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text:
\section{Introduction}
Solar radio emission is connected with solar magnetic activity, which maintains plasma acceleration and heating processes manifesting themselves in various dynamic events \citep{Mclean1985,Aschwanden2005}. The radio observational instruments are able to detect the related electromagnetic radiation in the form of different kinds of type II, type III, type IV radio bursts, and others \citep{MC1985,Mel2005}, carrying information about their source dynamic events. Among them, type III bursts are produced by energetic electrons, which propagate along magnetic field lines in the solar corona \citep{suzuki85,sinclair2014,Melnikkon08}. These particle beam sources of  type III bursts are thought to originate from eruptive processes in the solar atmosphere related to magnetic reconnection. On the other hand, type IV bursts are clearly associated with the onset and propagation of Coronal Mass Ejections (CMEs) \citep{stewart85,melnik08}. The types of radio bursts under consideration represent important diagnostic tools for the remote study of density profiles, properties of solar radio emission sources, and other physical characteristics of the solar atmosphere \citep{bougeret,Mann99,sinclair2014,melnikboiko11}.

Before we turn to the analysis of the observations, it is important to note that type III radio bursts are believed to be excited by several known plasma generation mechanisms \citep{Ginzburg58}. It is supposed that fast electrons generate Langmuir waves along their propagation. Furthermore, the excited Langmuir waves ($l$) can be involved in dynamic processes that result in the excitation of electromagnetic waves, with a characteristic frequency close to  that of local electron plasma. On the other hand, it is well known that meter and decimeter bands of radio emission spectra of  type IV bursts are characterized by a clear internal structure manifested through the so-called zebra pattern of spectrum and fiber bursts \citep{chernov2006,stewart85}.
It is conventionally accepted that one of the possible mechanisms for the creation of fiber bursts involves three wave-wave interaction processes of the form $l+w \rightarrow t$, where $w$ denotes the low frequency whistler modes \citep{rausche,chernov,kuijpers}.
The physical mechanism of the excitation of type IV radio bursts is related in most cases to the onset of CMEs.

The main focus of this paper is the observational study not of the fiber burst or zebra pattern structures of  type IV bursts, but instead the modified (narrow banded) type-III-like bursts within the decameter range of the spectrum that covers
the characteristic frequencies $8-32\;$MHz. These modified type-III-like bursts are detectable on top of type IV busts and seemingly undergo drastic influence from the latter. It is also well known that this emission most plausibly originates from higher altitudes in the solar atmosphere with rather lower density plasmas compared to its values at the solar surface. In agreement with previous studies \citep{gopals,antonov14}, we assume that the structured dynamic spectrum develops on top of background type IV radio bursts in the decameter range and can be a representation of radio bursts with similar morphological properties to usual type III bursts. Their spectral properties are significantly modified by the CME passage through the atmosphere and examination of this expectation is the main topic of current investigation. These specific radio bursts can be named as modified or narrow-band type-III-like bursts. Hereinafter, we refer to them as narrow-band type-III-like bursts. In the literature a number of other non-standard type III radios bursts such as type IIIb or type IIIl have been identified\citep{sinclair2014}. There was no significant number of type IIIb in our observational period of time, therefore we omitted them from the analysis. As regards the type IIIl bursts, according to \citet{cane2002}, are observed in low frequencies usually below $10\;$ MHz. Their duration can be several tens of minutes, which is significantly longer than the durations of our usual type III bursts. These bursts \citep{cliver2009} are associated to type II bursts, which were absent in our observational period. Therefore, the modified nosebanded type III bursts observed by us within the range $14-32\;$MHz cannot be identified as type IIIl bursts. In our case, the dynamic picture we have in mind is based on the assumption that there are regular sources of accelerated electron beams, which are generated mostly in the reconnection processes of closed magnetic field structures at lower altitudes (significantly far from our radio observational window). These electron beams then travel through the ambient plasma, in one case without a CME and in the other case with the presence of a CME, then they reach the heights in which we are interested (8-32 MHz observational window). This way in either of the cases the electron beams play the role of plasma probing agents, which produce a sequence of the type-III-like radio bursts with different spectral properties before, during, and after the CME. Consequently, the key object of the current study is to perform a systematic comparison of the properties of the emitted type III bursts in those consecutive intervals of time. Hence, we base our further conclusions bearing in mind the fact that the type III bursts observed in the initial quasi-stationary atmosphere and during the CME propagation (with background type IV radio burst) could be characterized with similar parameters like frequency drift, duration, and instantaneous frequency bandwidth \citep{chernov2007,mlkonov08,koval2010}, and these parameters contain the information about the coronal and interplanetary plasma in which the CME is propagating.

The radio telescope Ukrainian Radio interferometer of National Academy of sciences--2 (URAN--2) observed a type III burst storm and type IV bursts on June 13, 2014. In the present paper, a comparative analysis of the mentioned different states of the solar atmosphere is carried out with the aim to detect and measure properties of the coronal plasma before, during, and after the CMEs. As a matter of fact, solar radio observations are used to explore the solar wind properties needed for the modeling of solar density profiles \citep[e.g., see][]{Mann99,newkirk61} and heating and/or acceleration processes \citep[e.g.,\ see][and references therein]{shergelashvili}. Another important aspect of the analysis carried out in this paper is the combination of the radio data with the optical observations. The research results reported here are an attempt to analyze solar radio emission, exploiting the radio dynamic spectra (patterns from the ground-based telescope URAN-2 (Ukraine, Poltava), see Fig.~\ref{spectri}), in combination with the CMEs' position and time evolution inferred from data from the space-based optical telescope The Large Angle Spectroscopic Coronagraph (LASCO) onboard of Solar and Heliospheric Observatory (SOHO); see Fig.~\ref{CME}). We observed a statistically significant number of radio bursts and investigated their parameters. Our observations and statistical analysis enabled us to determine the plasma density profiles and radial sizes of the emitting sources, before the onset and along the CME paths.
\section{Observations and data analysis}\label{observations}

The type III and narrow-band type-III-like radio bursts discussed in this paper have been analyzed using data from the radio telescope URAN-2 (Poltava, Ukraine). This instrument represents the phased array of effective area $28000\;$m$^2$ consisting of $512$ broadband cross dipoles operating at frequencies of $8-32\;$MHz. The observation time span covered from 04:15 UT until 14:55  UT of June 13, 2014. We selected this date because it was very rich in dynamical events and directly corresponded to our objectives, that is,\ we had periods without type IV bursts but populated with type III radio bursts, and periods including type IV radio bursts representing background for (as we call them) narrow-band type-III-like bursts, which have similar spectral morphological properties as usual type III bursts, but with significantly different characteristic values of their dynamic parameters, and are observed in periods with CME onset. In total we analyzed $558$ radio bursts, $429$ of which were usual type III bursts and the other $129$ are modified by CME propagation.
We divided the total time span of the observation into four consecutive periods. We selected two time intervals with no CME propagation: the window from 04:15 to 08:00  UT we call period~1, and, analogously, we have period~3, which lasted from 10:10 until 12:50 UT. Period~3 represents the time span following the two coupled type IV bursts of period~2, and one before the third type IV burst occurred in period~4.
Accordingly, we distinguish two time intervals where type IV-like patterns are observed:\ from 8:00 UT  until 10:10 UT (period~2) and from 12:50 UT until 14:55 UT (period~4). Furthermore, throughout the text the type III bursts observed in periods 1 and 3 are referred to as usual type III bursts and those observed in periods 2 and 4 as narrow-band type-III-like bursts. The difference in corresponding dynamical spectra is discussed below in connection with Fig.~\ref{burstsample}. Consequently, we were able to investigate the radio emission properties of bursts in observational periods preceding, during, and following the CMEs that occurred within periods 2 and 4 (see the picture of the whole observational day in Fig.~\ref{spectri}) and to perform a comparison of the statistics of the radio events within the different time intervals.

At the same time, a number of space-based optical telescopes such as the SOHO and the Solar Dynamics Observatory (SDO)  detected  two CMEs, namely CME~1 with start time 07:36 UT, (see panel~A in Fig.~\ref{CME}, source \url{www.helioviwer.org}), and  CME~2 with start time 08:24 UT (see panel~B in Fig.~\ref{CME}), during period~2. In period~4 another CME was detected, which we call CME~3, with start time  12:24 UT (see panel~C in Fig.~\ref{CME}).
Therefore, we associate these CME events with the type IV radio bursts we observed. Also, we interpret the radio spectra within period~2 as the double pattern structure of the type IV radio bursts. Hence, we subdivided period~2 into two sub-intervals:\ 8:00-9:00 UT, corresponding to CME~1, and 9:00-10:10 UT, corresponding to CME~2. This subdivision has been inspected by us during the analysis of frequency drift and durations and other parameters for narrow-band type-III-like bursts. As we show in panel A (blue dashed and red solid lines) of Fig.~\ref{driftgraph}, when we divide period 2 into two equal parts and draw the approximations of drift rate dependence on the frequency, we observe that characteristic values of drift rates differ from each other drastically. The drift rates within time interval 08:00 to 09:00 (blue observed datapoints and dashed line of linear regression) have about 1.5 times larger values than those in interval 09:00-10:10 (red observed datapoints and solid line of linear regression). We obtain similar significant differences of the magnitude and/or slope of the regression lines within these sub-periods for their durations and other physical quantities as well (see panel A in Figs.~\ref{durationgraph}, \ref{bandwidthgraph}, and \ref{rLbound}). These findings justify and give an indication that our subdivision of period 2 into two parts is reasonable, even though because of the overlap of the time spans of the CME1 and CME2, the type IV radio bursts associated with them are not immediately visually distinguishable in the dynamical spectrum. Our argumentation is further proved by comparison with period 4, where we have only a single CME. In the latter case, when we formally divide period 4 into two equal intervals such drastic differences in the properties of physical quantities do not appear (characteristic rates and regression line slopes are of the same order of magnitudes), what indicates that period 4 is occupied by only a single type IV radio burst. Further details of quantitative analysis can be found in corresponding sections below.
In general, we identify both period~2 and period~4  as periods of type IV radio bursts (CME onset and propagation), within which the narrow-band type-III-like bursts carry the information about the observed CMEs and state of the solar atmosphere.

