one is thought to be related to thermal conduction losses \citep{2004psci.book.....A}. Considering the large number of flares used, the scatter around this flare template is remarkably low.

\textit{Kepler} obtained broadband white light observations (between 4200 and 9000~{\AA}) of stellar intensity and has vastly increased the number of solar-like stars on which flares have been observed, prompting a number of statistical studies \citep[e.g.][]{2015EP&S...67...59M, 2019ApJ...876...58N}, many of which consider flaring rates, with a particular interest in determining how likely the Sun is to produce an energetic superflare. While flares are a common feature of \textit{Kepler} light curves, the same cannot be said for white light flare observations of the Sun. Solar white light flares are rare because they tend to be relatively short in duration (a few minutes) and have a low contrast, making ``Sun-as-a-star'' observations of white light flares particularly challenging. Nevertheless, \citet{2011A&A...530A..84K} performed a statistical study of Sun-as-a-star flares observed in a number of data sets, spanning a range of wavelengths, including Total Solar Irradiance (TSI). \citeauthor{2011A&A...530A..84K} demonstrated that white light emission is ubiquitous in solar flares, regardless of the energy of that flare, and that, while there is some dependence on flare strength, the blackbody temperature of solar flares is between $8,000$--$10,000$\,K, which is similar to estimates for M dwarf flare temperatures \citep{1992ApJS...78..565H}. In a similar analysis to that of \citeauthor{Davenport2014ApJ}, \citeauthor{2011A&A...530A..84K} produced average flare profiles, using 2,100 flares, and found that the TSI profile only contained the impulsive phase, with no evidence of the gradual decay phase. \citet{2011A&A...530A..84K} speculated that this could be because the gradual decay was below the noise level.

However, using resolved observations of the Sun, it has been shown that white light flares are common even for relatively weak flares \citep[e.g.][]{2003A&A...409.1107M, 2006SoPh..234...79H, 2008ApJ...688L.119J}. \citet{2016ApJ...833...50K} use highly resolved white light observations of a single flare to produce a large number of light curves within the flaring region. The authors find that 58\% of the light curves can be well represented by a single-component decay phase, while the other 42\% are better represented by two components, akin to the morphology found by \citet{Davenport2014ApJ}. \citeauthor{2016ApJ...833...50K} also found that, where two phases are favoured, the cooling times correspond to those expected for the chromosphere and corona respectively \citep{2006ApJ...641.1210X}.

\citet{2017ApJ...851...91N} used the \textit{Helioseismic and Magnetic Imager} (HMI) onboard the \textit{Solar Dynamics Observatory} (SDO) to produce white light flare light curves, finding that, for a given energy, solar white light flares are an order of magnitude longer than stellar superflares observed with \textit{Kepler}. Although, it is worth noting that the energies of the solar and stellar flares do not overlap, and so this result is based on extrapolations. Furthermore, the solar light curves were obtained by selecting spatial regions corresponding to the flare, rather than using Sun-as-a-star data. Although potential explanations for the discrepancy are proposed in terms of differences in cooling or magnetic field strength, the authors remain understandably cautious, stating that a better understanding of the mechanisms responsible for white light emission would help clarify the situation.

The exact emission mechanisms responsible for white light flares are not yet totally clear \citep[see discussions in][and references therein]{2016ApJ...816...88K, 2016ApJ...833...50K}. It is generally assumed that continuum white light emission originates from the region encompassed by the mid-photosphere and lower chromosphere. White light flares can show good temporal correspondence with hard X-ray emission \citep[e.g.][]{1995A&AS..110...99F}, implying that energetic electrons play an important role. While these electrons are capable of reaching the chromosphere, the mechanism by which the energy is transported to the photosphere is still debated. To determine how analogous solar flare morphology is to the white light stellar flares observed by \citet{Davenport2014ApJ} this article considers $304$~{\AA}, $1600$~{\AA} and $1700$~{\AA} data from the \textit{Atmospheric Image Assembly} \citep[AIA;][]{Lemen2012SoPh_AIA} instrument onboard the SDO. Although these wavelengths are not traditionally considered as white light, and are outside the waveband observed by \textit{Kepler}, the lines are used here because they originate from various locations within the photosphere and chromosphere (as described in Section \ref{sec:Data}).

Although TSI and Sun-as-a-star SDO/HMI data may be more akin to Kepler data, solar flares are infrequently observed in these data, even in the case of large eruptive events. As a result, analyses often rely on assumed theoretical models. For example, \cite{Emslie2012ApJ} had to complement the direct measurements of bolometric irradiance by estimations based on modelling.  Moreover, the temporal resolution of SDO/AIA data is less than 1 minute, in contrast to TSI. This condition is important for the analysis of time profiles of solar flares which are more dynamic than stellar ones.

A better characterisation of the underlying shape of a flare permits studies of more transient flare light curve features, such as quasi-periodic pulsations \citep[QPPs; see][for recent reviews]{2016SoPh..291.3143V, 2020STP.....6a...3K}, which are notoriously difficult to detect and characterise robustly. Detection mechanisms that rely on detrending or model fitting \citep[e.g.][]{2018SoPh..293...61D, 2017A&A...600A..78P, 2019ApJS..244...44B} would benefit from information concerning the underlying flare shape.

This article aims to investigate the solar-stellar flare connection, and emission mechanisms associated with white light flares by comparing the flare profile associated with various layers of the Sun's lower atmosphere with the flare profile associated with white light observations of flares on an M dwarf obtained by \citet{Davenport2014ApJ}. The target of the study was to provide an instrument for the analysis of cooling during the decay phase and revealing cases related to additional sources of energy release. As previously mentioned, we use SDO/AIA data from the 1600~{\AA}, 1700~{\AA} and 304~{\AA} channels. In Section \ref{sec:Data}, we describe the data in more detail, including how they were combined to determine median flare profiles for each channel. These median flare profiles are then fitted with both a combination of two exponential functions and a broken power law, as described in Section \ref{sec:fitting}. The fits are discussed in detailed Section \ref{sec:discussion}, and the main conclusions are summarised in Section \ref{sec:conclusions}.

\section{Observations and data processing}
\label{sec:Data}
We obtained the total flux of the Sun-as-a-star using the images obtained  by AIA \citep{Lemen2012SoPh_AIA}  on-board SDO. The channels used here demonstrate the chromospheric and photospheric emission \citep{ODwyer2010A&A}: 1600~{\AA} (transition region and upper photosphere), 1700~{\AA} (temperature minimum, photosphere) and 304~{\AA} (chromosphere, transition region). The image cadence is 24~s for the 1600~{\AA} and 1700~{\AA} channels and 12~s for the 304~{\AA} channel.

The initial flare selection was performed using the GOES flare catalogue \footnote{\url{https://hesperia.gsfc.nasa.gov/goes/goes_event_listings/}}. Each event was visually inspected and was required to have a ``classical" flare time profile, consisting of a fast rise followed by a slow decay without any flattening or additional peaks in soft X-rays (SXR). When determining which flares to include in our sample the time interval onset was taken to be about 10 minutes before the flare maximum in GOES X-ray flux and the duration was defined as the length of time taken for the flux to decrease to the pre-flare level. More rigorous time scales were defined in the subsequent analysis, as described below. The initial  list consisted of 359 flares from B5 to X9.3 GOES class.

