text:
\section*{Plain Language Summary}

The UVS instrument on the Juno mission to Jupiter measures ultraviolet sunlight that is reflected from the planet's upper atmosphere and these observations can be used to measure the abundances of different gases in the stratosphere. In this paper, we study the spatial distribution of the molecule acetylene at Jupiter's south pole. We find that there is a significant increase in the acetylene abundance at the location of Jupiter's southern aurora. This suggests that the charged particles that travel along magnetic field lines towards Jupiter's poles and produce bright auroral emission also have a strong influence on the chemistry of Jupiter's upper atmosphere.

\section{Introduction}

Jupiter's strong magnetic field gives rise to the brightest and most energetic auroras in the Solar System. These auroras comprise main auroral emissions, which form a distorted and often discontinuous oval around the magnetic pole; complex polar emissions within the auroral ovals; and diffuse equatorward emissions, including the auroral satellite footprints \cite{grodent15}.

Auroral processes lead to localized heating of the atmosphere within the auroral regions \cite{caldwell80,drossart93b,sinclair17b} and may also be responsible for the high upper atmosphere temperatures across the entire planet \cite{waite83,odonoghue21}. Several previous studies have also suggested that the precipitation of high-energy charged particles may lead to the modification of Jupiter's stratospheric chemistry in the auroral regions. Using infrared observations from Voyager IRIS, \citeA{kim85} observed enhanced emission from a range of hydrocarbons, including C\textsubscript{2}H\textsubscript{2}, C\textsubscript{2}H\textsubscript{4} and C\textsubscript{2}H\textsubscript{6}, within Jupiter's northern auroral oval. They concluded that the enhanced emission was due to increased abundances of these species, although in the infrared spectral region they focus on, there is significant degeneracy between chemical abundances and stratospheric temperatures. \citeA{drossart86} obtained ground-based mid-infrared observations of Jupiter and similarly observed a C\textsubscript{2}H\textsubscript{2} emission hot-spot that coincided with the northern aurora, which they noted could be caused either by an enhancement in the C\textsubscript{2}H\textsubscript{2} abundance or an alteration in the thermal profile.

More recently, \citeA{sinclair17b,sinclair18,sinclair19} have sought to break the degeneracy between chemistry and temperature in order to map the distribution of hydrocarbons in Jupiter's polar regions. \citeA{sinclair17b} used a radiative transfer model to simultaneously constrain the temperature profile and chemical abundances using Voyager IRIS and Cassini CIRS infrared observations. \citeA{sinclair18} performed a similar analysis using high spectral resolution mid-infrared observations obtained from a ground-based telescope, making use of a two-step retrieval process that first used  CH\textsubscript{4} and H\textsubscript{2} S(1) emission to constrain the temperature and then retrieved the hydrocarbon abundances. These studies found that C\textsubscript{2}H\textsubscript{2} and C\textsubscript{2}H\textsubscript{4} are enhanced within Jupiter's northern auroral oval and \citeA{sinclair17b} suggested that the precipitation of charged particles leads to an increase in ion-neutral and electron recombination reactions which, by analogy with Titan's hydrocarbon chemistry, would favor the production of unsaturated hydrocarbons, including C\textsubscript{2}H\textsubscript{2} \cite{delahaye08}. \citeA{sinclair19} extended this analysis to study additional hydrocarbons and found that C\textsubscript{2}H\textsubscript{4}, CH\textsubscript{3}C\textsubscript{2}H and C\textsubscript{6}H\textsubscript{6} are also enhanced within the auroral region.

In this paper, we build on these previous studies by using ultraviolet reflected sunlight observations from the UVS instrument on the Juno mission to study the distribution of C\textsubscript{2}H\textsubscript{2} in Jupiter's polar regions. C\textsubscript{2}H\textsubscript{2} is the hydrocarbon with the strongest spectral signature in the reflected sunlight portion of the UVS spectrum and ultraviolet observations have the advantage of being insensitive to the thermal structure, and therefore complement the earlier infrared studies. The polar orbit of the Juno spacecraft provides a unique viewpoint of Jupiter's auroral regions, particularly the southern aurora which cannot be easily seen from Earth or from equatorial-orbit spacecraft. In Section~\ref{sec:results} we present reflectance maps of Jupiter's poles and show how the shape of the reflectance spectra varies across the polar region. By comparing reflectance maps made at different wavelength intervals, we can infer the C\textsubscript{2}H\textsubscript{2} distribution and we discuss how these results are impacted by uncertainty in the haze opacity and C\textsubscript{6}H\textsubscript{6} abundance. In Section~\ref{sec:discussion} we compare the proxy C\textsubscript{2}H\textsubscript{2} abundance maps with previous results obtained using infrared observations and discuss the possible mechanisms that drive the C\textsubscript{2}H\textsubscript{2} distribution.

\section{Juno UVS observations}
\label{sec:observations}

The Ultraviolet Spectrograph \cite<UVS,>{gladstone17} is a far-ultraviolet imaging spectrograph on NASA's Juno mission, which has been in a highly elliptical polar orbit around Jupiter since July 2016 \cite{Bolton17}. UVS covers the 68-210 nm spectral range with a spectral resolution that varies between 1.3 nm and 3.0 nm depending on the position along the instrument's slit \cite{greathouse13}. The primary scientific goal of the UVS instrument is to characterize Jupiter's far-ultraviolet auroral emissions and this spectral range was selected to include the H Lyman series and the Lyman, Werner, and Rydberg band systems of H\textsubscript{2}. However, the longer wavelengths covered by UVS extend into a spectral region that is dominated by reflected sunlight and this part of the spectrum is sensitive to hydrocarbons and aerosols \cite{gladstone17}. In this paper, we focus on the 175-205 nm reflected sunlight segment of the UVS spectrum.

Juno is a spin-stabilized spacecraft with a rotation period of $\sim$30 seconds. The UVS instrument slit is nominally parallel to the spacecraft's spin axis, allowing the slit to sweep across a swath of planet as the spacecraft rotates. In this paper, we exclusively use data from the wide part of the dog-bone shaped slit, as it has a better signal-to-noise ratio, particularly at the longer wavelengths where the instrument detector is less sensitive \cite{hue19b, hue21b}. UVS data is recorded in a pixel-list time-tagged format; by considering the position along the slit and the spin phase of the spacecraft at the time of observation, each photon can be assigned to a latitude and longitude on the planet. This geometric information can then be used to produce spatial maps of the ultraviolet radiation \cite{gladstone17}. In-flight radiometric calibration is achieved by observation of UV-bright O, B, A stars \cite{hue19b}, and radiances can be converted to reflectances by dividing by the solar spectrum \cite{woods09}, corrected for the solar incidence angle.

UVS obtains observations of Jupiter for several hours on either side of each perijove (the point of closest approach for the spacecraft), covering both the approach over Jupiter's north pole and the subsequent departure over the south pole. When the spacecraft passes through Jupiter's radiation belts, the UVS instrument records high background noise from high energy electrons and ions, and so data acquisition is temporarily paused to both protect the instrument from enhanced degradation \cite{kammer19} and to limit the volume of low-quality noisy data. Due to the precession of the Juno orbit over the course of the mission, the location of the perijove has gradually moved northwards over time, which has moved the approach observations further into the radiation belts. This means that the amount of UVS data obtained from the northern polar region has decreased over time \cite{gladstone19}  and when we co-add reflected sunlight data from many perijoves, as described in Section~\ref{sec:maps}, the signal-to-noise ratio and spatial coverage is significantly better for the south pole.

\section{Analysis and Results}
\label{sec:results}

\subsection{Molecular absorption}
\label{sec:molecules}

Figure~\ref{fig:gases} shows the absorption spectrum for C\textsubscript{2}H\textsubscript{2}, as well as five other molecular species in Jupiter's stratosphere that produce non-negligible absorption in the 140--205 nm spectral range. The transmission is defined as the transmission between an altitude of 100 km (5 mbar) and the top of the atmosphere. The column density for each gas was calculated using the atmospheric composition model described by Model C in \citeA{moses05}, with the exception of C\textsubscript{6}H\textsubscript{6}. As noted in~\citeA{sinclair19}, the peak of the C\textsubscript{6}H\textsubscript{6} distribution is likely to be higher in the atmosphere than predicted in \citeA{moses05} due to additional ion sources. We therefore follow a similar approach to~\citeA{sinclair19} and use an a priori vertical profile for C\textsubscript{6}H\textsubscript{6} that is 0.1\% of the a priori vertical profile for C\textsubscript{2}H\textsubscript{2}; this C\textsubscript{6}H\textsubscript{6} a priori vertical profile matches the \citeA{moses05} Model C C\textsubscript{6}H\textsubscript{6} profile at 3--5 mbar but has significantly higher densities at higher altitudes. Absorption cross-sections were obtained from \citeA{keller-rudek13} and were smoothed to match the 2.2 nm spectral resolution of the UVS wide slit.

\begin{figure}
\centering
\includegraphics[width=9cm]{compare_gases.png}
\caption{Absorption spectra for six molecules with significant absorption in the 140--205 nm spectral range. The transmission is defined as the transmission between an altitude of 100 km (5 mbar) and the top of the atmosphere. The absorption cross-sections have been smoothed to match the spectral resolution of the UVS wide slit. Two abundances are shown for C\textsubscript{6}H\textsubscript{6}: the a priori value (solid line) and 8$\times$ the a priori value (dashed line).}
\label{fig:gases}
\end{figure}

Figure~\ref{fig:gases} shows that while there are multiple highly absorbing species at \textless160 nm, C\textsubscript{2}H\textsubscript{2} and C\textsubscript{6}H\textsubscript{6} are the only species with non-negligible absorption at \textgreater175 nm. C\textsubscript{2}H\textsubscript{2} has a broad absorption feature that has a local maximum at $\sim$172 nm, while C\textsubscript{6}H\textsubscript{6} has a narrower feature that peaks at $\sim$179 nm. The solid purple line shows the absorption produced by the a priori C\textsubscript{6}H\textsubscript{6} distribution, which is considerably weaker than the C\textsubscript{2}H\textsubscript{2} absorption. However, the C\textsubscript{6}H\textsubscript{6} abundance is highly uncertain, and \citeA{sinclair19} showed that within the northern auroral oval the abundance can be as high as 0.8\% of the C\textsubscript{2}H\textsubscript{2} abundance, a factor of 8 higher than our a priori. The transmission curve for this higher value is shown by the dashed purple line in Figure~\ref{fig:gases}, showing that C\textsubscript{6}H\textsubscript{6} can also have a significant impact on the shape of Jupiter's 175--205 nm spectrum and must therefore be considered in the following analysis.