In panel~A of Fig.~\ref{burstsample} we show examples of a type III radio burst observed within period 1 or 3. According to recent publications \citep{melnik08,melnikboiko11} it is conventionally accepted that the type III burst fluxes change over a very wide range,\  from a few solar flux units ($1\;$s.f.u.$\;=10^{-22}\;$W m$^{-2}$ Hz$^{-1}$) up to $10^6\;$s.f.u. In agreement with previously reported measurements, our observations also evidenced that in periods 1 and 3, corresponding to non-disturbed corona, the type III radio bursts are observed within wider frequency bands compared to the ones seen in periods 2 and 4. Besides, we estimated the corresponding total fluxes and observed that the average values of type III bursts vary between $6.3-6.7$ s.f.u. in respective periods 1 and 3, excluding rare instances of powerful type III bursts with fluxes of thousands of solar flux units. We plot the time profile of the flux corresponding to the burst shown in panel~B. On the other hand, narrow-band type-III-like bursts observed in periods 2 and 4 show mean characteristic larger fluxes of magnitude compared to periods 1 and 3, which is in good agreement with previously obtained data \citep{antonov14}. As we mentioned above, the narrow-band type-III-like bursts are seen on top of the background type IV bursts and represent the ground physical state of corona during CME propagation through it. In panel~C of the same figure, we demonstrate the part of the dynamic spectrum from period~2 that shows a set of narrow-band type-III-like bursts. As regards the corresponding total fluxes, their mean values are many times larger than ones for type III bursts in periods 1 and 3, and they amount to about $60-65$ s.f.u in period~2 and $30$ s.f.u in period~4, accordingly. Finally, we discovered narrow-band type-III-like bursts with positive drift rates as well, which could become the subject of a separate analysis complimentary to this current study. All these observed properties of the bursts are in good agreement with other similar measurements \citep{antonov14,mlkonov08}.

In our analysis we follow the strategy that comprises direct measurements of the frequency drift and duration rates and uncertainty errors of observed radio bursts in each observational periods. Then the rates of the instantaneous frequency bandwidth (IFB) and characteristic length scales of the radio emission sources (with errors) are evaluated by using these measurements of the drift rates and/or durations (see corresponding descriptions in subsections below). As is known, within the framework of the accelerated particles beam mechanism, the emission frequency is related  to the local plasma frequency $f_{pe} =\left ( {e^2 n_e}/{\pi m_e}\right )^{{1}/{2}}$,
where $e$, $n_e$ , and $m_e$ are the electron charge, the electron number density, and its mass, respectively.
We divided the observational frequency domain $8-32\;$MHz into six sub-bands: $8-12\;$MHz, $12-16\;$MHz, $16-20\;$MHz, $20-24\;$MHz, $24-28\;$MHz, and $28-32\;$MHz. Before we analyze the results of measurements, it should be noted that we were not able to find
a statistically meaningful number of bursts within the range $8-12\;$MHz. Therefore, we detected the physical quantities for the frequency sub-bands  only starting from $12\;$MHz and beyond. Then we calculated the occurrence rates of the frequency drift, duration, and IFB values within each mentioned frequency sub-band of the dynamical spectrum and plotted corresponding histograms  For the sake of brevity we demonstrate only one example of such a set of histograms for the case of the frequency drift for period 1 in Fig.~\ref{histdriftrate}.  For the frequency drifts, durations, and IFBs, similar procedures are applied in each observational period separately and corresponding histograms constructed. In order to derive the mean  values for each frequency sub-band, we performed a Gaussian function fit to the plotted histograms, variance of which also determined the original observational uncertainty errors of the detected mean rates (further details about the total error estimation are given below).

In Figs.~\ref{driftgraph}-\ref{rLbound}, we plot observed values of quantities and fitting lines for periods 1 and 2 in corresponding panels A, and for periods 3 and 4 in panel B, in order to make states of the solar atmosphere before and during the CME directly comparable to each other. It should also be  noted that each observed value shown by the asterisks in Figs.~\ref{driftgraph}-\ref{bandwidthgraph} is calculated as a mean value of the Gaussian fitted to the corresponding histogram. Also the uncertainty errors are calculated. These errors come from the variance of the fitted Gaussian and the linear regression performed over the computed mean values and are shown in Figs.~\ref{driftgraph}-\ref{bandwidthgraph} as black and colored lines, respectively. We take into account the additional uncertainty coming from the linear regression (and width of the observational frequency sub-band in a dynamical spectrum) as we consider in cases of drift rate (Fig.~\ref{driftgraph}) and IFB (Figure~\ref{bandwidthgraph}) the linear regression, which is rather rough for the measured mean values of quantities but still enough for the analysis carried out in this paper. Therefore we compromise on taking linear fittings instead of higher order polynomial or other functions, but we impose the extra uncertainty on top of the original one that come from the histograms. A similar procedure is taken for durations (Fig.~\ref{durationgraph}), however in this case the linear fitting is applied to data and frequencies in logarithmic scales as the final function we are looking for is the power law.

More specifically, for the error estimation in the measurements of drift rates and IFB we use the  expression
\begin{equation}\label{errordriftifb}
\varDelta Y _{drift,IFB}= \overline{\varDelta {Y_{obs}} +p_1 \varDelta f} \frac{\left \lvert Y_{obs}-p_1 f-p_2\right \rvert }
{\overline{\left \lvert Y_{obs}-p_1 f-p_2\right \rvert}},
\end{equation}
where $p_1$ and $p_2$ are the coefficients (their values are given in corresponding tables below) of the linear regression and overlines on top of the expressions denote the simple mean values of them.
In case of duration, we use the expression
\begin{equation}\label{errorduration}
\varDelta Y_{Duration} = \varDelta {Y_{obs}} + q_1\varDelta f\left \lvert  \frac{Y_{obs}}{f} +\frac{\varDelta {Y_{obs}}}{f} \right \rvert \exp \left ( \varDelta {\ln Y_{obs}}\right ),
\end{equation}
where,
\begin{equation}\label{erroryln}
\varDelta {\ln Y_{obs}} = \frac{\left \lvert \ln Y_{obs}-q_1 \ln f-q_2 \right \rvert}{\overline{\left \lvert \ln Y_{obs}-q_1 \ln f-q_2\right \rvert}},
\end{equation}
where $q_1$ and $q_2$ are the coefficients of the linear regression of duration vs. frequency, both in logarithmic scale.
Finally, we evaluate the errors of the emission source sizes in Fig.~\ref{rLbound} as
\begin{equation}\label{errorysource}
\varDelta Y_{Source} = 0.3c\varDelta Y_{Duration}.
\end{equation}
In all these expressions, $\varDelta f=2\;$MHz represents the half widths of the above-mentioned frequency sub-bands in dynamic the spectrum. Equipped with the outcomes of the data analysis procedures outlined so far, we turn to the description of the results for each physical parameter observed in further detail.

\begin{figure*}[h]
\begin{minipage}[h]{0.7\linewidth}
\center{\includegraphics[scale=1.4]{fig1.eps}}
\end{minipage}
\caption{Observational data (dynamic radio spectrum) of June 13, 2014  from 04:15 UT to 14:55 UT by URAN-2 (Poltava, Ukraine). Period~1 corresponds to the time interval 04:15 - 08:00 UT, period 2 to 8:00 UT - 10:10 UT, period 3 to 10:10 - 12:50 UT, and period 4 to 12:50 UT - 14:55 UT.}
 \label{spectri}
 \end{figure*}
\begin{figure*}[h]
\begin{minipage}[h]{0.7\linewidth}
\center{\includegraphics[scale=0.2]{fig2.eps}}
\end{minipage}
\caption{CMEs detected by the Solar and Heliospheric Observatory (SOHO) during our observation periods (source: www.helioviewer.org), which caused type IV bursts. Panels A (CME 1) and B (CME 2) correspond to period 2, and panel C (CME 3) corresponds to period 4.}
 \label{CME}
 \end{figure*}