After processing the AIA images with the standard package of SolarSoftware \citep[SSW]{1998ESASP.417..225B, 1998SoPh..182..497F}, we obtained the total flux of the whole image for each time moment and produced a preliminary time profile of the flare. Thus, we processed the AIA images as if they were Sun-as-a-star or without an extracting the flare area and the resultant flux was equivalent to data of instruments observing without spatial resolution.  To enable a combined analysis of the flares of different strength and duration, the profiles were normalised in both flux and time. First, each time profile was normalised using the flux maximum observed in each flare, meaning the maximum in normalised flux was unity for all flares in the sample. Second, we defined the time moment of the flux maximum as zero, so the time of the rise phase had negative values and the decay phase time had positive values. Finally, to get the same time scale for events of different duration, we presented the time series in normalised units defined by the time taken for the intensity to decrease to half the maximum for each time profile ($t_{1/2}$), following the methodology of \cite{Davenport2014ApJ}. Then the duration of each time profile was limited to a range of --5 to 10 time bins ($t_{1/2}$). The time profiles in each channel were again checked to ensure there were no additional peaks during the decay phase that were missed when selecting the initial sample. The criteria for inclusion in the final sample was that any fluctuations in the time profile should be less than 30$\%$ of the flux value. We used the time profile derivative for control of this criterion. Application of this criterion also minimises uncertainties in the determination of the $t_{1/2}$ value. As we processed solar flares from X to B GOES class and saturation in emission could not be excluded, this current criteria allowed us to escape significant contribution from saturation when forming time profiles.

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_h_1600_median_final}
    \caption{Time profile of solar flare emission at 1600~\AA. Red data points are the individual data from the 102 flares in the sample, thick blue line shows the median values and the thin green lines show the interquartile ranges.}
    \label{fig:1600_prof}
\end{figure}

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_h_1700_median_final}
    \caption{Time profile of solar flare emission at 1700 \AA. Line colours and data symbols are as described in Figure \ref{fig:1600_prof}, except only 54 flare profiles were included. }
    \label{fig:1700_prof}
\end{figure}

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_h_304_median_final}
    \caption{Time profile of solar flare emission at 304 \AA. Line colours and data symbols are as described in Figure \ref{fig:1600_prof}.}
    \label{fig:304_prof}
\end{figure}

The final sample contained 105 events in total from the 1600~{\AA} and 304~{\AA} channels (104 from 1600~{\AA} and 102 from 304~{\AA}). All profiles are presented on the same plot, with data shown as red crosses in Figures~\ref{fig:1600_prof} and \ref{fig:304_prof} for the 1600~{\AA} and 304~{\AA} channels, correspondingly. The X class flare ratio is 6$\%$, the M class flare ratio is 58$\%$, the C class flare ratio is 35$\%$ and B class flare ratio is 1$\%$. Only 53 time profiles of emission in the 1700~{\AA} channel showed both significant response and satisfied the all criteria outlined above (see Figure~\ref{fig:1700_prof}).

To construct the average time profile we re-sampled time profiles to a time resolution of 0.001$t_{1/2}$ using linear interpolation, as was done by \cite{Davenport2014ApJ}. The average time profiles were defined as the median flux value computed at each time bin and are shown in Figures~\ref{fig:1600_prof}--\ref{fig:304_prof} as blue lines. One can see that the dispersion of initial data is significantly higher in the 1700~{\AA} band plot, despite containing a smaller number of flare profiles.

The standard errors, as shown in Figures~\ref{fig:1600_prof}--\ref{fig:304_prof}, are given by the median of values above and below the average value for high ($er_h$) and low values ($er_l$), correspondingly. This is also referred to as the interquartile range. As these errors are mainly asymmetric during the decay phase we used half of the sum of these two values ($\sigma =(er_h+er_l)/2$) as the error for the function fitting. The time-averaged time profiles obtained for the solar flares demonstrate the similar behaviour to the M4 dwarf flare time profile obtained by \cite{Davenport2014ApJ} (see in Figure~\ref{fig:1600_model}). During the decay phase, the evolution is fully agreed up to $t_{1/2}$ equal about 1 . After this moment, the solar intensity decays slower in all three wavelength bands relative to the M4 dwarf flare emission.

\begin{figure}
	\includegraphics[width=\columnwidth]{res_model1600.eps}
    \caption{ Comparison of the obtained time profiles of solar flare emission with the time profile of the M4 dwarf.}
    \label{fig:1600_model}
\end{figure}

\section{Decay phase fitting} \label{sec:fitting}
\citet{Gryciuk2017SoPh} determined an analytic template of the decay phase of a solar flare composed of a single exponent with various coefficients taking into account peculiarities of the flare profile shape. The template was derived and applied to soft X-ray observations that describe coronal plasmas. However, the decay phase of a solar flare is a composition of the cooling process and various heating processes, especially in lower layers of the solar atmosphere. As our time profiles clearly demonstrated a steep initial decay followed by a slower decline in flux, we decided to apply the two-phase model. This model was successfully used by \cite{Davenport2014ApJ} for the flares observed on an M4 dwarf. Despite the difference in the atmospheric structure (temperature and density stratification) between the Sun and M dwarfs, the flare evolution is similar in both cases \citep{Allred_2006ApJ}.

The average time profiles, obtained using the natural logarithm of flux, are presented in Figures~\ref{fig:1600_fit}--\ref{fig:304_fit}. The flux data were fitted using two straight lines, $f_1(t)=a_1\exp^{b_1t_{1/2}}$ and $f_2(t)=a_2\exp^{b_2t_{1/2}}$, corresponding to the two different decay phases. Initially, the same time regions as \cite{Davenport2014ApJ} were used for the fitting. These ranges are $0 < t_{1/2}< 0.5$ for $f_1(t)$ and $3 < t_{1/2}< 6$ for $f_2(t)$. The results are shown in red in Figures~\ref{fig:1600_fit}--\ref{fig:304_fit}. In addition, alternative time regions were chosen to improve the fitting of each phase:  $0 < t_{1/2}< 1.5$ for $f_1(t)$ (shown in blue) and $3 < t_{1/2}< 10$ for $f_2(t)$ (shown in green). The results of the fitting are shown in Table~\ref{tab:table1}.

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_fitted_1600_median_final_10.eps}
    \caption{Average (median) time profile of solar flare emission at 1600~{\AA} (black with error bars) fitted by two exponential functions for different periods. Red, dashed lines and red text in the legend correspond to the t1=[0, 0.5]$t_{1/2}$ and t2=[3, 6]$t_{1/2}$. Blue dashed lines and blue text in the legend correspond to t1=[0, 1.5]$t_{1/2}$, and light green solid lines and light green text in the legend correspond to t2=[3, 10]$t_{1/2}$. }
    \label{fig:1600_fit}
\end{figure}

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_fitted_1700_median_final_10.eps}
    \caption{Average (median) time profile of solar flare emission at 1700~{\AA} fitted by two exponential functions for different periods. The line and text colours correspond to the same period as on Figure~\ref{fig:1600_fit}.
    }
    \label{fig:1700_fit}
\end{figure}

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_fitted_304_median_final_10.eps}
    \caption{Average (median) time profile of solar flare emission at 304~{\AA} two exponential functions for different periods. The line and text colours correspond to the  same period as on Figure~\ref{fig:1600_fit}.}
    \label{fig:304_fit}
\end{figure}

\begin{table}
	\centering
	\caption{Results of fitting by two exponential functions $f_1=a_1\exp^{-b_1t_{1/2}}$ and $f_2=a_2\exp^{-b_2t_{1/2}}$.}
	\label{tab:table1}
	\begin{tabular}{lcccc}
		\hline
	Fit interval& &1600 \AA & 1700 \AA & 304 \AA \\
		\hline
	 $t_{1/2}$<0.5&$a_1$&1.000$\pm$0.001&1.008$\pm$0.010&0.952$\pm$0.034\\
	 $t_{1/2}$<1.5&$a_1$&0.994$\pm$0.006&0.971$\pm$0.013&0.923$\pm$0.013\\

	 $t_{1/2}$<0.5&$b_1$&0.680$\pm$0.005&0.800$\pm$0.040& 0.758$\pm$0.147\\
	 $t_{1/2}$<1.5& $b_1$&0.672$\pm$0.007&0.668$\pm$0.016&0.601$\pm$0.018\\