\subsection{Reflectance maps}
\label{sec:maps}

Figure~\ref{fig:maps} shows reflectance maps of Jupiter's southern and northern polar regions at wavelengths of 175--190 nm. As described in Section~\ref{sec:observations}, Juno UVS observations were converted from radiance to reflectance by correcting for the solar incidence angle and dividing by the solar spectrum \cite{woods09}. The maps shown in Figure~\ref{fig:maps} combine all dayside (local time of 8 AM to 4 PM, solar zenith angle less than 85$^{\circ}$) data obtained during the first 46 perijoves of the Juno mission (July 2016 - November 2022). The maps comprise observations made at a range of different spacecraft positions, spanning radial distances of 1.3--9.7 R\textsubscript{J}.

Because of the precession of the spacecraft orbit, the southern hemisphere (Figures~\ref{fig:maps}(a) and~\ref{fig:maps}(b)) has significantly better spatial coverage and signal-to-noise ratios than the northern hemisphere (Figures~\ref{fig:maps}(c) and~\ref{fig:maps}(d)). The higher noise level means that some `striping' is visible in the northern data. Figures in the right column are identical to figures in the left column but have a different grayscale stretch to highlight different morphologies. The average locations of the expanded and contracted auroral ovals \cite{bonfond17b} are shown in red.

\begin{figure}
\centering
\includegraphics[width=12cm]{combined_perijoves.png}
\caption{UV reflectance maps of Jupiter's south pole ((a) and (b)) and north pole ((c) and (d)). The figures show the mean reflectance in the 175--190 nm spectral range, which is sensitive to C\textsubscript{2}H\textsubscript{2} absorption. (b) and (d) show the same data as (a) and (c) but have a different grayscale stretch to highlight different morphologies. The average locations of the expanded and contracted auroral ovals \cite{bonfond17b} are shown in red.}
\label{fig:maps}
\end{figure}

The wavelength range of 175--190 nm was chosen because this is a spectral region that is sensitive to absorption by C\textsubscript{2}H\textsubscript{2}, as shown in Figure~\ref{fig:gases}. While slightly shorter wavelengths would be even more sensitive (C\textsubscript{2}H\textsubscript{2} has a local absorption maximum at $\sim$172 nm), shorter wavelengths are also increasingly sensitive to H\textsubscript{2 }auroral emissions that peak near 160 nm and lead to misleadingly high reflectances along the auroral ovals; 175--190 nm represents a spectral region that is sensitive to C\textsubscript{2}H\textsubscript{2} while minimizing the contamination from auroral emission.

Figure~\ref{fig:maps}(a) shows that the reflectance at all longitudes decreases towards the south pole. This is a well-known phenomenon and is caused by presence of stratospheric hazes at both poles; these hazes lead to a distinctive appearance in both the infrared and the ultraviolet \cite{west04}. In the infrared, there is a bright  ``polar hood'' in methane-band observations, due to the fact that the stratospheric haze particles scatter light before it has the chance to be absorbed by methane. In contrast, the UV polar hood is dark, as seen in Figure~\ref{fig:maps}(a), because the haze particles are less reflective than the Rayleigh-scattering molecular atmosphere.

Although the entire polar region in Figure~\ref{fig:maps}(a) is relatively dark, the segment within the southern auroral oval (marked by the red lines) is darker than the adjacent longitudes. This can be seen more clearly in Figure~\ref{fig:maps}(b), which presents the same data as Figure~\ref{fig:maps}(a) but with a different grayscale stretch to highlight morphology within the darkest regions. There is a distinct dark patch which aligns closely with the location of the auroral oval; the reflectance within the auroral oval is 0.02, while the mean reflectance at similar latitudes outside the oval is 0.05. A similar effect can be seen at the north pole, shown in Figures~\ref{fig:maps}(c) and~\ref{fig:maps}(d). These observations are noisier and have decreased coverage, but the same approximate trend can be seen; the region within the auroral oval has an even lower reflectance than the rest of the pole. These observations could be due to an increase in the haze concentration within the auroral ovals, which would lead to a local enhancement of the effect that causes the broader polar hood. Alternatively, it could be due to an increase in the C\textsubscript{2}H\textsubscript{2} and/or C\textsubscript{6}H\textsubscript{6} abundances, both of which would lead to increased absorption at 175--190 nm and therefore lower reflectance. In order to distinguish between these scenarios, we consider the full UVS spectra in Section~\ref{sec:spectra}.

\subsection{Spectra}
\label{sec:spectra}

To further explore how the UV reflectance varies across the polar region, we now consider the full UVS spectra. In order to obtain a sufficient signal-to-noise ratio, we focus solely on the southern polar region and co-add data to produce two representative spectra: (i) the polar auroral region, defined as within the contracted auroral oval, and (ii) the polar quiescent region, defined as outside the expanded auroral oval, but still poleward of 67.2$^{\circ}$S (the most-equatorward point of the expanded oval). In both cases, the data is limited to local times of 8 AM to 4 PM and is corrected for the solar incidence angle, as in Figure~\ref{fig:maps}.

\begin{figure}
\centering
\includegraphics[width=14cm]{spectra.png}
\caption{Comparison of UV spectra from the polar auroral and quiescent regions of Jupiter's southern pole. The polar auroral region is defined as within the contracted auroral oval and the polar quiescent region is defined as outside the expanded auroral oval but poleward of  of 67.2$^{\circ}$S. (a) and (b) show dayside spectra from the two regions (black) alongside a pure auroral emission spectrum (red). (c) and (d) show the reflectance spectra from the two regions once the auroral emission component has been removed; the spectral range dominated by the auroral emission is shaded out. (e) shows the ratio of the two spectra shown in (c) and (d). The wavelength range where an absorption feature is present is highlighted by the arrows.}
\label{fig:spectra}
\end{figure}

The representative spectra from inside and outside the southern auroral oval are shown in black in Figures~\ref{fig:spectra}(a) and~\ref{fig:spectra}(b) respectively. Because these spectra are obtained from the dayside of the planet in a spatial region with significant auroral emission, they consist of a combination of reflected sunlight and auroral emission. At longer wavelengths (\textgreater175 nm), the reflected sunlight component dominates, and at shorter wavelengths (\textless165 nm), the auroral emission dominates. The spectrum from the polar `quiescent' region still has a strong auroral emission component due to the diffuse equatorward emissions from the regions closest to the auroral oval.

In order to obtain a spectrum that consists of purely reflected sunlight, we first obtained a pure auroral spectrum by coadding polar data obtained during night time. This pure auroral spectrum is shown in red in Figures~\ref{fig:spectra}(a) and~\ref{fig:spectra}(b), and in each case, has been scaled to match the average radiance of the dayside spectrum at 157--160 nm. By subtracting these auroral spectra from the dayside spectra, and then dividing by the solar spectrum, we were able to produce the `clean' reflectance spectra shown in Figures~\ref{fig:spectra}(c) and~\ref{fig:spectra}(d).

Figures~\ref{fig:spectra}(c) and~\ref{fig:spectra}(d) have noticeably different spectral shapes. Figure~\ref{fig:spectra}(c), the reflectance spectrum from the polar auroral region, has a steep slope between 175 nm and 195 nm, while Figure~\ref{fig:spectra}(d), the spectrum from the quiescent region, is significantly flatter. Figure~\ref{fig:spectra}(e) further compares the two reflectance spectra by showing a ratio of the polar auroral region to the quiescent region. At 195--205 nm, the relative reflectance from the polar auroral region is relatively constant and $\sim$50\% of the reflectance at quiescent longitudes. This then decreases to $\sim$20\% by 175 nm, before increasing again at shorter wavelengths. The shape shown in Figure~\ref{fig:spectra}(e) is very similar to the shape of the C\textsubscript{2}H\textsubscript{2} absorption feature shown in Figure~\ref{fig:gases}, and is also consistent with the presence of C\textsubscript{6}H\textsubscript{6}. This suggests that the decreased reflectance at 175--190 nm in the polar auroral region is at least partially driven by an increase in these hydrocarbons.