\subsection{Drift rate}\label{driftrate}

The drift rate is one of the most important parameters of solar radio bursts. It corresponds to the time derivative of the emission frequency $df/dt$ (MHz s$^{-1}$) at a given frequency level. According to the definition, we calculated the frequency drift rates as a slope of local lines connecting the burst peak times at the boundaries of each frequency sub-band in the frequency-time diagram (local, piecewise linear fitting procedure).
Then, we performed a linear regression procedure on the sequence of the mean values of the frequency drift in different frequency sub-bands (as outlined above) obtained by the Gaussian fit on the histograms.
\begin{figure*}[h]
\begin{minipage}[h]{0.65\linewidth}
\center{\includegraphics[scale=0.24]{fig3.eps}}
\end{minipage}
\caption{ Examples of the decameter type III and narrow-band type-III-like bursts. The dynamic radio spectrum of the type III burst (panel A) and variation of its flux (panel B) in time. The dynamic radio spectrum of the narrow-band type-III-like bursts (panel C) and variation of their fluxes (panel D) in time.}
 \label{burstsample}
 \end{figure*}

\begin{figure*}[h]
\begin{minipage}[h]{0.65\linewidth}
\center{\includegraphics[scale=0.8]{fig4.eps}}
\end{minipage}
\caption {Example of drift rate histograms for the type III bursts during period 1 at frequencies $18\;$MHz (A), $22\;$MHz (B), $26\;$MHz (C), and $30\;$MHz (D).}
 \label{histdriftrate}
 \end{figure*}
We approximated the dependence of the drift rate on the emission frequency for observed
bursts by a linear fitting
\begin{equation}\label{linear}
 \frac{df}{dt} = -A \cdot f+B,
\end{equation}
 where coefficients $A$ (s$^{-1}$) and $B$ (MHz s$^{-1}$) are to be evaluated through linear fitting to
drift rates evaluated in each frequency sub-band, $f$ (MHz)
(in all following formulas throughout the text we measure the emission frequency $f$ in MHz)
and the corresponding fitting lines are plotted in Fig.~\ref{driftgraph}.
In panel~A of Fig.~\ref{driftgraph}, two lines are plotted corresponding to the sub-intervals within which type IV radio bursts occur. The dotted blue line corresponds to the sub-interval 08:00-09:00 UT, when CME~1 was detected, while the solid red line corresponds to CME~2 in the sub-interval 09:00-10:10 UT.
Our results show that the mean drift rates for the type III bursts we observed fall between $1-2.5\;$MHz s$^{-1}$ and for the narrow-band type-III-like bursts they range between $1.5 - 4.5\;$MHz s$^{-1}$. The drift rates increase with the frequency in each period. In some cases, the drift rates can be as small as $0.4\;$MHz s$^{-1}$, and sometimes single bursts have drift rates of more than $10\;$MHz s$^{-1}$ \citep[which is in agreement with the similar result reported by ][]{melnik08}. In addition, we detected a difference between the values of the drift rates of the narrow-band type-III-like bursts in period 2, when we observed two CMEs with different properties.

\begin{table*}[h]
\caption{Values of the constants A and B of the linear approximation for the drift rate as defined in Eq. \ref{linear}.}
\centering
\begin{tabular}{ l  c  c  c  c c }

 Coefficients               & Period 1   & Period 2 (CME1) & Period 2(CME2) & Period 3 & Period 4 \\
\hline
\hline
 A, s$^{-1}$                & 0.06 &   0.17             &  0.10 &       0.06 & 0.09  \\

 B, MHz$\cdot$s$^{-1}$      &  0.02&  -0.86              & -0.22 &      0.30  & 0.79 \\

\end{tabular}\label{tabledrift}
\end{table*}

In Table~\ref{tabledrift}, the linear approximation coefficients are shown for each considered period.
The values of coefficient $A$ in  periods 2 and 4 are significantly larger than those in  periods 1 and 3. The physical meaning of this fact will be described below.
\citet{wild1950} reported that the drift rates of type III bursts observed within the frequency range
of $70-130\;$MHz can be linearly approximated with characteristic values of the coefficient $A$ varying within
the range $0.16-0.5\;$s$^{-1}$ , which is in good agreement with recent estimations reported by \citet{melnikboiko11}. In a similar study \citep{antonov14} the frequency drift was approximated by the power law function $\sim af^n$. In that work the characteristic values obtained for the constants were $a=7 \cdot 10^{-3}$ and $n=1.73$, which correspond to the value of the coefficient in our linear approximation $A=0.14\;$s$^{-1}$  for the case of no CME, while in the presence of type IV bursts the value of $n=1.23$ and $a=4.5 \cdot 10^{-2}$ gives a corresponding value $A=0.12\;$s$^{-1}$. As one can see from Table~\ref{tabledrift}, in  periods 1 and 3 we infer values that are a factor of about 0.43 smaller, and in periods 2 and 4 the values obtained by us are comparable with \citet{antonov14} estimations.
The mean frequency drifts are monotonically increasing functions of the radio emission frequency, meaning decreasing with distance from the reference point where the frequency is about $30\;$MHz. In general, the direction of the emission source motion can be oblique to the density radial gradient, but as we consider a large number of radio bursts, we assume that the angle between these two directions is distributed somewhat homogenously and therefore we can represent the average radial component of the source velocity by the expression

\begin{equation}\label{v_s}
 v_s =\frac{2}{\pi}\int_0 ^{\frac{\pi}{2}} v_0 \cos \alpha d \alpha,
\end{equation}
where $\alpha$ is the angle between source velocity and radial direction and $v_s$ is the mean source velocity.
In Eq.~(\ref{linear}) the inequality $|B/Af|\ll1$ is valid, which is justified by our measurement given in Table \ref{tabledrift}.
In our analysis the value of electron beam velocity is always fixed to $0.3c$ and there are recent similar measurements for high frequency radio emissions $80-240\;$MHz related to type III radio bursts from the solar limb sources \citep{mccauley2018}. These authors use the radio imaging technique, which allows them to not only infer the density profiles but also to directly measure the emission source velocity.
Thus we have
\begin{equation}\label{density}
 \frac{df}{dt} =f\cdot \frac{1}{2n_e}\cdot \frac{dn_e}{dr}\cdot v_s,
\end{equation}
where $r$ is the radial coordinate.  Using the last expression we evaluated the density profiles provided that the average source velocity $v_s$ is taken to be $0.3c$ for accelerated electron beams \citep{melnikboiko11}.
In such an analysis of the density profiles, either the shape of the profile has to be fixed by imposing existing known profiles and evaluating the corresponding velocities of the emission sources, or on the contrary fixing the mean value of the source velocity and deriving the shape of the density profile from the observed rates of the frequency drift. In the current study we used the second method as we were interested in a comparison of the actually observed density radial distributions before and during the CME, independently from preassumptions laying under of any known standard solar atmospheric profiles.
Based on the comparison of Eqs.~(\ref{linear}) and (\ref{density}), the following relation is valid:
\begin{equation}\label{A}
  A=-\frac{1}{2n_e} \cdot \frac{dn_e}{dr}\cdot v_s.
\end{equation}
Supposing  that  the  velocity of the source is given and $A$ is calculated from observations, Eq. \ref{A} can be used to infer the exponential density profile
\begin{equation}\label{n}
   n=n_0\exp \left (-\frac{2A}{v_s}r \right),
\end{equation}
where $n_0$ is a normalization factor representing the density rate at the reference altitude, where emission frequency is equal to $30\;$MHz.
\begin{figure*}
\begin{center}
\includegraphics[scale=0.68]{fig5.eps}
\end{center}
\caption{Drift rate dependence on frequency according to the observations of type III and narrow-band type-III-like
bursts on June 13, 2014. Panel A corresponds to periods 1 and 2,
 and panel B to periods 3 and 4.
In panel A the dashed line linear regression with corresponding observationally measured values (asterisks with error
bars) are shown in blue and they are related to the interval 08:00-09:00 UT when  CME~1 was detected, and similarly the
solid line and corresponding measured values are shown in red for the interval 09:00-10:10 UT, when CME~2 was detected.
In panel B again the solid line and corresponding measured values are given in green and they show results for the time
interval 12:50 UT-14:55 UT, when CME 3 was detected. In both panels for data  and lines in period 1 and period 3, black
is used.}
\label{driftgraph}
\end{figure*}

\subsection{Duration}\label{duration}
The radio burst duration at a fixed frequency (i.e.,\ corresponding to a fixed density at a given radial distance) is caused by the radial sizes of the local radio emission sources and measured as half peak intensity levels \citep{suzuki85,elgaroy72,rutkevich}. Again we create data sets of the burst durations for each observational period separately, then we plot histograms of the duration occurrence rates and perform a Gaussian function fit to detect the mean duration values. There are several approximation formulas known for the dependence of duration on the emission frequency. In the frequency range 67$\;$kHz - 2.8$\;$MHz it has been approximated by \citet{suzuki85} as
\begin{equation}\label{suzukidulk}
    \tau= \frac{220}{f}=7.33 \left (\frac{f}{30}\right ) ^{-1},
\end{equation}
where the duration is measured in seconds.
On the other hand, \citet{elgaroy72} proposed  a dependence of the duration on the frequency by the  scaling law
\begin{equation}\label{lyngstad}
    \tau=60\cdot f^{-\frac{2}{3}}=6.21 \left (\frac{f}{30}\right ) ^{-\frac{2}{3}},
\end{equation}
\begin{table*}[h]
\caption {Values of the constants $k$ and $E$ of Eq. \ref{powerfunction}.}
\centering
\begin{tabular}{ c  c  c  c  c c }

 Coefficients   & Period 1   & Period 2 (CME1) & Period 2(CME2) & Period 3 & Period 4 \\
\hline
\hline
k              & -0.22    & -0.84         & -0.66         &  -0.79   & -0.64  \\

E, s                & 10.54     & 1.73             & 2.84            & 5.41      & 3.27 \\

\end{tabular}\label{durationtable}
\end{table*}
for the frequency range $300\;$kHz - $500\;$MHz. The durations obtained from our data are almost always smaller compared to Relation~\ref{suzukidulk}.
We approximate our measurements also as a scaling law similar to Expressions~\ref{suzukidulk} or~\ref{lyngstad},

 \begin{equation}\label{powerfunction}
 \tau= E \cdot \left (\frac{f}{30}\right ) ^{k},
 \end{equation}

where $\tau$ denotes the duration in seconds, $E$ is a constant measured in s, $f$ corresponds to the frequency, and $k$ is
the power exponent. We detect the values of the constant parameters from a fitting procedure outlined above and displayed in
Fig.~\ref{durationgraph}, and the obtained values of these parameters, $E$ and $k$, are given in Table~\ref{durationtable}.