	 3<$t_{1/2}$<6&$a_2$&0.367$\pm$0.016&0.336$\pm$0.021&0.421$\pm$0.018\\
	 3<$t_{1/2}$<10&$a_2$&0.298$\pm$0.007&0.275$\pm$0.011&0.341$\pm$0.007\\

	 3<$t_{1/2}$<6&$b_2$&0.186$\pm$0.010&0.110$\pm$0.013&0.203$\pm$0.009 \\ 3<$t_{1/2}$<10&$b_2$&0.141$\pm$0.004&0.066$\pm$0.006&0.156$\pm$0.003\\

		\hline
	\end{tabular}
\end{table}

\begin{figure}
	\includegraphics[width=\columnwidth]{res_plot_fitted_1600_median_bpw}
		\includegraphics[width=\columnwidth]{res_plot_fitted_1700_median_bpw.eps}
			\includegraphics[width=\columnwidth]{res_plot_fitted_304_median_bpw.eps}
    \caption{Average (median) time profiles (black) fitted by the broken power-law model (green line) and two exponential functions as shown in Figures \ref{fig:1600_fit}--\ref{fig:304_fit} (dashed blue lines) for t1=[0, 0.5]$t_{1/2}$ and t2=[3, 6]$t_{1/2}$.  The panels from the top to the bottom present 1600~{\AA}, 1700~{\AA} and 304~{\AA} bands, correspondingly. The red solid line marks the time interval of the second phase fitting. }
    \label{fig:1bow_fit}
\end{figure}

We also fitted the time profiles with a broken power-law model to reveal the time of the phase change and with the aim of finding a better description of the average time profiles.
The function was:
\begin{equation}
f(t)= A
   \begin{cases}
      \exp^{\textrm{\scriptsize{index$_1$}}\times t_{1/2}} & \textrm{for }t< t_{\textrm{\scriptsize{break}}},\\
      \exp^{\textrm{\scriptsize{index$_2$}}\times t_{1/2}} \times \exp^{(\textrm{\scriptsize{index$_2$}}-\textrm{\scriptsize{index$_1$}})\times t_{1/2}} & \textrm{for }t>t_{\textrm{\scriptsize{break}}},
     \end{cases}
     \label{eq:1bow_fit}
     \end{equation}
where $t_{\textrm{\scriptsize{break}}}$, index$_1$ and index$_2$ are all parameters determined by the fitting process.

\begin{table}
	\centering
	\caption{Results of fitting with a broken power law function }
\label{tab:table_bpow}
	\begin{tabular}{lccc}
		\hline
		 &1600 \AA & 1700 \AA & 304 \AA \\
		\hline

		index$_1$ & 0.680 $\pm$ 0.032 & 0.714 $\pm$ 0.035 & 0.589 $\pm$ 0.048 \\
	index$_2$ & 0.265 $\pm$ 0.032 & 0.207 $\pm$ 0.025  & 0.270 $\pm$ 0.034  \\
	t$_{\textrm{\scriptsize{break}}}$&	1.548 $\pm$ 0.155  & 1.282 $\pm$ 0.105 & 1.477 $\pm$ 0.198 \\
	$\chi^2$&	1.178   & 1.079 & 0.682 \\
		\hline
	\end{tabular}
\end{table}

Table~\ref{tab:table_bpow} shows the results of fitting equation \ref{eq:1bow_fit} to the median flare profiles, with $\chi^2$ values. A comparison of fitting a broken power-law model with the previous fitting, of two independent exponents, is presented in Figure~\ref{fig:1bow_fit}. One can see that the broken power-law model describing the decay phase of the average time profiles provides a good fit to the data until $t=6 t_{1/2}$. We note that the broken power-law function is a better fit to the flare profile at around 2$ t_{1/2}$.

\section{Discussion}\label{sec:discussion}
In this study we obtained averaged time profiles and fitted templates describing the decay phase of a solar flare for different spectral bands. As previously mentioned, there are two main mechanisms determining the cooling processes of a flare decay: radiative cooling and thermal conduction \citep{2004psci.book.....A}.
According to the model of plasma cooling, thermal conduction losses initially dominates during the first part of the decay phase. Later we observe the domination of radiation losses during the second phase \citep[see,][]{Cargill1995ApJ,Aschwanden2009ApJS}. \cite{Cargill1995ApJ} also noted that if radiative losses dominate during the initial phase of decay, they still dominate during the entire decaying phase. However, here we can discriminate between the steep \citep[called impulsive by][]{Davenport2014ApJ} and gradual phases during the decay phase of the analysed time profiles. For this reason, we focused our study on the fitting of the averaged time profiles with models consisting of two components only, as done in previous studies \citep[see e.g.][]{Davenport2014ApJ}.

Domination of thermal conduction or radiative losses relates to the cooling times due to these processes, and depends on temperature, density and loop length in the case of thermal conduction. Thus, the flux behaviour during the decay phase depends on two factors~--- the ratio between cooling by radiation and cooling by thermal conduction and the ratio between the temperature and density of the generating emission region.

The temperature of spectral lines that dominate in the formation of emission of the chosen spectral bands depends on the formation height of the emission. According to \citet{ODwyer2010A&A}, emission in the 304~\AA~band is
mainly formed by the doublet  H~II line (303.78{\AA}) that has $\log(T)=4.7$ and corresponds to the chromosphere and transition regions. We note that the SDO/AIA~{304\AA} band also has a contribution from two spectral lines with $\log(T)>6$ \cite[see][and references in it]{ODwyer2010A&A}. The first line is the Si XI 303.33~\AA~line with $\log(T) = 6.2$ whose contribution is significant in quiescent emission of off-limb active regions only. The Ca XVIII 302.19 A line with $\log(T)=6.85$ contributes to flare emission. However, its fraction of total emission was estimated as 0.05.

The quiet Sun emission in the 1600~\AA~band is generated predominantly by the C~IV line and continuum emission, both with $\log(T) = 5$. This temperature value implies that the level where the emission of this band is formed is higher than the formation height of the 304~\AA~band. The continuum dominates the emission of the 1700~{\AA} band for quiet Sun regions. Thus, the emission is formed at $\log(T) = 3.7$, and it typically originates from the photosphere. The results obtained by \citet{S2019ApJ} refined the contribution of the spectral lines emitted within the 1600~\AA~ and 1700~\AA~ bands. The authors confirmed the share of the C~IV doublet emission to the 1600~\AA~band, but they also revealed the domination of the C~I 1656~\AA~multiplet contribution over the continuum for the 1700~\AA~band. This means that emission in the 1700~\AA~ band is mostly formed at $\log(T) = 4$--4.2. Therefore, the emission from this band should be the closest in temperature to M4 dwarf flares, where $\log(T) \approx 4$ \citep{1992ApJS...78..565H}.

However, we should take into account that the structure of the atmosphere of an M dwarf star differs from the solar atmosphere. The temperature in the M dwarf atmosphere rises from cooler than the solar photosphere to hotter than the solar corona within a more narrow height range \cite[see,][]{Allred_2006ApJ}. Moreover, the initial energy release should occur lower in an M dwarf atmosphere
than in the solar one \cite[see Figure~8a,][]{Allred_2006ApJ}.

If we fit the first phase of cooling using the same time interval
as \cite{Davenport2014ApJ}, the coefficient $b_1$
of decay for solar flux is lower than that obtained by \citeauthor{Davenport2014ApJ} for the M4 dwarf even in the case of the 1700~\AA~band (0.800 \textit{vs} 0.965). Increasing the fitting interval for the first cooling phase up to 1.5$t_{1/2}$ decreased the coefficient $b_1$
to 0.668 for the 1700\,{\AA} band. We note that the difference between the coefficients obtained for different time intervals exceeds the error bars. Therefore, cooling during the first steep phase was found to be even slower for solar flares than for flares on the M4 dwarf. As the 1700~{\AA} channel and M dwarf flares are associated with similar temperatures this implies that the plasma responsible for M4 dwarf flare emission is denser than that associated with the 1700~{\AA} solar flares, and so potentially originates from a deeper layer. The fact that the coefficient decreases when the fitting range is extended could be related to the impact of chromospheric evaporation, which would cause an increase in flux at around 1--3$t_{1/2}$.