\subsection{Proxy C\textsubscript{2}H\textsubscript{2} and C\textsubscript{6}H\textsubscript{6} abundance maps}
\label{sec:modeling}

In \citeA{giles21b}, we used a radiative transfer and retrieval algorithm to model Juno UVS reflected sunlight spectra from Jupiter's low- and mid-latitudes in order to retrieve the zonally-averaged C\textsubscript{2}H\textsubscript{2} abundances. Ideally, we would perform a similar analysis for the polar region, in order to produce spatially-resolved C\textsubscript{2}H\textsubscript{2} maps and to determine the extent to which any variability in the C\textsubscript{6}H\textsubscript{6} abundance may affect these results. However, the high solar incidence angle at the poles means that the signal-to-noise ratios of the reflected sunlight spectra are significantly lower than they were at low latitudes, and this is compounded by the fact that we are interested in spatial variability on relatively small scales and therefore cannot co-add large spatial regions to reduce the noise. Instead, we can use the ratio between the reflectance at 175--190 nm and the reflectance at 190--205 nm as a proxy for the C\textsubscript{2}H\textsubscript{2} and C\textsubscript{6}H\textsubscript{6} abundances.

\begin{figure}
\centering
\includegraphics[width=9cm]{ratios.png}
\caption{(a) Synthetic reflectance spectra of Jupiter assuming a solar incidence angle of 80$^{\circ}$ and a haze-free atmosphere. The spectrum without either C\textsubscript{2}H\textsubscript{2} or C\textsubscript{6}H\textsubscript{6} is shown in black, the spectrum with the nominal C\textsubscript{2}H\textsubscript{2} abundance is shown in red and the spectrum with the nominal C\textsubscript{6}H\textsubscript{6} abundance is shown in blue. The two spectral regions used to calculate the reflectance ratio in (b) and (c) are shown by the arrows. (b) The relationship between the the C\textsubscript{2}H\textsubscript{2} scaling factor relative to the nominal vertical profile and the reflectance ratio for four different cloud models. (c) The relationship between the the C\textsubscript{6}H\textsubscript{6} scaling factor relative to the nominal vertical profile and the reflectance ratio for four different cloud models.}
\label{fig:ratio}
\end{figure}

Figure~\ref{fig:ratio}(a) shows three synthetic reflectance spectra generated using the NEMESIS radiative transfer code \cite{irwin08} and smoothed to match the spectral resolution of Juno UVS. The adaptation of NEMESIS for use in the UV spectral region is described in \citeA{melin20} and \citeA{giles21b}. As described in Section~\ref{sec:molecules}, we use the Model C atmosphere from \citeA{moses05} as the nominal atmospheric model for Jupiter. The black line in Figure~\ref{fig:ratio}(a) shows the reflectance spectrum of Jupiter if C\textsubscript{2}H\textsubscript{2} and C\textsubscript{6}H\textsubscript{6} are removed from the atmosphere, in the absence of any hazes and assuming a solar incidence angle of 80$^{\circ}$. The red line shows how the spectrum changes when the nominal C\textsubscript{2}H\textsubscript{2} abundance is included and the blue line shows the spectrum when the nominal C\textsubscript{6}H\textsubscript{6} abundance (0.1\% of the C\textsubscript{2}H\textsubscript{2} abundance) is included. Both species can clearly have an impact on the ratio between the mean reflectance at 175--190 nm and the mean reflectance at 190--205 nm; the ratio with no C\textsubscript{2}H\textsubscript{2} or C\textsubscript{6}H\textsubscript{6} is 1.00, the ratio with C\textsubscript{2}H\textsubscript{2} alone is 0.52 and the ratio with the C\textsubscript{6}H\textsubscript{6} alone is 0.89.

Similar reflectance spectra were generated for a range of C\textsubscript{2}H\textsubscript{2} vertical profiles, each consisting of the nominal vertical profile multiplied by a scaling factor between 0 and 3. For each C\textsubscript{2}H\textsubscript{2} scaling factor, the ratio between the mean reflectance at 175--190 nm and the mean reflectance at 190--205 nm was measured. The relationship between the C\textsubscript{2}H\textsubscript{2} scaling factor and the reflectance ratio is shown by the black curve in Figure~\ref{fig:ratio}(b); as the C\textsubscript{2}H\textsubscript{2} abundance increases, the reflectance at 175--190 nm decreases relative to the reflectance at 190--205 nm and so the reflectance ratio decreases.

The presence of polar hazes can impact the spectral shape. Jupiter's polar hazes are thought to include a range of particle sizes, with mean radii of approximately 0.09--1.1 \textmu m \cite{wong03}. This distribution of particle sizes leads to absorption that is expected to be approximately spectrally flat over the 165--205 nm wavelength range. However, even a spectrally-flat haze can affect the shape of the spectrum if it is located within the altitude region of peak sensitivity; as discussed in \citeA{giles21b}, the longer wavelength end of the UVS spectrum probes deeper into the atmosphere and therefore can be more impacted by the presence of haze, leading to a tilt in the spectrum and increasing the reflectance ratio.

This can be seen by the colored lines in Figure~\ref{fig:ratio}(b) which show the C\textsubscript{2}H\textsubscript{2}--reflectance ratio curves for the three different haze models used in \citeA{giles21b}: a compact layer at 10 \textmu bar, a compact layer at 5 mbar and an extended haze with constant density in the 100--1 mbar range, based on \citeA{wong03}. In each case, the optical thickness of the haze layer was scaled to match the optical thickness retrieved at a latitude of 75$^{\circ}$S in \citeA{giles21b}. For a given C\textsubscript{2}H\textsubscript{2} abundance, the presence of haze acts to increase the reflectance ratio of the synthetic spectrum and for a given observed reflectance ratio, the black no-haze curve shows the corresponding minimum C\textsubscript{2}H\textsubscript{2} scaling factor. However, despite the quantitative differences, the results from all four models shown in Figure~\ref{fig:ratio}(b) are qualitatively similar, showing that as the C\textsubscript{2}H\textsubscript{2} scaling factor increases, the reflectance ratio decreases.

The same method was used to study the effect of varying the C\textsubscript{6}H\textsubscript{6} abundance on the reflectance ratio. Figure~\ref{fig:ratio}(c) shows the relationship between the C\textsubscript{6}H\textsubscript{6} scaling factor and the reflectance ratio for each of the same four haze models. We present a larger range of scaling factors for C\textsubscript{6}H\textsubscript{6} (0--50) than we did for C\textsubscript{2}H\textsubscript{2} (0--3) for two reasons; firstly, the a priori C\textsubscript{6}H\textsubscript{6} abundance is not well constrained, and secondly, a much higher scaling factor is required to significantly decrease the reflectance ratio. Figure~\ref{fig:ratio}(c) shows that a scaling factor of 8, which is the abundance found by \citeA{sinclair19} at Jupiter's northern auroral oval, produces a reflectance ratio of 0.88 using the most realistic extended haze model. The reflectance ratio begins to level off beyond this, and even a scaling factor of 50 can only achieve a reflectance ratio of 0.73. Continuing to increase the C\textsubscript{6}H\textsubscript{6} abundance even further ultimately increases the reflectance ratio instead, as the small C\textsubscript{6}H\textsubscript{6} absorption features at $\sim$200 nm begin to have a greater effect; for the extended haze model, the minimum reflectance ratio that can be achieved using C\textsubscript{6}H\textsubscript{6} alone is 0.61, with a scaling factor of 225$\times$ the nominal value. This shows that while C\textsubscript{6}H\textsubscript{6} does influence the reflectance spectrum 175--205 nm, C\textsubscript{2}H\textsubscript{2} absorption must be primarily responsible for any regions of the planet with very low reflectance ratios.

\begin{figure}
\centering
\includegraphics[width=12cm]{scaling_factors.png}
\caption{(a)--(b) The ratio of the mean reflectance at 175--190 nm to the mean reflectance at 190--205 nm for Jupiter's south and north poles. (c)--(d) Proxy C\textsubscript{2}H\textsubscript{2} abundance maps assuming no C\textsubscript{6}H\textsubscript{6} absorption. (e)--(f) Proxy C\textsubscript{6}H\textsubscript{6} abundance maps assuming no C\textsubscript{2}H\textsubscript{2} absorption. The average locations of the expanded and contracted auroral ovals \cite{bonfond17b} are shown in black.}
\label{fig:ratio_map}
\end{figure}

Figures~\ref{fig:ratio_map}(a) and ~\ref{fig:ratio_map}(b) show reflectance ratio maps of Jupiter's north and south poles. The 175--190 nm reflectance maps shown in Figure~\ref{fig:maps} were divided by equivalent maps covering the 190--205 nm spectral range. As expected from Figure~\ref{fig:spectra}, Figures~\ref{fig:ratio_map}(a) shows that there is a region of low reflectance ratio which coincides with the polar aurora within the southern auroral oval. This low reflectance ratio within the auroral oval is markedly different from the adjacent, quiescent longitudes. Figure~\ref{fig:ratio_map}(b) shows a hint of a similar trend, with a lower reflectance ratio within the northern auroral oval, but the decreased spatial coverage and noisier data make this less clear-cut.