\begin{figure*}
\begin{center}
\includegraphics[scale=0.7]{fig6.eps}
\end{center}
\caption{Dependence of duration on frequency. The sequence of the line styles and coloring is the same as in Fig.~\ref{driftgraph}.}
\label{durationgraph}
\end{figure*}

\subsection{Instantaneous frequency bandwidth}\label{bandwidth_sec}
Instantaneous frequency bandwidth is the additional measurable parameter that characterizes the properties of the radio bursts we investigate. It can be detected directly by inferring half power bandwidth, that is,\ the bandwidth is defined as the half width of the Gaussian fit of power in the frequency domain, at a given instance.
 There is another way to carry out IFB estimation by using the following relation with the burst duration and frequency drift:
 \begin{equation}\label{bandwidth}
    \Delta f =\frac{df}{dt} \cdot \tau.
 \end{equation}
In our observational data analysis we used the second method for the measurements: Expression \ref{bandwidth} for the evaluation of IFB.
This way we calculated the instantaneous frequency bandwidth values for each frequency sub-band and performed the same
statistical analysis as we did for drift rate and duration. Again, we first plotted histograms of the instantaneous frequency bandwidth distributions to derive the mean bandwidth values for each frequency sub-band. Next, we approximated the systematic dependence of the bandwidth on the emission frequency by a linear fitting,
  \begin{equation}\label{bandwidthapprox}
    \Delta f = C \cdot f + D,
  \end{equation}
where $C$ and $D$(MHz) are constants evaluated through fitting. The results of these approximations are shown in Fig. \ref{bandwidthgraph}.
\begin{figure*}
\begin{center}
\includegraphics[scale=0.7]{fig7.eps}
\end{center}
\caption{Instantaneous frequency bandwidth dependence on the frequency. The sequence of the line styles and coloring is the same as in Fig.~\ref{driftgraph}.}
\label{bandwidthgraph}
\end{figure*}

\begin{table*}[h]
\caption {Regression coefficients  $C$ and $D$ of Eq. \ref{bandwidthapprox}.}
\centering
\begin{tabular}{ c  c  c  c  c c  }

Coefficients   & Period 1   & Period 2 (CME1) & Period 2(CME2) & Period 3 & Period 4 \\
\hline
\hline
 C             & 0.42     & 0.24          & 0.03        & 0.13   & 0.48  \\

 D, MHz         & 5.92     & 2.07          & 7.33         & 7.72    & -1.08 \\

\end{tabular}\label{bandwidthtable}
\end{table*}

The values of the fitting coefficients $C$ and $D$ are given in Table \ref{bandwidthtable} for each period. The sequence of panels, line, and marker styles and coloring in Fig.~\ref{bandwidthgraph} coincide with those in the figures for the drift rate and duration.
According to our observations, the IFB values for type III bursts lay between $9-21\;$MHz, and for narrow-band type-III-like ones they range from $6$ to $13\;$MHz. We find that the IFB is also an increasing function of the frequency, although for the case of CME2 it remains almost constant.

\section{Discussion}\label{discussion}
Our results show that the values of coefficient $A$ shown in Table \ref{tabledrift} range between $0.06-0.17\;$s$^{-1}$ , which is close to the results reported by \citet{wild1950} for the frequency range $70-130\;$MHz and analogously for the range $8-32\;$MHz reported by \citet{melnikboiko11}, where the values are in the range $0.07-0.12\;$s$^{-1}$. Within period 2 (as in period 4 the situation is different, as we argued above) we calculated two characteristic values of the coefficient $A$ and these values are drastically different from each other. We also observe that the values of coefficient $A$ in periods 1 and 3 are two to three times smaller than those in periods 2 and 4. We suppose that this is related to the physical properties of the two different CMEs that occurred in that period.  There may be different explanations of the observed properties of the local plasma. However, it is plausible to assume that significant sharpening of the density gradient in the instances of CME propagation may be related to certain magnetic islands, which represent local density enhancements due to confinement by the magnetic field that produces sharper density gradients at the edges between the islands and ambient coronal plasma. This hypothesis is in good agreement with the modern observations of magnetic islands and related density depletion regions \citep[for instance, see][]{erikson2014}.

It is not the primary goal of the current paper to build any rigorous density model as within our observational
framework we can estimate only the coefficient standing at $r$ in the exponential function of Expression \ref{n} or
equivalently the slope of the variation of frequency drift with the emission frequency determined by Relation \ref{A}.
Although, it could be appropriate to make a rough comparison of the values of the slope observed by us with ones recovered
from some of the existing coronal density models. For example, we analyzed two cases of such models given by
\citet{newkirk61}:
\begin{equation}\label{nnewkirk}
   n=n_{*}\cdot 10^{4.32\frac{R_{\sun}}{r}},
\end{equation}
where $n_{*}=4.2 \cdot 10^4\;$cm$^{-3}$  , and by \citet{leblanc1998}
\begin{equation}\label{nleblanc}
 n=\frac{n_{1}}{\left( r/R_{\sun}\right)^2} +\frac{n_{2}}{\left( r/R_{\sun}\right)^4} +\frac{n_{3}}{\left( r/R_{\sun}\right)^6},
\end{equation}
where  $n_{1}=3.3 \cdot 10^5 $, $n_{2}=4.1 \cdot 10^6$ , $n_{3}=8 \cdot 10^7\;$cm$^{-3}$.
We made a rough estimation of the corresponding values of exponent $A$ and compared them to the mean
observed ones. For this we recall that the $30\:$MHz and $20\:$MHz radio emission is approximately radiated from
altitudes $1.78R_{\sun}$ and $2.1R_{\sun}$, respectively. Therefore, from Newkirk's and Leblanc's models one
respectively has $A_{Newkirk}=0.22\;$s$^{-1}$, $A_{Leblanc}=0.23\;$s$^{-1}$ ($30\:$MHz) and
$A_{Newkirk}=0.16\;$s$^{-1}$, $A_{Leblanc}=0.19\;$s$^{-1}$ ($20\:$MHz).

The results also show that the type III burst mean durations in the frequency range $12-32\;$MHz are between $5-13\;$s \citep[which is in good agreement with values reported by][]{Mel2005}, and those for the narrow-band type-III-like bursts range between $1.5-5.5\;$s.

It is evident that the duration decreases with frequency in each period. Besides, we detected a difference between the values of durations of narrow-band type-III-like bursts corresponding to the two different type IV bursts observed within period 2, when two CMEs were launched from different heliographic positions.  As a matter of fact, the durations detected in the first sub-interval (08:00-09:00 UT, corresponding to CME~1) of period~2 have smaller mean values ($1.9-3.4\;$s) in each frequency sub-band compared to those in sub-interval 09:00-10:10 UT (corresponding to CME~2) ranging between $2.8-4.5\;$s.

 By inverting the electron density profile in Eq.~\ref{n}, an expression derived from the drift rates, and using the definition of the electron plasma frequency,
we can calculate the position altitude $h$ of the source propagating with respect to the reference point corresponding to $f^{(0)} _{pe}=30\;$MHz as
\begin{equation}\label{bidzina}
    h=\frac{v_s}{A} \cdot ln\left [ \frac{f^{(0)}_{pe}}{f_{pe}}\right ].
\end{equation}
This height is situated at different radial positions corresponding to local density scale heights (radial gradients) ultimately determined by the mean source velocity $v_s$. The parameter $A$ is the derivative of the drift rate with respect to the emission frequency, as defined in Sect. \ref{driftrate} and the values given in Table~\ref{tabledrift}.

As is well known, the burst durations carry information about the spatial size of the emission sources \citep{rutkevich12,rutkevich}. We calculate them using the expression
\begin{equation}\label{bidzi}
    L\approx v_s \cdot \tau=v_s \cdot E \left (\frac{f}{30}\right ) ^{k}
,\end{equation}
where $L$ is the radial length of the source.
\begin{figure*}
\begin{center}
\includegraphics[scale=0.7]{fig8.eps}
\end{center}
\caption{ Dependence of the emission source sizes $L$ on the radial distance from reference point $r-r(30\;$MHz$)  $(both are measured in solar radii). The sequence of the line styles and coloring is the same as in Fig.~\ref{driftgraph}.}
\label{rLbound}
\end{figure*}

Figure~\ref{rLbound} displays the dependence of the radial length of the emission source on the radial distance (both normalized by $R_{\sun}$). The reference height corresponds to a frequency of $30\;$MHz and the emission source speed is fixed to $v_s=0.3c$ (particle beam excitation mechanism for both type III and narrow-band type-III-like bursts are taken into account, because of reasoning given in the introduction and further in the text).

\begin{table*}[h]
\caption {Density scale height $H_{n_{e}}$ and its fraction on average per observational period radio emission source size $\bar{L}$.}
\begin{tabular}{ l  c  c  c  c }

Quantity                        & Period 1       & Period 2(CME1 / CME2)& Period 3       &Period 4    \\
\hline
\hline
$\bar{L}=L/R_{\sun}$                & 1.48        & 0.31/0.47            & 0.94          &  0.54      \\

$H_{n_{e}}/ \bar{L}$, $R_{\sun}$    & 0.74       & 1.2/1.36              & 1.09           & 1.32      \\