Fitting a broken power law to the 1700\,{\AA} band gave the decay coefficient index$_1$ equal to 0.714 and the time of the phase change as about 1.3$t_{1/2}$. This implies that a new phase with a different rate of cooling onsets after 1.3$t_{1/2}$. The coefficient index$_2$ for this phase, according to the fitting by a broken power law, is about 0.2. This value is close to the value obtained for M4 dwarf flare (0.29) but it does not fit time profile values above 5$t_{1/2}$. This could be due to the impact of the evaporation of the heated chromospheric plasma to the flare time profile \cite[see, for example,][]{Fl2011SSRv} .
As predicted by the modelling of \cite{Allred_2006ApJ} for the 304~{\AA} band, the contribution of the evaporation for solar flare flux is more significant than for M dwarfs. Figure \ref{fig:304_allred} contains a comparison of the 304~{\AA} band and the appropriate model from \cite{Allred_2006ApJ}, where we can see the model flux drop below the observed flux at around $t=t_{1/2}$. Then the impact of chromospheric evaporation is seen in the form of an increase in the modelled flux. Although we note the model flux again drops below the observed flux for $t>2t_{1/2}$.
\begin{figure}
	\includegraphics[width=\columnwidth]{res_model304.eps}
    \caption{ Comparison of the obtained time profile of solar flare emission at 304\AA~with result of modelling by Allred et al. (2006).}
    \label{fig:304_allred}
\end{figure}

In the case of fitting for t1=[0, 0.5]$t_{1/2}$, the relation between the decay coefficients of the first phase for the 1600~\AA, 304~\AA \ and 1700~\AA \ bands confirms that the temperature of the emission formation is as discussed above. The value of $t_{\textrm{\scriptsize{break}}}$ in the broken power-law fitting characterises the transfer from the radiative cooling to the contribution of chromospheric evaporation.  We obtained the lowest value of $t_{\textrm{\scriptsize{break}}}$ for the 1700~\AA~band (1.282) and the highest value for the 1600~\AA~band.
This is the same ordering as suggested by the temperature-height model of the solar flare atmosphere. An alternative way to specify a temperature-height model is through an analysis of the delay between maximums of flare emission in different spectral ranges. The delay between signals obtained in the UV and EUV bands are actively used for analysis of height-temperature dependence of solar atmosphere over the sunspot \citep[see,][]{Reznikova2012ApJ}. As one can see in Table \ref{tab:table0}, the delay between the maximum of flares in 304\AA~ band and 1600\AA~ band can be both positive and negative. The most common time delay was 17 seconds but a group of events demonstrated a negative delay of about 7 seconds. The uncertainties related to an image cadence of 24 seconds are 14 seconds (using the same approach as  \cite{Reznikova2012ApJ}). Thus we can conclude that negative delays are within error bars, and most of the positive delays are around this value. Such small delays, close to the level of uncertainties, agree with classical F1 and F2 flare models by \cite{Machado1980ApJ} suggesting a height difference between the layers with temperatures corresponding to 304\AA~and 1600\AA~bands of about 3 km.

When fitting the two exponents to the median flare  profiles, we obtained two sets of parameters for each of the first and second phases by fitting over different time intervals (see Table \ref{tab:table1}). The difference between the parameters obtained for the same phase, but for the different time intervals, exceeds the parameter uncertainty. Thus, it is necessary to determine which time intervals should be fitted to best represent the cooling processes. We believe that the decay during the second phase should be fitted using parameters obtained for t2~=~[3, 10]$t_{1/2}$ because the flux takes longer to decay in the solar atmosphere compared to the M dwarf flare profile. To reveal the decaying related to radiative and thermal conduction losses during the first phase, we should avoid the chromospheric evaporation contribution to emission. As mentioned above, the breakpoint, $t_{\textrm{\scriptsize{break}}}$ in the broken power-law fitting parameters characterises the transfer from the radiative cooling to the contribution of the chromospheric evaporation. For both the 1700 {\AA} and 304 {\AA} bands, the obtained values of $t_{\textrm{\scriptsize{break}}}$ were below 1.5. While, for these bands, the parameters obtained by fitting the different time intervals showed a significant difference, the parameters obtained by fitting the different time intervals for the 1600 {\AA} band, where $t_{\textrm{\scriptsize{break}}}$ was above 1.5, did not demonstrate a significant difference. All these facts indicate the impact of chromospheric evaporation to time profiles is not negligible (depending on observational wavelength), meaning that fitting over the interval t1~=~[0, 1.5]$t_{1/2}$ is not appropriate and the range t1~=~[0, 0.5]$t_{1/2}$ is favourable.

Based on a comparative analysis of the fitting results for solar and M dwarf flare templates, we can conclude that, for the Sun, the optimal template describing cooling processes consists of two exponents, fitted for t1~=~[0, 0.5]$t_{1/2}$  and t2~=~[3, 10]$t_{1/2}$ respectively.

We note that the second cooling phase of solar flares turned out to be more complicated than for M4 dwarf flares. The cooling of the 304~\AA~band during the second phase is marginally faster than for the 1600~\AA~band, which is hotter and originates from less dense plasma. It is possible that, during cooling the relative contribution of spectral lines with different temperatures to the emission of the 1600~\AA~band changes with time, which results in a faster decrease of emission flux. We also would like to note that the 304~\AA~band time profile demonstrated unusual behaviour. As emission of this band mostly forms by the emission of a single spectral line \citep{ODwyer2010A&A}, its time profile should be more akin to density evolution \citep[][]{Aschwanden2009ApJS}. This fact is confirmed by modelling \citep[see][]{Allred_2006ApJ}. However, the observed time profile shows an exponential decay, which is more characteristic of temperature evolution.

\begin{figure}
	\includegraphics[width=\columnwidth]{RC_model1600.eps}
		\includegraphics[width=\columnwidth]{RC_model1700.eps}
			\includegraphics[width=\columnwidth]{RC_model304.eps}
    \caption{Average (median) time profiles (black) fitted by functions of temperature evolution depended on radiative( blue) and conductive (red) losses.}
    \label{fig:model_fit}
\end{figure}

As mentioned above, there are two processes, namely thermal conduction or radiation losses, and domination of one of the process over the other would result in different behaviours of temperature. The temperature evolution during radiative cooling can be described as  $T(s,t)=T_0(s)[1-(1-\alpha)t/\tau_{r0}]^{1/(1-\alpha)}$, where $\tau_{r0}$ is the radiative cooling time at the start of the radiative phase, $\alpha$ is the coefficient of radiative losses function and $s$ is the coordinate along the magnetic field \citep[here and after,][]{Cargill1995ApJ}. The coefficient $\alpha$ is assumed to equal to -0.5 for log(T)>5. As the temperature range of the data analysed here is less this value, we cannot use this assumption. The dependence $T(t)=T_0(1+t/\tau_{c0})^{-2/5}$ describes the temperature evolution for the case of static conductive cooling (where $\tau_{c0}$ is the conductive cooling at the beginning). We performed fitting using these two functions for the analysed spectral bands, using $\tau_{r0}$, $\tau_{c0}$ and $(1-\alpha)$ as variables. The results can be seen in Figure~\ref{fig:model_fit}. The averaged time profiles for all bands are better fitted by the function corresponding to radiative cooling. Only the 304\AA~ band time profile demonstrates good agreement with the fitting based on conductive cooling for a short time interval when $t< 0.1t_{1/2}$.