Figure~\ref{fig:ratio_map}(c) shows the southern reflectance ratio map converted into a C\textsubscript{2}H\textsubscript{2} scaling factor, in the absence of C\textsubscript{6}H\textsubscript{6}. For each latitude, we use the appropriate haze opacity retrieved in~\citeA{giles21b} using the extended haze model. The haze retrievals do not extend beyond $\pm75^{\circ}$, so poleward of this a constant haze opacity is assumed. For these polar latitudes, the conversion relationship between reflectance ratio and C\textsubscript{2}H\textsubscript{2} scaling factor is shown by the orange line in Figure~\ref{fig:ratio}(b); for regions of the planet equatorward of $\pm75^{\circ}$, the conversion relationship falls between the orange line and black, haze-free line. As expected from~\citeA{giles21b}, Figure~\ref{fig:ratio_map}(c) shows that outside of the auroral region, the C\textsubscript{2}H\textsubscript{2} abundance decreases towards higher latitudes. In the polar auroral region, however, this trend is reversed. Figure~\ref{fig:ratio_map}(c) shows that the low reflectance within the auroral oval can be explained by a significant enhancement in the C\textsubscript{2}H\textsubscript{2} abundance; the mean C\textsubscript{2}H\textsubscript{2} scaling factor for the polar auroral region within the auroral oval is 2.5 compared to 0.8 at comparable latitudes outside of the auroral oval. Just as  Figure~\ref{fig:ratio_map}(b) showed a hint of the same reflectance ratio trend as Figure~\ref{fig:ratio_map}(a), Figure~\ref{fig:ratio_map}(d) shows a hint of the same C\textsubscript{2}H\textsubscript{2} enhancement within the northern auroral oval, but the noisy data prevents any firm conclusions from being drawn.

Figures~\ref{fig:ratio_map}(e) and~\ref{fig:ratio_map}(f) shows the reflectance ratio maps converted into C\textsubscript{6}H\textsubscript{6} scaling factors instead, in the absence of C\textsubscript{2}H\textsubscript{2}. Figure~\ref{fig:ratio_map}(e) shows that outside of the auroral oval, absorption from C\textsubscript{6}H\textsubscript{6} is technically able to reproduce the observed reflectance ratios, although it should be noted that we know from the full radiative transfer retrievals in~\citeA{giles21b} that the low-latitude spectral shape is actually due to C\textsubscript{2}H\textsubscript{2} absorption. However, within the southern auroral oval, there is no amount of C\textsubscript{6}H\textsubscript{6} that can reproduce the low reflectance ratios observed, which is why that region of the map in Figures~\ref{fig:ratio_map}(e) is empty. This can be further seen in Figure~\ref{fig:c6h6_c2h2}, which shows the combination of C\textsubscript{2}H\textsubscript{2} and C\textsubscript{6}H\textsubscript{6} scaling factors that are together able to produce a synthetic spectrum reflectance ratio of 0.52, the mean value within the southern auroral oval. As the C\textsubscript{6}H\textsubscript{6} increases, slightly less C\textsubscript{2}H\textsubscript{2} is required, but an extremely high levels of C\textsubscript{6}H\textsubscript{6} (\textgreater23$\times$ the a priori) the corresponding C\textsubscript{2}H\textsubscript{2} abundance starts to increase again. For this specific reflectance ratio, the C\textsubscript{2}H\textsubscript{2} scaling factor must fall in the 1.8--2.3 range, marked by the dashed lines. Since C\textsubscript{6}H\textsubscript{6} is unable to reproduce the low reflectance ratios within Jupiter's southern auroral oval, we can conclude that this effect must be primarily driven by a C\textsubscript{2}H\textsubscript{2} enhancement, with any possible enhancement in C\textsubscript{6}H\textsubscript{6} decreasing the C\textsubscript{2}H\textsubscript{2} abundances by up to 20\%.

\begin{figure}
\centering
\includegraphics[width=7cm]{c6h6_c2h2.png}
\caption{The combination of C\textsubscript{2}H\textsubscript{2} and C\textsubscript{6}H\textsubscript{6} scaling factors that are able to reproduce a reflectance ratio of 0.52, the mean value within the southern auroral oval. The minimum and maximum C\textsubscript{2}H\textsubscript{2} scaling factors are marked by the dashed lines.}
\label{fig:c6h6_c2h2}
\end{figure}

It should also be noted that there is some error associated with the haze opacity. In Sections~\ref{sec:maps} and~\ref{sec:spectra}, we noted that the decreased reflectance within the auroral oval could be partially caused by an increase in the haze opacity, as well as an increase in the hydrocarbon abundances, but in Figure~\ref{fig:ratio_map} we assume a constant haze opacity poleward of $\pm75^{\circ}$. However, if the hazes were more opaque within the polar auroral region, the contrast in the C\textsubscript{2}H\textsubscript{2} scaling factor within the oval relative to the scaling factor at quiescent longitudes would actually be even greater than what is shown in Figures~\ref{fig:ratio_map}(c) and~\ref{fig:ratio_map}(d). Figure~\ref{fig:ratio}(b) showed that when additional hazes are present in a model, an even higher C\textsubscript{2}H\textsubscript{2} abundance is required to produce a given reflectance ratio. The presence of additional hazes can therefore only intensify the polar auroral phenomenon shown in Figure~\ref{fig:ratio_map}.

A similar effect exists with respect to the auroral emissions within the polar region. The wavelength interval of 175--190 nm was chosen in order to minimize the contribution of the auroral emissions which peak at $\sim$160 nm (see Figures~\ref{fig:spectra}(a) and \ref{fig:spectra}(b)). However, the edge of this emission feature may still contribute a small amount of flux, which would act to slightly increase the apparent reflectance within this interval, and therefore increase the ratio of the 175--190 nm reflectance to the 190--205 nm reflectance. Accounting for any such emission component would therefore further decrease the reflectance ratio within and in the immediate vicinity of the auroral ovals, while the reflectance ratio in the quiescent auroral regions would remain the same. Accounting for any residual auroral emission would therefore only act to intensify the polar auroral phenomenon shown in Figure~\ref{fig:ratio_map}.

In summary, we can conclude that the C\textsubscript{2}H\textsubscript{2} abundance is significantly enhanced within Jupiter's southern auroral oval. There are three factors that can act to modify the C\textsubscript{2}H\textsubscript{2} scaling factors presented in Figure~\ref{fig:ratio}(c): the presence of C\textsubscript{6}H\textsubscript{6}, the presence of additional hazes and residual auroral emissions. While the first of these can decrease the auroral C\textsubscript{2}H\textsubscript{2} abundance by up to $\sim$20\%, the latter two would both act to actually further increase the auroral C\textsubscript{2}H\textsubscript{2} abundance. A similar trend may exist for the northern auroral oval, but the poor spatial coverage and signal-to-noise ratio prevent us from drawing any firm conclusions from the Juno UVS data.

\section{Discussion}
\label{sec:discussion}

In Section~\ref{sec:results}, we showed that the shape of Jupiter's reflectance spectrum varies significantly across the polar regions of the planet, and that this change in shape can be used to infer spatial variability in the C\textsubscript{2}H\textsubscript{2} abundance. As described in \citeA{giles21b}, the UVS reflected sunlight spectrum is sensitive to the total column abundance down to the 5--50 mbar region, but the C\textsubscript{2}H\textsubscript{2} number density peaks at 0.55 mbar \cite{moses05} and it is therefore this part of the atmosphere that has the strongest influence on the spectral shape. In the south pole, the C\textsubscript{2}H\textsubscript{2} abundance generally decreases towards higher latitudes, with the exception of the auroral region; within the southern auroral oval, the C\textsubscript{2}H\textsubscript{2} abundance is higher than the abundance at low latitudes and is a factor of $\sim$3 higher than adjacent quiescent, non-auroral longitudes. It is possible that there is also an enhancement in the C\textsubscript{6}H\textsubscript{6} abundance within the auroral ovals, as shown from infrared observations by~\citeA{sinclair19}, but the UVS data cannot independently confirm this.

The decrease in the C\textsubscript{2}H\textsubscript{2} abundance towards higher latitudes is consistent with previous studies that have performed full radiative transfer retrievals as a function of latitude. \citeA{giles21b} used zonally-averaged Juno UVS data to study the latitudinal variability of C\textsubscript{2}H\textsubscript{2} and found that the abundance decreased by a factor of 2--4 towards the poles. Similar results were also obtained using infrared observations from the Cassini spacecraft \cite{nixon07} and from ground-based telescopes \cite{fletcher16,melin18}.

The enhancement of C\textsubscript{2}H\textsubscript{2} within the southern polar auroral region is similar to results from \citeA{drossart86} and \citeA{sinclair17b,sinclair18}. \citeA{drossart86} analyzed FPGS data from NASA's Infrared Telescope Facility (IRTF) and found that there was a localized region of strong C\textsubscript{2}H\textsubscript{2} emission that coincided with the location of Jupiter's northern auroral oval. They concluded that this could be due to either a thermal anomaly or an enhancement in C\textsubscript{2}H\textsubscript{2}. More recently, \citeA{sinclair17b,sinclair18} used infrared observations from spacecraft and ground-based telescopes to simultaneously retrieve temperatures and hydrocarbon abundances in Jupiter's polar regions. \citeA{sinclair17b} used data from Voyager IRIS and Cassini CIRS, while \citeA{sinclair18} performed similar analyses using data from the TEXES spectrograph at the IRTF. All three sets of infrared observations showed an enhancement in the C\textsubscript{2}H\textsubscript{2} abundance within the northern auroral oval, relative to the quiescent, non-auroral longitudes, although \citeA{sinclair17b,sinclair18} do note that there is some degeneracy between the thermal profile and the C\textsubscript{2}H\textsubscript{2} abundance.