$H_{n_{e}}$, $R_{\sun}$             & 1.09       &0.37/0.64               &  1.03         & 0.71        \\

\end{tabular}\label{sourcetable}

\end{table*}

In Fig.~\ref{rLbound} the length of the source increases with distance in each period. Also, the values of $L$ are significantly smaller in periods 2 and 4 (which range between $0.2-0.7\;R_{\sun}$) than in periods 1 and 3 (ranging between $0.65-1.65\;R_{\sun}$). As regards the values of radial widths of the observational window $h_w=r(14\;$MHz$)-r(30\;$MHz$)$, they are larger in the periods before the CME propagation (with sizes $h_w > 1.5\;R_{\sun}$ both for periods~1 and 3) compared to periods 2 and 4 with values $h_w\approx 0.6\;R_{\sun}$ (CME1), $h_w\lesssim 1\;R_{\sun}$ (CME2), and $h_w\gtrsim 1\;R_{\sun}$ (CME3). This means that the emission sources expand and reach their observed sizes at different radial distances depending on density profile differences between quiet (periods 1 and 3) and type IV radio burst (periods 2 and 4) epochs.
In Table \ref{sourcetable} we provide the values of the density scale heights $H_{n_{e}}$ and their ratios on average per period radio emission source size $\bar{L}$. In the periods of absence of CME (periods 1 and 3), the density scale height ratio on the mean emission source size $\bar{L}$ is rather small compared to the cases of CME propagation (periods 2 and 4). This fact may indicate that before the CME the characteristic sizes of the radio emission sources are large and they are comparable or even exceed the density scale height values (see Table \ref{sourcetable}). From the same table it is also evident that, on the contrary, during the CME's the emission, sources are considerably smaller than the characteristic length of the density radial variation. The smaller spatial scales of the emission sources and corresponding scale heights (Table \ref{sourcetable}) within periods 2 and 4 may indicate a link with the magnetic islands \citep{erikson2014} forming in the CME passage regions. On the other hand, narrowing of the radial observation windows demonstrates the sharper density radial gradients. The main final conclusion of this analysis is that both the density scale heights and emissions sources decrease during the CME propagation, however emission source sizes drop down more drastically, so that we observe the increase in the ratio of these quantities.

\section{Conclusions}\label{secconcl}
Our goal was to compare the characteristics of solar radio type III bursts during pre-CME eruption and CME propagation periods, as we wanted to observe whether there are any differences between these periods that are manifested in values of the plasma parameters. To accomplish this, we used data from the telescope URAN-2 recorded on  June 13, 2014. The results of our analysis show that, indeed, the plasma properties are significantly different in observation periods with and without CMEs.

The general tendency in the drift rate values we obtained is that they increase with the emission frequency, ranging between $1-2.5\;$MHz s$^{-1}$ for type III and  between $1.5-4.5\;$MHz s$^{-1}$ for narrow-band type-III-like bursts. The values of the linear fitting coefficient $A$ in periods 1 and 3 are two to three times smaller than those in periods 2 and 4. We concluded that this fact could be caused by the presence of magnetic islands \citep{erikson2014} at the CME passage areas.

The durations for type III bursts are between $5-13$ s and between $1.5-5.5 $ s for narrow-band type-III-like ones. The duration rate decreases with emission frequency in each period. Using the duration, we determined normalized spatial sizes of the emitting sources $L/R_{\sun}$ as a function of the normalized radial distance $h=r-r(30\;$MHz$)$. It is important to note that the positions of the reference points have been calculated using the density profile model for each period separately, corresponding to the respective values of the coefficient $A$. In pre-eruption periods, the characteristic sizes of the emitting sources range as $L=0.7-1.7\;R_{\sun}$. During the CME propagation periods, they range as  $L=0.2-0.7\;R_{\sun}$. In both cases, the emission sources expand with radial distance.

The instantaneous frequency bandwidth increases linearly with the emission frequency. Its values for type III bursts range between $9-20\;$MHz and for narrow-band type-III-like ones they lay between $6-12\;$MHz. The presence of the spread of the radio bursts in the frequency domain is usually ascribed to the range of the emitted radio wavelengths, which in turn is described in terms of the characteristic cross-sectional sizes of the magnetic structures.

The method presented in this work is useful for the radio diagnostics of pre-, during, and post- CME corona. We performed a general analysis of our results in conjunction with optical observational signatures of the CMEs. The results obtained in this paper create a solid background for the further development of observational and theoretical tools for coronal plasma diagnostics in future applications.

\begin{acknowledgements}
This work was supported by Shota Rustaveli National Science Foundation grants DI-2016-52 and FR17\_609. The investigation was initiated and developed within European Commission FP7-PEOPLE-2010-IRSES-269299 project - SOLSPANET. The work of G.D. has been realized within the framework of Shota Rustaveli National Science Foundation PHD student's research (individual) grant DO/138/6-310/14 and grant for young scientists for scientific research internship abroad IG/47/1/16. The work of B.M.S. and M.L.K. was supported by the Austrian Fonds zur Frderung der wissenschaftlichen Forschung (FWF) under projects P25640-N27, S11606-N16, and Leverhulme Trust grant IN-2014-016. The work of T.V.Z. was supported by the Austrian Science Fund (FWF)  under project P30695-N27. M.L.K. additionally acknowledges the support of the Russian Science Foundation (grant  18-12-00080) and FWF project I2939-N27. We would like to express our appreciation to Dr. C. Briand and Dr. J. Magdalenic for valuable discussions and constructive suggestions on the content of the manuscript. We are thankful to the referee, Prof. G.P. Chernov, for constructive comments on our paper that led to significant improvements of the content.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


text:
Almost legal it's Week 20 of O'Dark 30, KUT's exploration of the world of independent radio production. Every Sundays at midnight on KUT 90.5 Austin we present 3 hours of a little bit of everything from the world of independent radio production.
Episode 20 includes My Thoughts on Working for God and Elvis...The Prince of Kosher Gospel...The Hula Lesson...ben franklin death ray...An Addict Named Lady...The Godfather of Ambient Chamber Music...No Brother of Mine...Manufacturing Melodies...KUT's semi-regular Portrait of an Artist--Mo Stoycoff...Holy Land Tour...Waiting on a Furendo
The Prince of Kosher Gospel
From Alex Goldmark | 04:14
First person vignette with music.
Alex Goldmark
Joshua Nelson, a proud African-American-Jew, explains how he fuses the soul music he loved as a boy with the sometimes dreary liturgical songs of his Jewish faith. He sure can spice up a service, just have a listen to the music he makes.
The Prince of Kosher Gospel | 04:14
The Hula Lesson
From Outer Voices | 57:26
In "The Hula Lesson" we join Hawaiian Hula teacher Roselle Bailey and her halau of multicultural women to find out what hula is, what it means to Hawaii, and why so many non-Hawaiians love it.
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Hula is more than girls dancing with coconut bras and grass skirts, with strains of Don Ho in the background. In fact, hula is a complete expression of a traditional culture, which uses dancing and singing for teaching social lessons, and for recounting history. In "The Hula Lesson" we join Hawaiian Hula teacher Roselle Bailey and her halau of multicultural women to find out what hula is, what it means to Hawaii, and why so many non-Hawaiians love it.
The Hula Lesson | 57:26
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An Addict Named Lady
From Next Generation Radio | Part of the NPR's Next Generation Radio series | 04:46
A suburban family?s secret struggle with an uncommon addiction comes to light in this personal essay by Laura Mirsch.
Next Generation Radio
An Addict Named Lady | 04:46
The Godfather of Ambient Chamber Music
From John Diliberto | Part of the Echo Location: Soundings for New Music series | 03:30
Harold Budd started out as a jazz drummer in the 1950s, then became a student of Schoenberg style serialism. Against that backdrop, he revolted the only way he could: making a political statement by creating what he called "pretty music," going against the perceived wisdom of what avant garde music was at the time. With producer John Diliberto, Harold Budd talks about and demonstrates exactly what he means and why he's a legend among ambient musicians.
John Diliberto
It's part of Echo Location: Soundings for New Music, the weekly digest from Echoes host and Peabody Award winning producer John Diliberto, exploring the latest in modern music with quick hitting interviews, music and commentary. Each edition of Echo Location features a beautifully edited music blend, that's combined with John's thoughtful insights and artists's comments to make a sound-rich journey for listeners. Each episode can stand on its own or be scheduled as a weekly or occasional series.
The Godfather of Ambient Chamber Music | 03:30
No Brother of Mine
From Todd Melby | 59:30
"No Brother of Mine" offers an unflinching look at U.S. sex offender policy that reaches beyond the headlines and into the lives of real people. Reported over four years by award-winning independent producers Todd Melby and Diane Richard, this hour-long documentary combines audio-rich storytelling that puts the listener in the scene with expert interviews that lend perspective and propel the narrative forward. It provides a nuanced examination of issues surrounding federal online registration laws, residency restrictions, Romeo and Juliet laws and the growing use of civil commitment.
Todd Melby
In an attempt to protect the public from sexual violence, the U.S. has enacted get-tough laws targeting released sex offenders. Many were inspired by high-profile cases in which children were raped and killed by strangers, a heinous albeit rare crime. Federal law now requires states to register all sex offenders online, including those committed of consensual teen sex and of public urination and indecent exposure. Dozens of states and municipalities have created buffer zones that prevent offenders from living near schools, playgrounds and parks. And about 20 states—including California, New York, Minnesota and Washington—indefinitely confine the worst offenders to mental hospitals.
Proponents contend that these laws make society safer. Opponents say they're often ineffective and violate civil liberties.
Since 2006, award-winning producers Diane Richard and Todd Melby interviewed leading experts and victims' advocates about the impact of these laws. They've also spent time getting to know four Minnesotans convicted of sex crimes, in prison and since their release. In many ways, these men represent the complexity of the issue. Their crimes span a spectrum of sexual violence. All are felons. Each completed a sex offender treatment program.
These men's stories put a candid human face on the highly politicized issue of sex crimes, the damage they cause and some of their common roots. Together, the documentary provides a nuanced examination of issues surrounding online registration laws, residency restrictions, Romeo and Juliet laws and the growing use of civil commitment.
Produced with dual narrators, "No Brother of Mine" combines audio-rich storytelling that puts the listener in the scene with expert interviews to propel the narrative forward. The result is a probing look from many different perspectives at a nation grappling with how to handle the sensational yet banal reality of sexual violence and at the struggles released offenders face in a society that no longer wants them.
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Manufacturing Melodies
From Zak Rosen | 06:22
A sound-rich profile of Frank Pahl, a Wyandotte, Michigan based musician and toy instrument builder.
Zak Rosen
Frank Pahl grew up in a Wyandotte, MI. A town outside of Detroit, where most people work in a factory, making cars or something having to do with them. But Pahl defied his family's expectations of him, and has for the past 20-years tinkered with toys and tools for the sheer enjoyment of the process, rather than a pre-determined end result, and he's been able to etch a living out of his sound experiments. He's specifiaclly interested in the sound of youth and childhood, and has been collecting toy instrments for years and years.
Manufacturing Melodies | 06:22
From Jake Warga | 13:27
Never before aired! PRX exclusive!
A personal tour through the Holy Land, looking at how the conflict started and what it's like today between Jerusalem and Bethlehem...between birth and re-birth.
Also a slideshow:
http://hearingvoices.com/news/2009/12/holy-land-tour/
A narrated audio-rich trip through the holy land exploring the modern state of Christmas. Between Jerusalem and Bethlehem, between Easter and Christmas, there is a modern and yet ancient wall. In my travels I explore the origins of the conflict, all the way back to Abraham:
"...The name "Isaac" means "He Laughs" His laughter and blood becomes David's...A lineage dripping with laughter, but blood is mixed with tears. Ishmael, the name, means "He Weeps" The brother of Isaac, the brother of Laughter, weeps to this day...
...In Jerusalem, religions compete to see which can get you up the earliest. Call to prayers from loud speakers in minarets try to beat the roosters. Then come wake-up bells from churches. Not even an Atheist can over-sleep in the holy land. "
Holy Land Tour | 13:27