\section{Conclusions}\label{sec:conclusions}
Based on the results of reconstruction and analysis of averaged time profiles of solar flare decay phases obtained within 304~\AA, 1600~\AA~and 1700~\AA~spectral bands, we can conclude the following:
\begin{itemize}
\item The processes of cooling during the decay phase of solar flares are the most closely described by fitting of a combination of two independent exponents for t1~=~[0, 0.5]$t_{1/2}$  and t2~=~[3, 10]$t_{1/2}$.
\item The parameters obtained for the 1700~{\AA} solar flare time profile, which is theoretically closest in temperature to the M dwarf flares, are consistent with models that imply that the white light M dwarf flare emission is formed in a higher density of layer.
\item Fitting a broken power-law model allows the contribution of chromospheric evaporation to be taken into account. However, it is not sufficient for a full description of the second part of the decay phase.
\end{itemize}

\section*{Acknowledgements}

This research was partly supported by the grant of the Russian Foundation for Basic Research No.~17-52-10001. A.M.B. acknowledges the support of the Royal Society International Exchanges grant IEC/R2/170056. This research was partly supported by the budgetary funding of Basic Research programs No. II.16 (LKK).

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


text:
Aleurolobus azadirachtae es un hemíptero de la familia Aleyrodidae, con una subfamilia: Aleyrodinae. Fue descrita científicamente en 1993 por Regu & David.

Referencias

azadirachtae

redpajama_set_name: RedPajamaWikipedia


When Comerford Foley was first founded five years ago, we had grand plans for our brand new accountancy firm – and 2016 has been a year that's seen us making great strides towards our goal of being the most progressive accountant in Waterford County, and further afield across Ireland and the UK.
When you're focused on pushing your business forward, it's easy to lose sight of how far you've travelled. So we thought we'd take a step back and look over the past 12 months to see just how much has changed at Comerford Foley in 2016 – and how much better we can help your business to become its own success story too.
One huge change has been our move to new office space in Tramore. We'd founded Comerford Foley from our initial HQ in Dunhill, but as time went on, and we expanded our team, it became clear we needed bigger offices with more space and room to grow the Comerford Foley family to meet our clients' needs.
We're now happily set up in our newly refurbished offices at Riverstown Business Park, and it's been great to spread out, have more room for face-to-face client meetings and become a focal point of the local Waterford business community.
We ended 2015 as a team of six, and over the course of 2016 we've expanded to a larger, more robust staff of ten people! You can read more about everyone on our About us page.
Derek Lowry has joined the team to head up our corporate finance and business solutions. He's got 14 years' experience of working with businesses to help them improve their financial performance, which allows us to offer your business a completely rounded accounting and business advisory package.
Ewelina Cooke has joined us as our first accounting trainee, after completing her Bachelor of Business and Higher Certificate in Business Studies from Waterford Institute – and bringing some international flair to the office with her Polish background.
Anne O'Hanlon joined us to assist with increased administration, and is a support and help to the whole team in our new offices.
Ludmila Zaharia expanded her role, becoming a tax trainee during 2016. Originally from Moldova, Ludmila has completed her ACCA qualifications and is now a specialist in Irish tax and tax planning.
Finally, Darragh McCormack has joined us, bringing his accounting, audit, tax and business advisory skills to the table – and working closely with clients to help them move forwards and become more profitable. He has over 13 years of experience in helping clients and brings a wealth of technical accounting and tax knowledge to the team.
Growing the team has made such a difference, allowing us to expand our services, deliver a wider range of advice and help you – our business clients – to get on top of the big picture of strategic planning, profit improvement and long-term success.
It's not just the firm that's been growing – so have some of our families. Jane gave birth to her first child – a bouncing baby boy called Fionn, back in April, and has been juggling her new role of 'mummy' alongside managing her pivotal role in the firm. We hear that 3am feeds are marginally easier than year-end tax returns!
Colin ran not one, but two marathons this year – Rotterdam in April, and Dublin in October. This is quite an achievement when you're also heading up such a busy accountancy business, being a family man and still having time to fit in those early morning training runs. This was part of a group that raised money for multiple local charities during 2016. We're proud of Colin, although you may not see the rest of us racing him to the finish line. We are happy to be proud from the sidelines.
And Ewelina and Ludmila have both had their noses in the text books, working through their training and learning even more about how to help you and your business to get on top of your finances.
Lastly (and very much not leastly) we've been working with the team at the Profitable Firm agency to refresh our logo, update our brand colours and design the wonderful new website you're reading this blog on.
You're on the site now, so look around – we hope you agree that it's much easier to find our services and start getting to know the team.
So, there you have it. 2016 has been a year of change, growth and evolution for us as a firm, and we're looking forward to 2017 and working even more closely with you and your business.
We're planning great things for the next 12 months, and we can't wait to help your business get a better handle on financial management, profit improvement and building the best possible business you can for the New Year.
We'd like to extend a big thank you to all our clients, friends and family for their continued support this year – we wouldn't be where we are without you.
Have a very merry Christmas and a happy New Year, from all of us at Comerford Foley!


You can Contact Brian Houchins who has selected the price option to be PayWhatULike. This means you decide the price and expiry date to send Brian Houchins a message but it must be $1 or more. If your message is not read before it expires, you can get your money refunded.


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Aug 4, 2022 - Politics & Policy
DOJ sues Peter Navarro over Trump White House emails
TuAnh Dam
Former White House adviser Peter Navarro. Photo: Drew Angerer/Getty Images
The Department of Justice is suing former White House adviser Peter Navarro for emails from a private account he used while working for former President Trump and for allegedly "wrongfully retaining" those communications, according to court documents.
Why it matters: The lawsuit is an unusual move by the DOJ's Federal Programs Branch — which typically pursues civil matters — targeting alleged sloppy federal records maintenance from the previous administration, per CNN.
What they're saying: The suit alleges that Navarro "refused to return any Presidential records that he retained absent a grant of immunity for the act of returning such documents."
"Mr. Navarro is wrongfully retaining Presidential records that are the property of the United States, and which constitute part of the permanent historical record of the prior administration," the suit continued.
The other side: Navarro's lawyers told The Hill that he "never refused to provide records to the government."
"As detailed in our recent letter to the Archives, Mr. Navarro instructed his lawyers to preserve all such records, and he expects the government to follow standard processes in good faith to allow him to produce records. Instead, the government chose to file its lawsuit today," his attorneys added.
Of note: Navarro had previously been indicted for contempt of Congress for refusing to comply with subpoenas from the House select committee investigating the deadly Jan. 6, 2021, U.S. Capitol riot.
Navarro refused to give testimony or produce documents in compliance with the subpoena.