The results presented in this study build upon the previous works in two ways. Firstly, \citeA{drossart86} and \citeA{sinclair17b,sinclair18} found C\textsubscript{2}H\textsubscript{2} enhancements in the northern polar auroral region, but the southern aurora could not be clearly seen in the observations, because the viewing geometry in each case was close to equatorial and the southern auroral oval is restricted to high latitudes. In contrast, Juno UVS has significantly better coverage at the south pole than the north. Secondly, this study makes use of observations from a completely different spectral region; unlike previous infrared observations, the UV spectra used in this study are not sensitive to the temperature of the atmosphere so there is no degeneracy between the inferred C\textsubscript{2}H\textsubscript{2} abundance and the thermal profile. The striking similarity between the south polar map shown in Figure~\ref{fig:ratio_map}(a) and the north polar maps presented in \citeA{sinclair17b,sinclair18} acts to both confirm the latter's results using an independent spectral region and also show that the same phenomenon exists at both poles.

Stratospheric C\textsubscript{2}H\textsubscript{2} is thought to mainly form on Jupiter from photochemical by-products following methane photolysis \cite <e.g.,>{gladstone96}. The peak C\textsubscript{2}H\textsubscript{2} production regions are $4\times10^{-3}$\,mbar and 0.4\,mbar, and the freshly formed acetylene then diffuses downward to higher pressure levels \cite{hue18b}. The decrease in the C\textsubscript{2}H\textsubscript{2} abundance from the equator to the poles can be explained by the decrease in the solar insolation at high latitudes, and this observed latitudinal trend agrees with the results of photochemical models \cite{gladstone96,hue18b}. However, the low solar insolation rates at Jupiter's poles mean that an alternative mechanism is required to explain the high C\textsubscript{2}H\textsubscript{2} abundances within the auroral regions that were observed in both this work and in the previous infrared studies. The clear correlation between the location of Jupiter's polar aurora, which are located poleward of the main auroral oval, and the region of enhanced C\textsubscript{2}H\textsubscript{2} absorption suggests that the upper-atmosphere chemistry is being modified by the influx of charged auroral particles and the increase in ion-neutral and electron recombination reactions favors the production of C\textsubscript{2}H\textsubscript{2} \cite{sinclair17b}.

The majority of Jovian photochemical models neglect ion-neutral chemistry and while \citeA{kim94} did study the effect of hydrocarbon ions on the neutral ones, they focus on photoionization from solar extreme ultraviolet photons in the low- and mid-latitudes and make use of chemical networks that have since been updated, including updated reaction rates, additional chemical pathways, and updated branching ratios. In order to explore the exact mechanism by which auroral chemistry may favor C\textsubscript{2}H\textsubscript{2} production, we can instead consider an analogy with Titan's hydrocarbon chemistry, as discussed in \citeA{sinclair17b}. Several ion-neutral photochemical models of Titan's atmosphere have found that electron precipitation triggers the formation of the key ion CH\textsubscript{3}$^+$, which in turn leads to the formation of C\textsubscript{2}H\textsubscript{5}$^+$ \cite{delahaye08, Loison15, Dobrijevic16}. C\textsubscript{2}H\textsubscript{5}$^+$ can then lead to the formation of C\textsubscript{2}H\textsubscript{2} directly, through

\begin{center}
 \item C\textsubscript{2}H\textsubscript{5}$^+$ + e$^-$ 	$\rightarrow$ C\textsubscript{2}H\textsubscript{2} + H\textsubscript{2} + H
\end{center}

\noindent or indirectly, by first forming C\textsubscript{2}H\textsubscript{4}

\begin{center}
 \item C\textsubscript{2}H\textsubscript{5}$^+$ + e$^-$ 	$\rightarrow$ C\textsubscript{2}H\textsubscript{4} + H
  \item C\textsubscript{2}H\textsubscript{5}$^+$ + HCN 	$\rightarrow$ C\textsubscript{2}H\textsubscript{4} + HCNH$^+$
\end{center}

\noindent which is then photolyzed to produce C\textsubscript{2}H\textsubscript{2} and H\textsubscript{2}. A similar pathway could lead to the enhanced production of C\textsubscript{2}H\textsubscript{2} within Jupiter's auroral regions.

\citeA{kim94} suggested that C\textsubscript{2}H\textsubscript{2} would be easily destroyed in Jupiter's auroral regions due to ion chemistry, due to the reaction

\begin{center}
 CH\textsubscript{5}$^+$ + C\textsubscript{2}H\textsubscript{2} $\rightarrow$ C\textsubscript{2}H\textsubscript{3}$^+$ + CH\textsubscript{4}
\end{center}

In \citeA{Dobrijevic16}, the rate used for this reaction was 5\% slower than the rate used in \citeA{kim94}, leading to a slightly slower C\textsubscript{2}H\textsubscript{2} destruction rate. However, the reaction leading to the formation of CH\textsubscript{3}$^+$, the main building block of C\textsubscript{2}H\textsubscript{5}$^+$, was taken to be 9\% slower in \citeA{Dobrijevic16}, which might also decrease the C\textsubscript{2}H\textsubscript{2} production rate relative to \citeA{kim94}. While enhanced electron precipitation is a plausible driving mechanism for the enhanced C\textsubscript{2}H\textsubscript{2} abundances, the development of an ion-neutral photochemical model of Jupiter's polar regions, using the most recent reaction rates, is needed in order to reach a firm conclusion.

Both this study and \citeA{sinclair17b,sinclair18} have shown that the C\textsubscript{2}H\textsubscript{2} enhancement at Jupiter's poles is longitudinally-restricted to the auroras, instead of being well-mixed across the entire polar region. Jupiter's main auroral regions are encircled by electrojets \cite{rego99}, which have speeds of 1--2 kms\textsuperscript{-1 } and extend from the sub-\textmu bar level \cite{chaufray11} down to at least the middle stratosphere \cite{cavalie21}. One possibility is that these electrojets act as a dynamical barrier to limit the loss of materials produced within the auroras. Alternatively, C\textsubscript{2}H\textsubscript{2} may be efficiently transported outside of the auroral region into the quiescent region, but once in a location where neutral chemistry dominates, it may be rapidly converted into other chemical species such as C\textsubscript{2}H\textsubscript{6} before it can become homogenized across the entire polar region \cite{sinclair17b}. This latter scenario would also explain the increasing C\textsubscript{2}H\textsubscript{6} abundance from the equator to the poles observed by Cassini CIRS \cite{nixon07}, which cannot be explained by a combination of neutral photochemistry and dynamics alone \cite{hue18b}.

In order to obtain sufficient signal-to-noise ratio for this study, we combined observations from the entire Juno mission to date, a period of over 6 years. This means that we are unable to study any temporal variability in the C\textsubscript{2}H\textsubscript{2} auroral enhancement. If the C\textsubscript{2}H\textsubscript{2} auroral enhancement is caused by the influx of charged particles, we might expect the abundance to vary with time, depending on the strength and size of the auroras, which in turn may vary depending on both solar activity and internal factors within the Jovian system~\cite<e.g.>{bonfond12,nichols17,yao22}. The extent to which the C\textsubscript{2}H\textsubscript{2} abundance varies with time may provide additional constraints on the chemical lifetimes and transport rates in the auroral region. Future studies may be able to examine the temporal variability of auroral C\textsubscript{2}H\textsubscript{2}; long-term ground-based infrared observations can be used to track the C\textsubscript{2}H\textsubscript{2} emissions with time~\cite{sinclair18}, and the next-generation UVS instrument on the JUICE mission~\cite<Jupiter Icy Moons Explorer,>{grasset13} is expected to make observations of Jupiter's high latitudes starting in 2031 and will allow a direct comparison with these Juno UVS observations from 2016--2022.

\section{Conclusions}
\label{sec:conclusions}

Reflected sunlight observations from the UVS instrument on the Juno spacecraft show enhanced C\textsubscript{2}H\textsubscript{2} absorption within Jupiter's southern auroral oval. This builds on previous infrared observations which have shown higher C\textsubscript{2}H\textsubscript{2} abundances within the northern auroral oval \cite{sinclair17b,sinclair18}. Our ultraviolet observations both provide a confirmation for these previous results, making use of an independent spectral region, and show that the same phenomenon exists at both poles. Future studies are required to study whether the C\textsubscript{2}H\textsubscript{2} enhancement varies with time.

The localized enhancement of C\textsubscript{2}H\textsubscript{2} is likely caused by the influx of charged particles within Jupiter's auroras, which lead to increased ion-neutral and electron recombination reactions. Ion-neutral photochemical models of Titan's atmosphere provide insight into possible pathways that would favor the production of C\textsubscript{2}H\textsubscript{2} in Jupiter's auroral regions. The development of ion-neutral photochemical models of Jupiter, using the recent chemical reactions rates, is an important next step in understanding the influence of the auroras on Jupiter's polar composition.

\section*{Acknowledgements}

We are grateful to NASA and contributing institutions, which have made the Juno mission possible. This work was funded by NASA's New Frontiers Program for Juno via contract with the Southwest Research Institute. BB is a Research Associate of the Fonds de la Recherche Scientifique - FNRS.