redpajama_set_name: RedPajamaCommonCrawl


Our 8th "Stockholm Hardware" meetup! This time we focus on "wireless". Event is 18-21 with talks starting 18:30.
This event is co-organized with IoT Stockholm.
We will have a mix of main speakers and short 5 minute lightning talks. The event will be live-streamed and archived on our youtube channel.
We will have light food & refreshments.
Aktiviteten arrangeras av Stockholm Hardware.


A lean chicken dish with Japanese style teriyaki sauce. You can substitute chicken for fish, pork, or beef.
1TO MAKE TERIYAKI SAUCE: In a small bowl, mix ginger, soy sauce, honey, water, and mirin together. Set aside.
2Rub pepper on butterflied chicken breasts.
3Heat an oil coated nonstick skillet. Cook the chicken breasts over medium heat until for 3 minutes on each side or until golden brown.
4Add teriyaki sauce, lower the heat, and cover the chicken with a lid. Simmer for 5 minutes or until the chicken is fully cooked and the sauce is thickened. Remove from heat.
5Rest chicken in teriyaki sauce for 1 minute and slice into ¼-inch in thickness.


For each element in a, return True if there are only decimal characters in the element.
Decimal characters include digit characters, and all characters that that can be used to form decimal-radix numbers, e.g. U+0660, ARABIC-INDIC DIGIT ZERO.


So far this year, we have considered the work of Amity in terms of their missionary & outreach work and also their humanitarian work in response to natural disasters. In this issue, the focus is upon their continuing work to improve living standards of people in rural communities across China.
Simply put, water is life. It is estimated that over a billion people in the world lack safe drinking water. In China alone, some 200 million people still struggle daily to get safe drinking water. As an independent non-governmental organisation (NGO) working in China for 27 years, the Amity Foundation has witnessed the consequent human tragedies, including poverty and water-borne diseases that disproportionally affect the young and lead to high rates of child mortality. The Amity Foundation is privileged to have provided assistance to millions over the last quarter of a century. In the last six years alone they have built over 650 water systems or well projects across China.
As part of Amity's response to the United Nations Conference on Environment and Development, they have also organised projects, such as the so-called 'Walks for Living Water' in Hong Kong, to raise awareness—and raise funds—of this issue still affecting so many people in mainland China. The walks have seen up to 2,500 people and a variety of schools, churches and other groups taking part and have in themselves raised money to provide clean drinking water in eight remote villages in Guizhou Province, thereby benefitting over 10,000 people directly.
Another focus of Amity's work is education & fostering and their main project for 2013 is to help left-behind children in rural villages, often adversely affected when their parents leave to find work in other provinces. Thousands of children have been sponsored over the past few years. This sponsorship has allowed orphans and left-behind children to still have hope in the future with many progressing from primary school to high school and even on to university.
Jia's father died from cancer in January, 2002. Shocked by her husband's death, her mother suffered from mental illness before she also died, in a car accident, in October, 2003. They left behind four children. Due to financial difficulties, Jia's three elder sisters dropped out of education and Jia was sent to live with one of her uncles. After her uncle and his family left to work in another province, Jia was left to live alone.
With Amity sponsorship, she was able to enter the best local high school in July, 2009, ranking sixth among all the contestants from her county. She tells Amity that in the future she wishes to be admitted to Beijing Foreign Studies University so she can realise her elder sisters' education dream.
These are just two of many concerns Amity currently is helping to alleviate across China.
Over the August Bank Holiday weekend the Ellams family were lucky enough to join Rev'd. Denise at Greenbelt. A festival where faith, arts and justice meet which is held at Cheltenham Racecourse. Most of us hadn't been to Greenbelt before and wondered what it was going to be like.
All of us enjoyed the weekend. There was so much to do, see, hear and taste. From music, talks, poets, magicians, comedians, show, films, discussions authors, silent disco's, food vans, services of all descriptions, and stalls.
This is what Georgina and Jonny had to say.
"I think Greenbelt was Amazing! It's a brilliant place to take young children and older children as well. I was really impressed with the amount of different things to listen to and do. When my Mum said it was a Christian Festival I was a bit like everyone is, 'is it just going to be praying?' but it weren't I went to listen to a poet called Harry Baker and his poems were great and on all sorts of topic's. I also enjoyed the comedians Adrian Plass and Milton Jones. There was a main stage where bands and singers preformed. I thought the best act was the London Gospel Choir because they were very lively and excitable. I loved Greenbelt and I really want to go again."
Great atmosphere, good acts- great for music and comedy, good friendly place, people, atmosphere, safe acts for children, good facilities. Good venue and clean.
Not much – in fact nothing this year.
Harry Baker, Milton Jones, Adrian Plass, London Gospel Choir and Lemor were amazing. I enjoyed the camping, although you don't have to camp. Greenbelt is a great festival for members of any religion or none at all. Fantastic for all ages. Greenbelt is a must do festival."
If you are thinking of going next year, it would be good if a group from Frodsham Methodist Church could go together. If we book before the end of January the tickets are cheaper. Adult weekend ticket is £99. Under 18 weekend ticket is £54. Family weekend ticket. (2 adults and 2 children ) £254. Single parent weekend pass with 2 children £156. Speak to Andrea Ellams for details.


4 cm canvas material with tropical motif. And genuine leather ends (SG logo emboss in leather) for absolute maximum strength and longevity. Adjustable to 90 Cm. Its also for mirorrless camera we provide two ring with leather for protect your camera.


If something isn't right with your new goodies, then we are happy to accept a exchange for a different size or colour, or give you store credit.
Get Yourself Dressed is an independent, Melbourne festival wear brand that focuses on making you look and feel the best you possibly can! We aim to make clothing that can be worn by boys and girls which keeps you looking fab in your festival fashion.
You won't find our fabric prints anywhere else as they are all original and the neon designs are made especially by our in-house textile designer. So if you are ready to get playful, colourful and have some fun on the dance floor – come and check our our festival clothing.