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While the parade of flowers may be finished for the year, the gardener is not. It's time to clean out flowerbeds and put away garden décor and equipment.


text:
import { dep } from 'worona-deps';

export const reducerCreators = {
  get objectCreator() { return dep('subscriptions', 'reducerCreators', 'objectCreator'); },
  get isReadyCreator() { return dep('subscriptions', 'reducerCreators', 'isReadyCreator'); },
};

export const sagaCreators = {
  get collectionWatcherCreator() {
    return dep('subscriptions', 'sagaCreators', 'collectionWatcherCreator');
  },
};

redpajama_set_name: RedPajamaGithub


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The Penn Law School Mob Scores a Victory
The Wall Street Journal March 19, 2018
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Now Black Lives Matter wants Amy Wax fired for arguing that preferences harm their 'beneficiaries.'
The campus mob at the University of Pennsylvania Law School has scored a hit. Prof. Amy Wax will no longer be allowed to teach required first-year courses, the school's dean announced last week. Now the leader of Black Lives Matter Pennsylvania wants Ms. Wax's scalp. According to a weekend newspaper report, if she isn't fired within a week, "he plans to make things on the West Philadelphia campus very uncomfortable."
Ms. Wax's sin this time was to discuss publicly the negative consequences of affirmative action. Her punishment underscores again the dangers of speaking uncomfortable truths in a university setting.
The academic left has been gunning for Ms. Wax since last August, when she co-wrote a Philadelphia Inquirer op-ed calling for a return to the "bourgeois culture" of the 1950s. She was branded a white supremacist for advocating personal responsibility, even though the op-ed criticized "the single-parent, antisocial habits, prevalent among some working-class whites."
Half the Penn law faculty signed an open letter denouncing the op-ed. The dean, Ted Ruger, asked her to take a leave of absence and stop teaching her first-year course, Ms. Wax wrote last month in this newspaper. She declined his request. (The law school denied her account and said the discussion was merely "about the timing of a regularly-accrued sabbatical.")
The latest outrage arises from a web video Ms. Wax recorded in September with Glenn Loury, an economist at Brown University. Forty or so minutes in, the discussion turned to racial preferences. Mr. Loury noted that, on average, students admitted via preferences "are less academically qualified—by definition!" Ms. Wax brought up the "mismatch" effect: the idea that the so-called beneficiaries of preferences have difficulty competing with peers who were admitted without them. "Take Penn Law School, or some top 10 law school," Ms. Wax said. "Here's a very inconvenient fact, Glenn. I don't think I've ever seen a black student graduate in the top quarter of the class and rarely, rarely in the top half. I can think of one or two students who've scored in the top half in my required first-year course."
Ms. Wax added that she teaches a "class of 89, 95 students" each year, "so I'm going on that because a lot of this data is of course a closely guarded secret." That is an understatement. Schools pay fanatical attention to the racial makeup of their student bodies, then work just as fanatically to conceal the resulting gaps in qualifications and subsequent academic achievement.
Ms. Wax suggested that preference beneficiaries would do better in colleges where their academic preparation equaled that of their peers. "If they were better matched, it might be a better environment for them," she said. "We're not saying they shouldn't go to college. We're not saying that. I mean, some of them shouldn't." The statement that some college students would be better off in vocational training or work is true for all races, particularly for the millions who drop out before getting a degree.
The video had been online for months before someone at Penn got wind of it. Cue an alumni and student petition protesting Ms. Wax's "disparaging, false and deeply offensive claims."
The petition worked. In the campus email last week announcing Ms. Wax's removal from first-year teaching, Mr. Ruger denounced her claims as false: "Black students have graduated in the top of the class at Penn law." At the same time, he insisted that Penn does not "collect, sort or publicize grade performance by racial group."
Although Ms. Wax's statements were general, Mr. Ruger accused her of violating the school's confidentiality policy and conscripting students in the service of her "musings about race in society." He also accused her of saying that some black law students at Penn shouldn't "even go to college," when she was speaking of the mismatch problem more broadly.
Though couched as a subjective perception, Ms. Wax's casual observations about the mismatch effect at Penn were too sweeping—there have undoubtedly been some black students in the top quarter of the class—and she might want to correct that overstatement. But the mismatch effect is absolutely real, at Penn and elsewhere. In the early 1990s, the Law School Admissions Council tracked 27,000 students at nearly 90% of all accredited law schools. Of the 2,000 students attending the most "elite" law schools, 52% of blacks were in the bottom tenth of their class, compared with 6% of whites. Only 8% of blacks were in the top half of their class. Bar failure rates were also skewed; the LSAC data showed that 19% of blacks graduating from these elite schools failed the bar, compared with 3.5% of whites.
In 1995 UCLA law professor Richard Sander gathered GPA data on first-year law students at 19 law schools, including Penn. Though the number of self-identifying black respondents from Penn was small, the patterns there closely tracked those in the LSAC data set. There is no reason to think anything has changed.
Mr. Ruger has accused Ms. Wax of a "conscious indifference" to the truth. The burden is on him to disclose the data that prove her thesis wrong. It is conceivable that to maintain plausible deniability about the effects of its racial preferences, Penn does not collect or analyze data on the performance of black law students. That information, however, would be easy to assemble.
The diversity industry has given notice: Discuss the costs of affirmative action, and you can be punished and publicly shamed. The real scandal is not what Ms. Wax said but that schools refuse to be transparent about admissions policies that impede students' success.
This piece originally appeared in The Wall Street Journal
Heather Mac Donald is the Thomas W. Smith fellow at the Manhattan Institute, contributing editor at City Journal, and the author of The War on Cops.
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The Military Industrial Complex is a term coined by President Dwight D. Eisenhower to describe the web of policies and monetary relationships between legislators, national armed forces, and the military industrial base. The articles in this category address the relationship between our legislators and the lucrative defense contract industry.
WJ Astore: Three Ford-class carriers will cost at least $43 billion (despite the $4 billion "savings"), but you hear few dissenting voices in Congress.
WJ Astore: Instead of toughness, Trump as president has proven to be the Pentagon's lackey.
WJ Astore: How much money will satisfy America's military-industrial complex? If $733 billion is a "floor," or a bare minimum for national defense spending each year, how high is the ceiling?
Tom Hastings: To create more jobs, to create more educational opportunities for our young people, vote for candidates who will cut military spending and increase education.
Brent Budowsky: Believers in freedom and democracy owe a profound debt to Defense Secretary Mattis, who towers above all others inside the Trump administration as a bulwark of the democratic alliance.
W.D. Ehrhart: Currently, the US military maintains 800 bases in 70 countries worldwide with US forces stationed in another 60 countries. What are we doing in all these places? Most Americans do not know, and do not care.
Why Is It Bad News When Military Spending Declines?
WJ Astore: The sober, sane, thing to do, according to military experts, is always to expand military spending.
Kristin Christman: What's the use of all that science in developing weapons if there's no science in evaluating the application of weapons to real world problems?
Does the fact that society struggles with defining an age of majority (i.e. legal adulthood) have implications on the ethical age at which someone should be deemed responsible and capable of being a member our nation's military and projection of deadly force?
Lawrence Wittner: Although two out of three Americans oppose increasing Military spending, the U.S. government is boosting it to record levels.
Jaime O'Neill: Just one of Donald Trump's golfing trips to his Mar a Lago property costs more than the annual budget for Meals on Wheels, the program Republican eliminated that delivered meals to low-income seniors.
WJ Astore: Ike knew that national safety shouldn't be equated with military prowess; quite the reverse, as he warned us against the unchecked power of a burgeoning military-industrial-Congressional complex.


Rating: 9.06 from 31 votes.
In 1994, Kurt Cobain was riding on the top of the world as the creative genius behind the biggest rock band in the world. However, the singer/songwriter was notoriously full of personal demons as he struggled with depression and substance abuse. Tired of the rigors of fame and the pressure of the mainstream music industry, Kurt Cobain shot himself.
Soaked in Bleach challenges this established narrative of Cobain's death as a suicide. Interviews of various people surrounding the circumstances including private investigator Tom Grant (whom Kurt's wife, Courtney Love, hired to find Kurt right before his body was found), Seattle Police Chief Norm Stamper, and Rosemary Carroll who served as Cobain and Courtney Love's attorney. The film looks to examine inconsistencies in the idea that the Nirvana singer succumbed to depression and killed himself. Instead, the filmmakers focus on examining the possibility that foul play was involved.