\section*{Data Availability Statement}

The Juno UVS data used in this paper are archived in NASA's Planetary Data System Atmospheres Node: https://pds-atmospheres.nmsu.edu/PDS/data/jnouvs\_3001 \cite{trantham14}. The data used to produce the figures in this paper are available in \citeA{giles23_data}. The NEMESIS radiative transfer and retrieval tool is available from \citeA{irwin20_nemesis}.

redpajama_set_name: RedPajamaArXiv


As our Administrative Assistant, Bethany will chase down and find a way to make our customers dreams a reality. She is the ultimate customer advocate! Bethany loves to cook, play disc golf, and cuddle with her three kitties. If she were a promotional product, she would be a branded mug because she likes to be cozy and always has coffee nearby.


Have you ever noticed that supermarkets often have damaged stuff at the front of the shelf? It might be a dented tin of baked beans or a frozen pizza where the box has got crushed. In fact I have even seen a sellotaped-up box of frozen fish fingers - can you believe that?
Now, this could either be down to a) customers have picked them up, changed their mind and put them down again with the result being that they get endlessly stuck at the front of the shelf, or b) the supermarket leaves them them in the hope that a frazzled customer who's in a hurry will pick them up by mistake.
Surely the best thing to do would be to just chuck any damaged goods out with the garbage? I would imagine the supermarket makes enough money without trying to get a few pence from damaged stuff. Or, here's an idea - sell these products off at a reduced price and by that, I mean a proper reduction not just a few pence off here and there.
It's not the first time I've ended up with a box of fresh orange juice but no plastic straw to push in the top. Also, I got a box of beefburgers home and discovered there was a hole in the box. So, yes, I should be more careful. I also think the supermarkets could just remove these products at the same time as they are checking the sell-by dates.
On a slightly different note and whilst we are talking about shopping and supermarkets, when the staff on the tills go for their breaks, could they try not to knock customers out of the way? I know we can be a pain in the backside but still - the stampede can be a bit obvious and it's difficult trying to pay for shopping when another cashier is trying to squeeze past to go for their fag break.
It's all because of people who don't care and who throw things around. In fact I'm more concerned about clothing/footwear being damaged by people who try them on - not just in TKMaxx. I've just seen in a large department store a £315 pair of shoes damaged to a state where nobody would want to pay the full price for it anymore. Makes me feel like I were in some uncivilized country rather than in the UK.
Most supermarkets will dump damaged goods in the reduction area, e.g. reducing something originally 3 for £10 to £3.25 each, in the hope that someone who is too thick with numbers would happily pick them up thinking he/she's got a real bargain.
If you can't be bothered to check if the straw is missing or there's a hole in your packet, do you honestly think a shelf stacker will.
Never ever pick anything from the front of the shelve or indeed top of the fruit and veg container, always go to the back or dig down.
Good one! It's funny isn't how we've all gone back to buying beef and I'm still not sure whether the situation has changed. I just HOPE a few loopholes have been closed. I now alternate vegeburgers with beefburgers so I should be ok at least half the time.
It is fairly common to find multipack items that have been opened and some of the contents removed. Used to see it with cans of beer or crisps, even sweets.
I am constantly frustrated by the number of goods with opened boxes, why people have to open a fresh box to 'see the contents' when there is already an open box defeats me. It's fair enough to check the contents if you are purchasing, but mostly people are just being nosey.
In our local B&Q they stock a lot of broken goods for sale on their shelves. Their management doesn't seem capable of managing their stock.
Quote... "Also, I got a box of beefburgers home and discovered there was a hole in the box."
At least it wasn't a horse.


text:
Q: How can I hide identifier names in compiled projects? When I compile a project containg code such as:
ttest = record
   one, two: string;
   three: integer;
end;

I can see in the EXE strings like "ttest", "one", "two", and "three".
This is in any verion of Delphi, even in Free Pascal.
Is there any possibility to not put this in the compiled program? Without using packers, encrypters, or the like.

A: Try turning off every kind of debug information you can find in the Project Options dialog (menu item Project/Options), then rebuild the whole project (i.e. not just Compile, use the Project/Build menu item so that every unit in the project is recompiled). That should fix it.
The actual options you have to deselect in the project options depend on your Delphi version: for Delphi 2006/Turbo Delphi, these include all options under Debugging on the Compiler tab (maybe except "Assertions") and on the Linker tab "Include TD32 debug info" / "Include remote debug symbols". Newer Delphi versions have a "Build Configuration" feature similar to Visual Studio, selecting "Release" here and rebuilding should remove all "telltale" debugging information.

A: Not sure that this will help, but check out create smaller delphi xe executable, it seems like removing the RTTI could solve your problem.

A: Just avoid to put your data as published, if possible, otherwise fields names are visible. Additionally, don't forget that every method created when cliking the property inspector is automatically put as published (because they are also used in the dfm files). So each 'Button1Click' etc is visible and therefore easily localizable (method code).
Just check any program compiled with Delphi in IDA free and with the special 'Delphi string IDC script (find it at the IDA palace)'.In the Names window you'll easy see every TSomething, every TSomething published properties and methods...

A: I solved the problem. Using "string" in records causes that the record name is visible in executable

redpajama_set_name: RedPajamaStackExchange


Wheel Conversion Plate - AndyMark Inc.
This conversion plate acts as a hub between larger motion components featuring a 1.875" bolt circle to components of a smaller mounting circle such as a NeveRest Gearmotor. The bore of this plate fits shafts that are familiar to FIRST Tech Challenge teams.


SLE News - International assistance is pouring into Sri Lanka as the government continued efforts to provide relief to tens of thousands of people affected by severe floods and landslides owing to days of heavy rains. Torrential rains in Sri Lanka has forced over 375,000 from their homes and stranded thousands in the worst flooding to hit the island in decades.
Two Indian naval ships with aid supplies are expected to reach the country on Saturday, in addition to an Indian transport carrier scheduled to arrive with relief supplies on Friday night, Defense Ministry officials said.
The United States has provided 50,000 US dollars for emergency humanitarian aid to meet the urgent needs of victims of the ongoing landslides and flooding, officials added.
The meager U.S. assistance is raising eyebrows in light of the boast by both sides of strengthened relations between Colombo and Washington. However, $50,000 is the maximum immediately available from the Office of Foreign Disaster Assistance (OFDA) for relief efforts.
Nepal which is facing challenges of its own recovering from the massive April 2015 earthquake that killed over 8000 people has contributed $100,000.
Chinese Foreign Minister Wang Yi has sent a message of condolence to Foreign Minister Mangala Samaraweera and expressed willingness to offer assistance, according to Xinhua news agency. But no funds have been released to Colombo.
"We believe that under the leadership of the Sri Lankan government, the people of Sri Lanka will definitely be able to overcome difficulties and the disaster," Foreign Minister Wang said in his message.
Other countries which have pledged assistance include Pakistan and Australia while the Commonwealth Secretary General Patricia Scotland on Friday called on Commonwealth member countries to provide support to Sri Lanka through coordinated operation in the aftermath of devastating landslides which struck in Sri Lanka's Kegalle District.
The Sri Lankan government estimates 200,000 of the displaced are from the capital of Colombo alone.
Evacuation efforts by the military continued in Colombo on Friday and Saturday as houses remained underwater due to severe rains in the past week.
The Navy said efforts were being made to evacuate families living in flood prone areas in case the rains continue. Navy boats were also patrolling the flooded areas distributing aid and water to the families who were residing in the upper floors of their houses.
"We are trying our best to evacuate the people, but many families do not want to move. We cannot leave them there. It is dangerous," Xinhua quoted a navy official involved in rescue efforts in flood hit Kollonnawa as saying.


text:
Coluber virgatus est un synonyme attribué à trois espèces de serpents du genre Elaphe  :
 Coluber virgatus Schlegel, 1837, synonyme de Elaphe climacophora (Boie, 1826)
 Coluber virgatus Temminck & Schlegel, 1837, synonyme de Elaphe quadrivirgata (Boie, 1826)
 Coluber virgatus Boettger, 1898, synonyme de Elaphe schrenckii Strauch, 1873