Srisailam Sri Mallikarjuna Swamy Temple is one of the ancient Shiva temples located in Kurnool District of Andhra Pradesh, India. Srisaila Devasthanam is one of the 12 Jyotirlingas of Shiva and one of the 275 Paadal Petra Sthalams. The temple lies in a picturesque environment of Nallamalai Hills on the banks of the Krishna River. Sri Mallikarjuna Jyotirlinga Temple is around 212 km south of Hyderabad and 179 km from Kurnool.
Srisailam Shiva Temple enshrines Shiva as Mallikarjuna Swamy and Parvati Devi as Goddess Bhramaramba Devi (one of the eighteen Mahasakthis). Shiv-Parvati are believed to be self-manifested here. The huge temple complex consists of separate several sub shrines, pillared halls, mandapas and springs.
9 Nava Brahma Temples – Each of them enshrined with Sivalingas named after the eight forms of Siva such as Bhava, Sarva, Esana, Pasupathi, Rudra, Ugra, Bheeema and Mahadeva. The ninth temple is having the Moksha linga.
The entire complex is fortified by the most impressive Prakaram wall of massive stones. Nallamalai Hills is also known by the names Siridhan, Srigiri, Sirigiri, Sriparvatha and Srinagam.
Maha Sivarathri is the most important festival celebrated here as Brahmothsavams in the month of Magham (February – March). The festival is celebrated for eleven days with Navahaknika Deeksha. Important events in Mahasivarathri include Ankurarpana, Dhwajarohana, Vahana Sevas to God and Goddess, Lingodhbhavakala Maharudrabhishekam to God, Pagalankarana, Kalyanothsavam, Radhothsavam and Dhwajavarohana.
Ugadi celebrations performed for a period of five days generally March/April.
Dasara Celebrations in September or October.
Kumbhothsavam is the most significant festival of the temple of Srisailam in which various offerings are made to Goddess Bhramaramba Devi. This festival celebrates on the first Tuesday or Friday after full moon day of Chaitram.
Sankranthi utsavams begins with the Dhwajarohana and ends with the Dhwajavarohana.
Arudrothsavam, Kartheeka masothsavams, Sravananamosothsvams are some of the other festivals.
Air: The nearest Airport is Hyderabad (230 KM) from where buses are plying to Srisailam everyday frequently.
Rail: Markapur, which is 91 KM from Srisailam in Guntur-Hubli, line on South Central Railway from where buses are available to Srisailam.
Road: Srisailam is well connected by APSRTC.Buses not only from all corners of the State but also from Bangalore, Chennai etc. The Karnataka Road Transport Corporation is also running buses from various main cities of that state.


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DIY Edit
DIY Edit: 04 Self-Referential Language
Even though I'm an editor for hire, I firmly believe in self-editing. Each month I'm going to drop a tip for developing your ability to edit your own work or identify things to look for as you edit. Make sure to check out all the DIY Edit Tips to improve your self-editing.
04 Narration: Self-Referential Language
One of my writing professors always marked our stories for what she called "self-referential language." This syntax plagues first person and close third person point of view by calling attention to the fact that the reader is an observer of a character.
Phrases like "I watched…" or "She looked…" or "He heard…" shift the focus from the POV character's observations (the purpose of first and close third narration) to the observation of the character.
Consider the difference in these sentences:
From the window I watched the valets pack the carriage.
Outside the window, the valets packed the carriage.
In the first sentence, the reader is focused on the character watching the valets through the window. If this image were in a movie, the screen would include the window frame and the character in front of the window, looking out on the valets.
In the second sentence, it's still clear that the POV character is inside the house, but this version of the sentence focuses the reader on watching the valets through the eyes of the POV character. As a movie, what the character is watching fills the screen, and the reader is fully immersed in the point of view of the first person narrator.
Editing out self-referential language can make the point of view more immersive and bring the reader closer to the characters and action. It can also help eliminate weak and overused verbs. Here are some combinations to look out for when trying to strengthen your point of view narration:
I/he/she watched
I/he/she saw
I/he/she looked
I/he/she heard
I/he/she listened
I/he/she touched
I/he/she smelled
I/he/she tasted
Watch out for other verbs and sentence constructions that put the emphasis on the character observing rather than on what the character is observing.
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November 7, 2017 /0 Comments/by Alli
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The Write Life: Fresh Start December
The Write Life: NaNoing November
The Write Life: Prepping October
The Write Life: Escaping September
The Write Life: Helpful August
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Testing the equality of two proportions for combined unilateral and bilateral data
Yanbo Pei, Man Lai Tang, Jianhua Guo
In many medical comparative studies (e.g., comparison of two treatments in an otolaryngological study), subjects may produce either bilateral (e.g., responses from a pair of ears) or unilateral (response from only one ear) data. For bilateral cases, it is meaningful to assume that the information between the two ears from the same subject are generally highly correlated. In this article, we would like to test the equality of the successful cure rates between two treatments with the presence of combined unilateral and bilateral data. Based on the dependence and independence models, we study ten test statistics which utilize both the unilateral and bilateral data. The performance of these statistics will be evaluated with respect to their empirical Type I error rates and powers under different configurations. We find that both Rosner's and Wald-type statistics based on the dependence model and constrained maximum likelihood estimates (under the null hypothesis) perform satisfactorily for small to large samples and are hence recommended. We illustrate our methodologies with a real data set from an otolaryngology study.
Communications in Statistics: Simulation and Computation
Maximum likelihood
Type I Error Rate
Maximum Likelihood Estimate
Test Statistic
Pei, Y., Tang, M. L., & Guo, J. (2008). Testing the equality of two proportions for combined unilateral and bilateral data. Communications in Statistics: Simulation and Computation, 37(8), 1515-1529. https://doi.org/10.1080/03610910802140232
Pei, Yanbo ; Tang, Man Lai ; Guo, Jianhua. / Testing the equality of two proportions for combined unilateral and bilateral data. In: Communications in Statistics: Simulation and Computation. 2008 ; Vol. 37, No. 8. pp. 1515-1529.
@article{6137b28a4cfb4284a30fa4b6661bbdbf,
title = "Testing the equality of two proportions for combined unilateral and bilateral data",
abstract = "In many medical comparative studies (e.g., comparison of two treatments in an otolaryngological study), subjects may produce either bilateral (e.g., responses from a pair of ears) or unilateral (response from only one ear) data. For bilateral cases, it is meaningful to assume that the information between the two ears from the same subject are generally highly correlated. In this article, we would like to test the equality of the successful cure rates between two treatments with the presence of combined unilateral and bilateral data. Based on the dependence and independence models, we study ten test statistics which utilize both the unilateral and bilateral data. The performance of these statistics will be evaluated with respect to their empirical Type I error rates and powers under different configurations. We find that both Rosner's and Wald-type statistics based on the dependence model and constrained maximum likelihood estimates (under the null hypothesis) perform satisfactorily for small to large samples and are hence recommended. We illustrate our methodologies with a real data set from an otolaryngology study.",
author = "Yanbo Pei and Tang, {Man Lai} and Jianhua Guo",
journal = "Communications in Statistics Part B: Simulation and Computation",
Pei, Y, Tang, ML & Guo, J 2008, 'Testing the equality of two proportions for combined unilateral and bilateral data', Communications in Statistics: Simulation and Computation, vol. 37, no. 8, pp. 1515-1529. https://doi.org/10.1080/03610910802140232
Testing the equality of two proportions for combined unilateral and bilateral data. / Pei, Yanbo; Tang, Man Lai; Guo, Jianhua.
In: Communications in Statistics: Simulation and Computation, Vol. 37, No. 8, 01.09.2008, p. 1515-1529.
T1 - Testing the equality of two proportions for combined unilateral and bilateral data
AU - Pei, Yanbo
AU - Tang, Man Lai
AU - Guo, Jianhua
N2 - In many medical comparative studies (e.g., comparison of two treatments in an otolaryngological study), subjects may produce either bilateral (e.g., responses from a pair of ears) or unilateral (response from only one ear) data. For bilateral cases, it is meaningful to assume that the information between the two ears from the same subject are generally highly correlated. In this article, we would like to test the equality of the successful cure rates between two treatments with the presence of combined unilateral and bilateral data. Based on the dependence and independence models, we study ten test statistics which utilize both the unilateral and bilateral data. The performance of these statistics will be evaluated with respect to their empirical Type I error rates and powers under different configurations. We find that both Rosner's and Wald-type statistics based on the dependence model and constrained maximum likelihood estimates (under the null hypothesis) perform satisfactorily for small to large samples and are hence recommended. We illustrate our methodologies with a real data set from an otolaryngology study.
AB - In many medical comparative studies (e.g., comparison of two treatments in an otolaryngological study), subjects may produce either bilateral (e.g., responses from a pair of ears) or unilateral (response from only one ear) data. For bilateral cases, it is meaningful to assume that the information between the two ears from the same subject are generally highly correlated. In this article, we would like to test the equality of the successful cure rates between two treatments with the presence of combined unilateral and bilateral data. Based on the dependence and independence models, we study ten test statistics which utilize both the unilateral and bilateral data. The performance of these statistics will be evaluated with respect to their empirical Type I error rates and powers under different configurations. We find that both Rosner's and Wald-type statistics based on the dependence model and constrained maximum likelihood estimates (under the null hypothesis) perform satisfactorily for small to large samples and are hence recommended. We illustrate our methodologies with a real data set from an otolaryngology study.
JO - Communications in Statistics Part B: Simulation and Computation
JF - Communications in Statistics Part B: Simulation and Computation
Pei Y, Tang ML, Guo J. Testing the equality of two proportions for combined unilateral and bilateral data. Communications in Statistics: Simulation and Computation. 2008 Sep 1;37(8):1515-1529. https://doi.org/10.1080/03610910802140232


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Home Tags GreenWood Forest Park
Tag: GreenWood Forest Park
GreenWood Welcomes Two Millionth Visitor
Linda Roberts - 6 August 2016 0
GreenWood Forest Park reached a major milestone when they welcomed their two millionth visitor. On Friday, August 5. at about 12:30pm the Roberts family, from Bangor...
BBC Radio Wales comes to GreenWood Forest Park, Y Felinheli
BBC Radio Wales will broadcast live from North Wales' leading family adventure Park, GreenWood Forest Park on Wednesday, August 10. The popular Wynne Evans show...
GreenWood Forest Park named winner in the 2016 TripAdvisor Travellers' Choice...
Linda Roberts - 1 July 2016 0
GreenWood Forest Park today announced that it has been recognised as a winner in the 2016 TripAdvisor Travellers' Choice™ awards for Amusement Parks in...