One need not be a substance abuser to attend; rather, we invite anyone seeking support and friendship. All our meetings are "open".
The Capuchin Soup Kitchen also sponsors Jefferson House, a twelve-bed, residential treatment facility for indigent males seeking to reclaim their lives from addictions. Residents normally complete their rehabilitation in six to nine months. During that time they learn to practice honesty, courage and other virtues essential to recovery and to the development of a sober, healthy and happy life. They participate in twelve-step recovery meetings, and are encouraged to continue such participation following their departure from Jefferson House. The program also provides opportunity to work at other Capuchin Soup Kitchen locations, for which the men are paid a modest stipend. New residents to Jefferson House are admitted via referral from inpatient substance abuse treatment programs. Jefferson House is accredited by CARF International and is one of the top 3% of therapeutic communities who received no recommendations for needed program revisions during CARF's most recent triennial accreditation review.
Call for an admission interview. Admissions on a bed-available basis.
Business Hours - 9:00 a.m. - 5:30 p.m.
The Capuchin Soup Kitchen's Jefferson House advisory council member thinks the world of J-House and all that it does for people.


text:
Q: When does the while loop check for its condition Hi I have something like:
Version 1:
bool noErrors = true;
while(noErrors)
{
   noErrors = ValidateControl(txtName);

   // other code
}

Version 2:
bool noErrors = true;
while(noErrors)
{
   if(!ValidateControl(txtName)) break;

   // other code
}

I use this code to validate a form and if the validation returns false, I want to break before executing "other code". Since I do not know when the loop checks for its condition, I do not know which makes more sense. Should I use the first or the second version, or maybe a third one?
Thank you for your time

A: Version 2 will break before running the //other code. Version 1 will not check until the start of the next iteration.
bool noErrors = true;
while(noErrors)
{
    noErrors = ValidateControl(txtName);
    // other code
}

Checks before each iteration.
bool noErrors = true;
do
{
    noErrors = ValidateControl(txtName);
    // other code
} while(noErrors);

Checks after each iteration.
Neither check during an iteration. As stated by the other answerers, the following code simplifies the example but makes me ask the question, is the validity of txtName likely to change during the execution of the loop? Would some other limiting condition be more useful?
while (ValidateControl(txtName))
{
    // other code
}

If the validity of txtName will not change, consider,
if (ValidateControl(txtName))
{
  while(/*Some other condition*/)
  {
      // other code
  }
}

A: The condition is only ever checked at the start of any possible iteration. So in version 1 the "other code" would be executed even if noErrors has been set to false in the first line of the body... whereas in version 2 it wouldn't... but noErrors looks like it's somewhat useless in version 2.
Could you change it to:
while (ValidateControl(txtName))
{
    // other code
}

?

A: A while loop evaluates its condition before the first iteration, and inbetween each subsequent iteration. The condition is never evaluated inside the loop body.

A: It checks it before running again (first time, after first run and so on). You have to break or whole chunk of code will run.

A: The while loop checks the condition before it iterates over the block of code that it precedes. You can also make it check the condition at the end by using a do-while construct. Your version #2 will produce the result you desire.

A: The while loop checks the condition before executing the entire code block.  If you want to break execution before the other code is executed, use Version 2.

A: The loop condition is only evaluated at the start of each loop, so in your first version, the "other code" will still be executed, even if ValidateControl returns false.
Your second version works better, and will not run the "other code" if ValidateControl returns false, however it also does not set noErrors to false if the validation fails. If that's not important, and noErrors is only the loop condition, then you might as well change your while loop to while(true), if it is used later in the code, then you'll need to change version 2 slightly:
bool noErrors = true;
while(noErrors)
{
    if(!ValidateControl(txtName))
    {
        noErrors = false;
        break;
    }

    // other code
}

A: If this is in a validation routine, I wouldn't even BOTHER with a WHILE() construct...  In the past, I would typically test each specific validation routine that did just that... no looping involved such as
Function bool IsAllDataValid()
{
    if ( ! (ValidateControl(txtName) )
        return false;

    if ( ! (ValidateControl(OtherField ))
        return false;

    etc...

    return true;
}

Then you don't have to worry about where the mix is of include or bypass certain blocks of code...  You could just have...
if IsAllDataValid()
{
   Do Your Other Code
}