Synonyme de serpents (nom scientifique)
Colubrinae

redpajama_set_name: RedPajamaWikipedia


Armenians in the eastern U.S. are witnessing a unique "changing of the guards" in the leadership of the Apostolic Church. Both the Prelacy and the Diocese elected new spiritual leaders at their respective assemblies in May 2018. The Prelacy elected its vicar, Archbishop Anoushavan Tanielian, while the Diocese chose a long serving son, Hayr Daniel Findikian. Both men are immensely qualified to lead the church with their humility, intellect and spirituality. The former, already a bishop in the church, was confirmed and elevated by Catholicos Aram I of the Great House of Cilicia. The latter, currently a Vartabed, will be elevated to a bishop by Catholicos Karekin II, Catholicos of All Armenians later this spring. Both men, with renown credibility with the young generation, have created an air of excitement as they begin the next phase of their respective ministries. Father Daniel, who grew up in the Binghamton, New York parish, will become the first American-born Armenian to be consecrated a bishop and serve as Primate. This is a remarkable and worthy milestone in the evolution of the Armenian Diaspora.
Here's the issue or, should I say, the opportunity. His elevation should be a highly visible event that serves as an instrument to inspire emerging and future generations. His elevation is a foregone conclusion. The question is whether this "once in a lifetime event" will be optimized for the faithful. Hayr Daniel was elected in early May 2018, yet his elevation will have taken a full year… currently scheduled for May 11, 2019 at Holy Etchmiadzin. Our leaders should be viewing this event from a perspective of how to inspire and energize the Diocese. My understanding is that the consecration was delayed due to the renovation of the Cathedral at Holy Etchmiadzin. Sounds reasonable? Well, how about conducting the elevation in New York City at St. Vartan's Cathedral. As far as I know, there is no requirement to consecrate bishops at Holy Etchmiadzin. Hosting the consecration in New York City could have elevated the Primate months earlier and given access to thousands of those he will serve. Imagine the hundreds of perhaps thousands of young people who could have witnessed the elevation and proudly proclaimed years from now…. "I was there." Think of the future and the scores of faithful who would be inspired to serve when witnessing such a beautiful event. All the youth from St. Nersess summer studies programs and the seminary who have been students of Hayr Daniel would be there to share in the joy. Why is it so difficult to understand the needs of the faithful? Why are our leaders so removed from these issues?
Too often we are told that we just don't understand. Perhaps that's the problem.. .we do understand.
Instead a few hundred will travel to Armenia. There will be no live stream. The rest of us get to watch a replay. Wonderful. Our leaders must think beyond the small space they apparently reside in. It is simply a matter of how you view leadership. To serve or to be served? I am sure there are a litany of excuses. Too often we are told that we just don't understand. Perhaps that's the problem.. .we do understand. We just have a different perspective. With the challenges we face, our objective should always be based on inclusion.
A secondary benefit would be the opportunity for our Vehapar to demonstrate incredible public sensitivity to an important US Diocese by coming to America and offering this gift. Let's face it. Our church here in America is at a crossroad. On the one hand there are impressive programs happening at the parish and Diocesan level. However, they simply are not connecting to enough people. Our individual faith may grow but it does not necessarily equate to participation in the institution known as the Armenian Apostolic Church.
Our individual faith may grow but it does not necessarily equate to participation in the institution known as the Armenian Apostolic Church.
Leaders have a responsibility to reach beyond to bring others to new heights. Our people need what I will refer to as "emotional experiences" that touch their hearts. Once that connection is made to the church, identity will be established and commitment soon follows. Not an easy task but we must never lower our expectations. The stakes are too high. Given the public perception and credibility issues of Karekin II, it would have been a "win-win" for all to witness this marvelous blessing in New York City. Instead, we are left to wonder what could have been. How long must we endure sub-optimizing? Left with the mixed feeling that it could have much better. Yes, they have been given the authority, but the "followers" have a responsibility to make their expectations—their very needs—clear. The hierarchical structure of the church does not require the faithful to be silent. It is quite the opposite. Silence can be misinterpreted as ambivalence. That will only create more separation between the leaders and those they serve.
The good news is that the sun will rise, and Fr. Daniel will be elevated. We rejoice in the consecration to bishop of such a fine clergyman as Fr. Daniel. Armenians, for the most part are very passive when it comes to the church. Many consider discussing topics such as this or other challenges the church faces as being "negative" or "disrespectful." We must challenge ourselves to shift our thinking from a static church to a dynamic one. A dynamic church confronts it problems without fear that its mission will be compromised. It must believe that it will be enhanced. Of course, we all have different perspectives on what those changes or opportunities are, but imagine what a joyful institution the Armenian Church can be when the issues are debated and not the intentions of individuals. In today's church, unfortunately, our inability to provide an effective forum or process to discuss our challenges enables some to simply walk away. Decline can be a silent process. We cannot assume that new immigrants will continually replenish our local parishes, thus providing the perception of parish vitality. Creating an exciting and fresh environment that provides the spiritual nourishment to the faithful according to the Armenian Church is a long term challenge in the diaspora. We must seek every opportunity to help build that identity.
This particular opportunity is less about the Primate and more about Vehapar and others in positions of authority to use that authority for the benefit of the faithful in their journey to find Christ and the Armenian Church. We will wait for the next opportunity with the hope and prayer that it is realized. In the meantime, I encourage all, with love in your heart, to work for a stronger Armenian Church.
Stepan was raised in the Armenian community of Indian Orchard, MA at the St. Gregory Parish. A former member of the AYF Central Executive and the Eastern Prelacy Executive Council, he also served many years as a delegate to the Eastern Diocesan Assembly. Currently , he serves as a member of the board and executive committee of the National Association for Armenian Studies and Research (NAASR). He also serves on the board of the Armenian Heritage Foundation. Stepan is a retired executive in the computer storage industry and resides in the Boston area with his wife Susan. He has spent many years as a volunteer teacher of Armenian history and contemporary issues to the young generation and adults at schools, camps and churches. His interests include the Armenian diaspora, Armenia, sports and reading.
This article raises important points but ignores what all Armenians who leave our Church say: it is more of a national institution than a religious one. That it focuses more on the nation than on the dogma. This of course has roots in loss of national independence for most of our history, but in 21st century America, where Armenian-Americans have access to all the world's religions, the Armenian Church has to teach more theology and dogma. Otherwise more and more Armenians will become Protestants, Buddhists or whatever religion they feel brings them closer to God.
Well Said Moushetsi Azad – in addition to this as a devout Christian of Armenian origin residing in Sydney Australia I have not attended the Armenian Church for some time now due to the lack of inclusion , I love my Church don't get me wrong but when you are shunned away as i have many times due to the fact my Armenian is not so great I have had to scour the the streets of Sydney to find the lonely oriental churches like the local Coptic church which i have attended now a few times to sit there in a house of GOD still not belonging but at least understanding the holy scripture as it is spoken in English.
There is a great opportunity for the church in Sydney or the ones around the globe if they are willing to reach out to each Armenian household and bring that fire back to each family, our Church is beautiful our sermons even more. It dsont feel right when I have to light candles and huddle my family around me while I recite our holy Badarag each Sunday , even though my children love it they still need to know the Church is there for them !
Are you putting Protestants and Buddhists together at the same faith level? Protestants are Christians and believe in Devine God and the Holy Trinity and Buddhism is a man-made religion. Before you throwing them in the same pot, please read about occult religions.
I had the good fortune serving as acting director at diocese in 2015 during the 100th anniversary as well as signatory to the historic mass at national cathedral. We did a full 360 analysis of paying members and parishes. Fr. Daniel at the time was finding his place and respected him as a scholar. His challenge now is to be a spiritual leader beyond a theologian; which I hope time will allow him the well rounded experience. Most of us remember fondly poetic leadership of Primate T.M. As a NYC resident and 2nd to last chairman of diocesen parish, St. Gregory, a whole community of NYC residents have been lost (both votes and presence) with the diocese going back to 1990's not to mention the rest of other parishes which actually can vote. We hope our new Vicar and Surpazan Hyre will recharge the spiritual experience. On May 18th the Diocesen Primate will return to St. Vartan for a function; so not all is lost where as our 2nd grand daughter will be baptized also in St. Vartan on May 19th.
Thank you Mr. Piligian, you are so right ! The Consecration would have brought greater stature to St. Vartan as a Premier Cathedral in the number one city in the world. It would have elevated the stature of the rank of an "Armenian" Bishop within the clergy of the United States. It would have been an opportunity to coincide with the month of April and the commeration of the Genocide.. It would have provided Fr. Fidikian with greater publicity within the religious community participating at his elevation in St. Vartan's Cathedral and the publicity and opportunity of participation by the congregation of the Eastern Diocese……Just a few of the benefits…..maybe next time.


TORONTO (AP) The Toronto Maple Leafs signed restricted free-agent forward Connor Brown to a three-year contract extension Saturday.
The deal has an average annual value of $2.1 million per season.
The 23-year-old right winger had 20 goals and 16 assists in 82 regular-season games last season. He added an assist in six playoff games.


Does it matter where I create my notes?
I have imported a large amount of PDFs into Zotero. Retrieving the metadata creates a "parent" for each PDF. As I write notes about the article, I would like to make each note a separate entry, so I have been adding a note to the parent file (under the "notes" tab) rather than using the field that is visible when the PDF file itself is selected. I like being able to use the tag feature for each individual note so I can quickly get to the information from the article based on the tag.
My question is whether attaching the notes to the parent file rather than to the PDF file will create a problem with the citation feature in Scrivener since the citation information comes from the parent file and not the PDF?
What you are doing already is the recommended practice.
You should generally always work with "Parent" items in Zotero, as these allow for full metadata, citing in word processors, formatting references, etc. It's usually best to use notes attached to the parent item to store notes about an item, rather than the note field that's part of the attachment item. I would recommend only using the tag and note fields that are part of the PDF attachment item to store comments specifically about the PDF file (e.g., I tag "online first" versions of a PDF as such so that I can go back and replace with the final version later; the Zotfile plugin stores extracted Tables of Contents in the PDF attachment item's note field).
One thing that you should be aware of is that having a very large number of notes can eventually slow down your library. I would generally recommend storing most/all of your notes about an item in one note attached to the parent. You can still tag this note and use Cmd/Ctrl+F to find things within the note.
Notes (either attached to the parent or to the attachment item) are not accessible to Scrivener or other citing methods. What exactly is your concern/use there?
Great! Thank you @bwiernik. I will use one note attached to the parent file and use the tags then.
My question re: Scrivener was whether attaching notes to the parent file in Zotero (which is where Scrivener pulls the citation information from) would screw up the citation in Scrivener. But if the notes are not accessible, then I am not concerned.
Technically, the attachments and notes are distinct items are distinct items in the Zotero database, but with a special relationship as being children to the parent item.