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Clown-Acrobat delivers a quirky and heartfelt solo performance
by Elizabeth Garrison | 5/10/19 2:00am
At some point, every person has felt pressure to live up to some kind of expectation to fulfill a role and project an external image of ourselves to others.
Acrobats are no exception to this human experience. In his solo show, "Patinoire," clown-acrobat Patrick Léonard breaks the illusion that circus performers are larger than life by revealing the human element behind creating an act. Léonard gives the audience an intimate glimpse into the physical and emotional challenges a performer faces when they put themselves in a vulnerable position in front of an audience. By giving us a look into his mind, he provides the audience with valuable insight into our own lives.
Last Wednesday and Thursday, Léonard performed "Patinoire" in Spaulding Auditorium at the Hopkins Center. Before Thursday's show, Léonard anxiously paced in the lobby as audience members entered the theater. Despite the fact that Léonard has toured "Patinoire" across North America and Europe over the past five years, the naïve observer would have assumed that this was his first time on stage. With his disheveled hair and jittery mannerisms, Léonard looked terrified as he frantically checked over a list. This image was not exactly what came to mind when I had originally pictured what the co-founder of Montreal's renowned Les 7 Doigts de la Main (The Seven Fingers) circus would look like before a show.
At the beginning of "Patinoire," Léonard challenged my expectations by asking the audience members to leave their assigned seats and move closer towards the stage. Throughout the performance, Léonard encouraged the audience to break out of the traditional role of passive spectators. He spoke directly to audience members and at times would climb off the stage to join the audience. At one point, Léonard pulled someone on stage, handed him a pair of Chinese juggling sticks and left him there alone, looking confused. After a few moments of awkward silence, the people still sitting in the audience began to call out words of encouragement as the man slowly started to let loose and dance around the stage. The audience broke out into applause.
When Léonard returned to the stage, he proclaimed, "Even when you don't know what you are doing, it doesn't matter if everyone loves and supports each other."
I thought this message was a poignant and powerful reminder that there is no shame in asking for help. Later, Léonard went on to perform many unusual feats throughout the rest of the show, such as precariously stacking audio equipment into a tall tower and climbing on top of it, but what I found to be the most compelling part of the performance was the final act.
During most of the show, the back curtain had been closed and Léonard would unexpectedly disappear behind it, leaving the audience staring blankly at an empty stage. Each time this happened, he was gone longer and longer, creating more suspense. After each pause, Léonard would return from behind the curtain as if nothing had happened, but the sense of unease never went away. Throughout the show, Léonard kept promising a spectacular final act, and when the curtain finally opened during his finale, it revealed a towering slide that reached the ceiling where he sat at the top. When he slid down the slide, the audience members gasped, shocked at the startling speed he was moving with. As he took his bows, "Y.M.C.A." played and the audience members danced and sang along, sharing a heartfelt moment. Instead of going backstage, Léonard walked out of the theater with the audience, stopping to give people hugs along the way.
I left the theater feeling inspired. Léonard's performance reminded me of the value in vulnerability and the resulting human connection.
Tags: arts
'Citrus,' a compelling choreopoem, celebrates black women
Gob Squad's "War and Peace" is bizarre, political, relevant
'Cotton Patch Gospel' explores themes of community in theater


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Peru, Nebraska: Sandstone Cliff Carvings
Before Roland Sherman died in 2007, he spent about 20 years making odd sculptures on a sandstone cliff near his home. He didn't talk about it, and now he isn't around to explain it.
5th St., Peru, NE
Enter Peru from Hwy 67. Drive north through town on 5th St. The trailhead and parking area are at the far north end of 5th St. From the trailhead, walk south towards the Missouri River, about 15 minutes, and look for sculptures on the bluffs.
24/7 (Call to verify)
Visitor Tips and News About Sandstone Cliff Carvings
Sandstone Cliff Sculptures
Corn fields are the norm in Nebraska, so when we locals find a sandstone cliff we like to carve our initials and make sculptures on them as evidenced by the Roland Sherman Memorial Area, a part of the Steamboat Trace Trail for hikers and bikers in Peru, Nebraska.
The sandstone sculptures were created over 20 years ago by resident Roland Sherman and in 2007 finished in 2nd place in a vote for the Seven Wonders of Southeastern Nebraska. (Losing only to a dog shelter near Auburn!).
The sculptures are all within a 15 minute walk of the trail head in Peru. The trailhead has free parking and modern restrooms.
The sculptures are on a cliff facing east, so visiting before noon makes for the best viewing, but the trail and sculptures are accessible 24/7 and there is no charge. The area opposite the cliffs and the trail is lowland and susceptible to flooding. Mosquitoes and frogs were very abundant when my family last visited in spring of 2008.
[Bob DiPaolo, 01/19/2010]
Stoner Drug Store and Soda Fountain, Hamburg, IA - 9 mi.
A&W Root Beer Papa Burger, Auburn, NE - 8 mi.
Climb Aboard Lewis & Clark's Boat, Nebraska City, NE - 13 mi.
Spiky Viaduct, Council Bluffs, IA - 54 mi.
Create and Save Your Own Crazy Road Trip!
Nebraska Latest Tips and Stories
OMAR The Bridge Troll, Omaha, Nebraska
Rest Area - Hay Bales, Easy Chair, Toilet, Alliance, Nebraska
World's Largest Ball of Stamps, Boys Town, Nebraska
Troll Under Pedestrian Bridge, Omaha, Nebraska
Odyssey: Iowa's Spiky Towers, Council Bluffs, Iowa
Nearby Hotels: Peru, Nebraska
Super 8 By Wyndham Rock Port MO, 10 mi. (From $61)
Best Western Nebraska City Inn, 13 mi. (From $98)
Holiday Inn Express & Suites NEBRASKA CITY, 13 mi. (From $129)
Super 8 By Wyndham, Nebraska City, 14 mi. (From $66)


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Late Night Style Late Night Vibes
» NYC-Based Singer-Songwriter Aicha Dosso Reveals Dazzling Debut Music Video "Bien"
NYC-Based Singer-Songwriter Aicha Dosso Reveals Dazzling Debut Music Video "Bien"
Despite her young age, NYC-based cosmopolitan artist Aicha Dosso has already lived many lives at once. A model, actress, writer and singer-songwriter, she is now releasing her debut music video for the single "Bien." This french song is a sublime single that revives the French art of parisian cabaret. Aicha adds her personal touch as well as some NYC vibes to the mix, giving the overall effort a mainstream feel.
She sings beautifully and exposes her indie-pop sound for the first time to the public on "Bien," for what seems to be the first release of many more to come. Born in Ivory Coast, she has studied at La Sorbonne, the prestigious University in Paris before moving to New York City where she currently resides.
In parallel to a successful acting career that saw Dosso as a lead in the award-winning feature BYE BYE AFRICA (as Aicha Yelena; Venice Film Festival, CinemA venice Award in the category Best First Film, Luigi De Laurentiis Award – Special Mention) and in a 2010 film CEREMONY (dir. Max Winkler, starring Uma Thurman), she is now taking the path towards a musical success, so make sure to watch "Bien" below:
Kev Brown x J Scienide – "Cutlass Supreme"
Lil Durk is bigger and better on 'The Voice'
Late Night News Late Night Style
Some Make Music While Others Create A New Genre: KatchUp – "Vini"
When most artists make music, some prodigious talents come-up with a new genre. That's what NY-based Haitian-American artist
The New Hip-Hop Project By Rising Artist Losk33 "Lord Have Mercy" Featuring Foogiano Is Already Out
Talking about his new collaboration with Foogiano titled "Lord Have Mercy," Losk33 shared, "It was a gift
Review: Dejhare – "Do What You Gotta Do"
Singer-songwriter Dejhare released her new dance-EDM track "Do What You Gotta Do," spiced up with pop influences


COLUMBIA – The Indian Land High School basketball teams had a tough night at Keenan High School in Columbia on Friday, Jan. 11.
The Lady Raiders opened the KHS hardwood sweep with a 76-22 win, and the Keenan boys followed with a 89-59 victory.
The Lady Raiders, in their 54-point win, were led by Milaysia Fullwiley with 33 points. Dyani Burke hit 22 for Keenan.
The Indian Land girls, who fell to 1-15, 1-1, were led by Gabbi Wilson's seven points, two rebounds, one steal and one assist.
Kristen Falk scored six points and had three rebounds. Allie Floyd had five points, making three of four free throws.
Daniella Wilson netted two points and six rebounds. Crystal Strother added two points.
In the boys game, Keenan, 18-1, 2-0 in region, rolled to a 22-11 first-period lead.
Keenan held a 51-21 lead at the half. The Raiders led 71-38 after three periods on the way to the win.
KHS was led by Raekwon Horton, who had 26 points and 10 rebounds.
JaSean Morris scored 19 points, hitting 7 of 10 free throws, and had five rebounds. Asanti Price netted 11 points for Keenan who had 11 of 12 players score in the region win.
Destin Clark netted 30 points to lead the Warriors in the loss to Keenan. Clark netted 13-18 on two-point shots.
Jersey Graves scored six and had five rebounds. John Fose netted five points.
Adrian Pledger scored four. Tre Thompson tallied three points and had six boards.
Gabe Shook and Chase Dougherty each had two points.
"Keenan beat us in all phases of the game in the first half," IL coach Nate Smith said. "Keenan beat us on the boards and they ran the floor well. They used their size to pound the ball inside.
ILHS hosted Camden on Tuesday, Jan. 15, and visits Fairfield Central High of Winnsboro on Friday, Jan. 18.