redpajama_set_name: RedPajamaStackExchange


text:
Black Love
This is just….everything.
Posted on February 23rd, 2011 - Filed under Hot Videos
Tags :: black beauty, black bodies, black love, dark skin, naked, nude, nudity, Til the End of Time, Timothy Bloom, V. Bozeman
On the Color Caste, or; Are You Light Enough in Here?
I've often said to folks that the biggest thing holding black folks back was not racism or white supremacist thought, but the degree to which we have collectively internalized racism and white supremacist thought.
There is a difference.
In most circles, internalized racism is known solely as self-hatred. But this is a very amorphous term, self-hatred. In reality, the politics of race, gender, and class are understood to be much more complex. A lot of black people do wonderful things for the community, mentor young blacks, live "upstanding" lives, but still unconsciously uphold white supremacist ideals.
This is most prevalent in the realm of aesthetic beauty. We as black people, far more than white folks it would seem, have bought into white supremacist beauty standards. And it is such a widespread phenomena that entire industries base their decisions on how much we devalue black beauty.
What this means is that black folks who have Eurocentric features are far more likely to be successful, both in the larger culture and the black community, than those who's features are coded as "African" or "ethnic".
The success of Beyonce is a well-known testament to this fact. Matthew Knowles studied well from the Berry Gordy school of economics. Destiny's Child was created so that any of the four (then, three) girls could be a little girl's favorite. This is why all the girls' hair color, especially in the beginning, was different. But Matthew Knowles knew that Beyonce, as the lightest, would be the most "captivating" girl — simply because she was lightest. So she was made the front-woman. And she was lightened in magazines and given blonde hair.
This was very purposeful on Matthew Knowles' part. It was not just some arbitrary decision. It was a conscious choice. He understood the color struck black bourgeoisie and White America. He knew black folks would hail her as a beauty, the way Halle was hailed before her. He also knew little white girls would see a little of themselves in her and "identify."
Let's face it, there is a reason that Halle Berry, Beyonce, and Alicia Keys are the only black women to get on the covers of major magazines last year — they are relatively light-skinned women.
Of course, the tragic irony is that all three of these women are darker than they appear in magazines. They are always lightened for magazines, particularly when featured in a high-end magazine.
Now, it's important to impress upon people that a discussion of the way in which light-skinned women are perceived is not to slight their talent or their skill or their accomplishments. We must begin to understand the reality that the avenues to success are not the same for all black people. Light-skinned women are accepted as beautiful before darker-skinned women.
This was readily apparent in the most recent season of America's Next Top Model. The last three finalists were Nicole (a white girl with brown hair), Nik (a light-skinned black girl, possibly biracial, with blondish hair), and Bre (a dark-skinned black girl from Harlem).
Bre was always presented as angry and unrelenting. And she was always coded as "street." Every single time she came before Tyra and the judges, euphemisms for "dark" and "black" were used to describe her. And such descriptions were both good and bad depending, mostly, on how her competitors were judged. So when the white girls were kinda bland or boring or generic, Bre's "edginess" made her standout. When the other girls were "fierce", then Bre was "too edgy".
What this means is that while the other girls were competing against each other, Bre was competing against the other girls and herself — her blackness.
We have to become aware of the way that competition was set up to be much more difficult for Bre. The last competition was a Cover Girl photo shoot. Cover Girl, for decades, didn't use black models–of any hue. Cover girls are the "all-American girl", which is nearly always coded as "white."
Now, the reality that Cover Girl doesn't even make products for darker complexions should be a well-known fact and should have been a signal to viewers of the show that something was off about the competition.
Of course, Bre wouldn't win. Not over Nicole and Nik who are the kind of "look" that one normally associates with Cover Girl.
Many responses to this season talked about racism but only because Nik wasn't picked. The reality that on BET.com and other black websites, black folks were saying Tyra was racist for not picking Nik is a sad testament to the reality that we so narrowly understand the complexity of racism and how we've internalized it.
For most black people, Bre's loss made sense. She wasn't good enough. She was too "edgy." She had "too much attitude." She was too "street." Nearly every blog or webposting or review talked about Bre as having "too much attitude" as if models are the sweetest girls on the planet.
All this means is that Bre was too black.
A friend of mine, Mikey , told me that there have been more dark-skinned supermodels than light-skinned and that means that Nik should have won. He is right.
But what folks have to understand about skin colors in modeling is that dark-skinned models were always shown to be exotic, not beautiful. Exoticization is not beauty. They are not synonyms. When it comes to beauty, or white supremacist standards of beauty, dark-skinned women are at a disadvantage.
Bre could never have won that contest. It was designed to be unfair to her. Whether or not it was purposeful is irrelevant. That is what internalized racism means; it's not on purpose.
Tyra, as the executive producer, would probably say that Bre wasn't "versatile" enough. This is just sidestepping the issue. The reality is that the show was rigged to make the competition harder for Bre. Tyra knows better than anyone how hard it is for darker-skinned models and she played the game well for the last 15 or so years (with the weave and sublimating black vernacular in her speech).
Now that she's retired, she's crying on her talk show about how hard it was for her and how she wants to make it easier. But she's not doing that. She's playing by the rules of the modeling industry that says if you are non-white you better look a little white or work the weave. And if you are black, you can't be "too black."
Darker-skinned women shouldn't have to be "versatile." They shouldn't have to sublimate their blackness and try to look "all-American." Who they are should be enough. A diversity of beauty should be celebrated. Black beauty should not be acceptable only when it can be exoticized or "enhanced" by a few European features.
With people of color there are only two routes you can go in the modeling world — emphasize European features (in photos or with blonde hair or straight hair of any color) or exoticize non-European features.
This is what happened with the early darker-skinned models like Iman and Beverly Johnson where their blackness was always coded in opposition to white beauty, as exotic because it wasn't white beauty. Black folks think of it as just beauty, but in reality we did passively understand that the politics of opposition reinstates, reinforces, that whiteness is still the barometer of beauty, the penultimate.
Darker-skinned models' exoticization only serves to reinscribe the primacy of white beauty.
I say all this not to say that light-skinned women don't deserve their success. But we must begin to understand how we enable such success to occur by our overvaluing of lighter-skin. We need to understand that we don't champion our darker-hued women with talent enough. We need to, as my boy Mikey says, "love the spectrum" of blackness.
What that means is we need to have a darker counterpart to Beyonce, to Halle, to Alicia. It shouldn't be darker-skin = less sexy. But it is.
We need to change that.
There is a reason that 702 didn't explode, beyond discussions of whether or not their songs were any good. Meelah is a beautiful dark-skinned woman. As such, she doesn't have the same "appeal" that Beyonce did as lead singer of Destiny's Child.
The fact that we even have to "choose" is a testament to how the larger culture pits us against one another and only allows one person of color at the top at a time. It is perfectly legitimate to like both 702 and Destiny's Child, but that needs to occur to a degree that 702's label would feel obligated to promote 702 as much as Destiny's Child is promoted. So they would be on "equal" footing.
With black artists, there is usually one star and then a bunch of "lesser talented" "lesser attractive" people pulling up the rear.
Why can't they all be on the same level, whatever that level may be?
What that means is, we need to show more love for darker-skinned people. This is not unfair. What you are doing is balancing the scale. It's called equity. By doing so, you are not devaluing lighter-skinned.
Think of it like a seesaw. For centuries light-skin has been getting all the love and reaping the rewards of society. Dark skin has been undervalued. So that means that the end with light skin on it is on the ground with dark in the air. By adding more dark to the side of the seesaw with dark skin on it you start to level the seesaw.
This is equity. You aren't lessening light skin, you are balancing.
Posted on January 7th, 2006 - Filed under Culture,Music
Tags :: Alicia Keys, America's Next Top Model, Berry Gordy, BET, Beverly Johnson, Beyonce, Beyonce Knowles, black model, colorstruck, Cover Girl, dark skin, Destiny's Child, Eurocentric, Halle Berry, Iman, internalized racism, light-skinned, Matthew Knowles, model, white beauty standards


Get ready for a showdown with the Carrera DIGITAL 132 GT Race Stars race set! This action packed set comes with two highly detailed 1:32 slot cars: a Ferrari 488 GT3 AF Corse and a BMW M6 GT3 Team Falken, both with real working headlights & taillights. High speed lane changing and passing is made easy with the 2.4GHz WIRELESS+ speed controllers which allow you to freely move around the 23+ foot track layout. The included control unit even allows drivers to set the top speed of each car.
The assembled GT Race Stars race track layout size is 10.01 x 5.58 ft and the running length is 23.95 feet.
All Carrera DIGITAL 132 race sets allow changing lanes and passing with up to 6 cars (for example, to expand this race set from 2 cars to 3 cars, requires the additional purchase of a Carrera DIGITAL 132 slot car and a DIGITAL 132 2.4 GHz WIRELESS+ speed controller).
Includes: 1 - Ferrari 488 GT3 AF Corse 1:32 slot car, 1 - BMW M6 GT3 Team Falken 1:32 slot car, 11 - standard straights, 8 - 1/60° curves, 1 - DIGITAL 132 double lane change track, 1 - DIGITAL 132 left lane change curve, 1 - DIGITAL Control Unit w/ connecting track, 2 - 2.4 GHz WIRELESS+ speed controllers, 1 - 2.4 GHz WIRELESS+ receiver, 1 - 2.4 GHz WIRELESS+ double charging station, 2 - Lithium-polymer batteries for speed controllers, 1 - AC/DC transformer, bridge supports, 52 - track section bolts, 4 - guardrails, 28 - guardrail supports, 4 - replacement contacts and instructions.


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In emergency rooms, especially in the case of acute symptoms, the central dogma of patients' treatment effectiveness consists of rapid disease diagnosis and subsequent targeted cure. Personalized medicine is progressively acquiring importance for both of these purposes and for drug development. In turn, a deeper knowledge of each individual's metabolome is becoming important for defining individual phenotypes. In recent years, analysis of the human metabolome through the systematic study of bio-specimens (biofluids, tissues, etc.) has strongly developed.
Precision medicine may significantly contribute to rapid disease diagnosis and targeted therapy, but relies on the availability of detailed, subject specific, clinical information. Proton nuclear magnetic resonance (1H–NMR) spectroscopy of body fluids can extract individual metabolic fingerprints.
In this project, we studied 64 patients admitted to the Florence main hospital emergency room with severe abdominal pain. A blood sample was drawn from each patient at admission, and the corresponding sera underwent 1H–NMR metabolomics fingerprinting. Unsupervised Principal Component Analysis (PCA) analysis showed a significant discrimination between a group of patients with symptoms of upper abdominal pain and a second group consisting of patients with diffuse abdominal/intestinal pain. Prompted by this observation, supervised statistical analysis (Orthogonal Partial Least Squares–Discriminant Analysis (OPLS-DA)) showed a very good discrimination (>90%) between the two groups of symptoms. This is a surprising finding, given that neither of the two symptoms points directly to a specific disease among those studied here. Actually herein, upper abdominal pain may result from either symptomatic gallstones, cholecystitis, or pancreatitis, while diffuse abdominal/intestinal pain may result from either intestinal ischemia, strangulated obstruction, or mechanical obstruction. Although limited by the small number of samples from each of these six conditions, discrimination of these diseases was attempted. In the first symptom group, >70% discrimination accuracy was obtained among symptomatic gallstones, pancreatitis, and cholecystitis, while for the second symptom group >85% classification accuracy was obtained for intestinal ischemia, strangulated obstruction, and mechanical obstruction. No single metabolite stands up as a possible biomarker for any of these diseases, while the contribution of the whole 1H–NMR serum fingerprint seems to be a promising candidate, to be confirmed on larger cohorts, as a first-line discriminator for these diseases.