The 2016 Candidates Meet & Greet is scheduled for Wednesday, October 19, from 6:00 – 8:00 pm at The Renaissance Centre, 405 S. Brooks Street, Wake Forest. Candidates who are on the ballot in November will have tables and be available to speak with attendees. This is a free event open to the public.
Candidates who have confirmed their attendance are listed below (as of Oct. 19, 2016). Check back periodically for updates.


A lovely fixture, featuring discreet carving around a full upper band, a base medallion, and dramatic, multi-toned mineral veining. Recently rewired, the light holds three 60 watt incandescent bulbs, or three LED bulbs of any wattage equivalence.
Eileen Lane Antiques Pair of Art Deco Alabaster Pendants, ca. 1930.


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Bushmen aren't poachers: Protests greet Botswana President in London
Vocal protests were held outside the 'London Conference on the Illegal Wildlife Trade 2014' today to highlight the plight of Africa's last hunting Bushmen.
© Survival International
Loud protests at an anti-poaching conference in London today highlighted the devastating impact of a hunting ban on Africa's last hunting Bushmen in Botswana. Ian Khama, President of Botswana, was reported to be attending alongside Prince Charles and Prince William.
Protesters outside the 'London Conference on the Illegal Wildlife Trade 2014', chanted slogans and carried placards reading 'Botswana: Bushmen hunters are not poachers'.
Botswana is persecuting the Bushmen of the Central Kalahari Game Reserve in the name of wildlife conservation by stopping them from hunting game. But the Bushmen pose no threat to the wildlife of the CKGR, alongside which they have lived sustainably for centuries.
The Botswana government's hypocrisy was recently exposed by revelations that large parts of the CKGR have been leased out for fracking, and a mine by Gem Diamonds is projected to start operations inside the CKGR in October 2014.
A 2006 high court ruling confirmed the Bushmen's right to live and hunt in the CKGR, but the government continues to intimidate, torture and arrest Bushmen for hunting. The majority of Bushmen are forced to apply for restrictive permits to enter their ancestral land in the CKGR – a policy which has been likened to the hated Pass Laws under apartheid South Africa.
The Bushmen are prevented from hunting game on their ancestral land in the name of conservation, which a judge likened to condemning the tribe to 'death by starvation'.
© Survival
A high court judge involved in the 2006 court case said that the government's refusal to allow the Bushmen to hunt 'was tantamount to condemning the [Bushmen] to death by starvation.'
Survival has launched a travel boycott of Botswana and an ad campaign highlighting the government's drive to deport the Bushmen from their land. The boycott has been supported by thousands of travelers and by celebrities Gillian Anderson, Quentin Blake, Joanna Lumley, Sophie Okonedo, and Mark Rylance.
Survival's Director Stephen Corry said today, 'President Khama should not hide the persecution of the Bushmen behind the mask of conservation. To ban the Bushmen from hunting while at the same time opening up the reserve to fracking and mining is sheer hypocrisy.'
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redpajama_set_name: RedPajamaCommonCrawl


The definition of automate is "to run or operate by using machines and computers instead of people to do the work." So naturally, for the Automate Contest we are looking for projects that automate some process or task that might otherwise be done by human hands or brain.
We've got some amazing prizes up for grabs: a Tessel Master Pack (complete with every Tessel product, from accelerometers to cameras to GPS), Beginner Packs, and gift certificates to the Tessel shop. We'll be judging the entries based on clarity ingenuity, creativity, quality of presentation, and execution of the Instructable.
The Automation Contest is closed.
Create a new Instructable that fits the guidelines outlined in the contest description above. To be eligible, Instructables must be published between Mar 9, 2015 and Apr 20, 2015 (11:59pm PT).
Upon publishing your Instructable you'll see checkboxes for open contests. Select Automation Contest. If you have entries currently eligible for entry, it will also show up by clicking "Enter this Contest" on the right side of this page.
Sponsor. The Instructables Automation Contest (the "Contest") is an on-line contest with skill, ability and knowledge components that is sponsored by Autodesk, Inc., a Delaware corporation having its principal office at 111 McInnis Parkway, San Rafael, CA 94103, USA ("Sponsor"), in connection with the Instructables service and website, www.instructables.com, (the "Sponsor Site"). The Contest is co-sponsored by the company or companies listed here, if any (each, a "Co-Sponsor"): The Contest is governed by these Official Rules (these "Rules"). For any questions regarding the Contest, the Sponsor may be contacted by email at [service@instructables.com] or by mail at the address identified in Section B.18 ("Winner's List; Mailing List") below.
Winner Selection. There will be 19 total winner(s) for the Contest. The winner(s) will be selected on April 20, 2015, and Sponsor will announce the winner(s) on April 21, 2015. Each winner will be awarded only the prize(s) for which that winner was selected, as described below.


Count Miklós Bánffy de Losoncz (30 December 1873 — 5 June 1950) was a Hungarian nobleman, liberal politician, and historical novelist. His books include The Transylvanian Trilogy (They Were Counted, They Were Found Wanting and They Were Divided), and The Phoenix Land.
The native form of this personal name is losonczi gróf Bánffy Miklós. This article uses Western name order when mentioning individuals.
The Bánffy family emerged in 15th century Transylvania and established itself among the foremost dynasties of the country. They owned a grand palace in Kolozsvár (Romanian: Cluj-Napoca, German: Klausenburg), one of the main cities of Transylvania and one of the province's largest castles at Bonchida. One branch was raised to a barony in the 1660s, while another became counts in 1855. The barons produced a 19th-century prime minister of Hungary (Dezső Bánffy), and the counts held important offices at court. Among the latter was Count Miklós, born in Kolozsvár on December 30, 1873.
Beginning his political career at the time when Hungary was a constituent of Austria-Hungary, Bánffy was elected a Member of Parliament in 1901 and became Director of the Hungarian State Theatres (1913–1918). Both a traditionalist and a member of the avant-garde, he wrote five plays, two books of short stories, and a distinguished novel. Overcoming fierce opposition, his intervention made it possible for Béla Bartók's works to have their first performance in Budapest.
Bánffy became Foreign Minister of Hungary in his cousin Count István Bethlen's government of 1921. Although he detested the politics of the Regent, Admiral Miklós Horthy, he worked to review the boundary revisions confirmed by the Treaty of Trianon after World War I through which Transylvania had been transferred to Romania. Little progress was made, and he retired from office.
His trilogy, A Transylvanian Tale, also called The Writing on the Wall, was published between 1934 and 1940. Bánffy portrayed pre-war Hungary as a nation in decline, failed by a shortsighted aristocracy.
In April 1943, Bánffy visited Bucharest to persuade Ion Antonescu's Romania together with Hungary to abandon the Axis and sue for a separate peace with the Allies (see also Romania during World War II). The negotiations with a delegation led by Gheorghe Mironescu broke down almost instantaneously, as the two sides could not agree on a future status for Northern Transylvania (which Romania had ceded to Hungary in 1940, and where Bonchida was located). Two years later, in revenge for Bánffy's actions in Bucharest, his estate at Bonchida was burned and looted by the retreating German army.
Hungary and Transylvania were soon invaded by the Soviet Union's Red Army, an event which marked an uncertain status for Northern Transylvania until its return to Romania. His wife and daughter fled to Budapest while Bánffy remained on the spot in a vain attempt to prevent the destruction of his property. Soon after, the frontier was closed. The family remained separated until 1949, when he was allowed by Romanian communist authorities to leave for Budapest, where he died the following year.
A mellowing communist regime in Hungary permitted the reissue of A Transylvanian Tale in 1982, and it was translated into English for the first time in 1999. The Castle of Bonchida is now being restored as a cultural center. An apartment is being prepared for the use of the Count's family.


The United States became a spacefaring nation 60 years ago today.
On Jan. 31, 1958, the nation launched its first successful satellite — Explorer 1, which rode to Earth orbit atop a Jupiter-C rocket from Florida's Cape Canaveral Missile Annex (now called Cape Canaveral Air Force Station).
The success of Explorer 1 soothed a lot of jangled nerves among the American political and military elite, who had recently endured three humbling space setbacks.
The United States' first satellite, Explorer 1, launches into orbit atop a Jupiter-C rocket on Jan. 31, 1958.
The first two jolts came courtesy of the Soviet Union, which launched the first-ever artificial satellite, Sputnik 1, on Oct. 4, 1957, and followed that up a month later by lofting a dog named Laika to orbit, aboard the Sputnik 2 craft.
The United States tried to answer on Dec. 6, 1957, with a satellite launch of its own. But the rocket carrying the nation's first would-be spacecraft, the 3.5-lb. (1.6 kilograms) Vanguard Test Vehicle 3, burst into flames shortly after liftoff, live on national TV.
So, the Explorer 1 launch "certainly salved the open wound; there's no doubt about that," former NASA Chief Historian Roger Launius told Space.com last fall.
The satellite was designed and built by engineers at the Jet Propulsion Laboratory (JPL) in Pasadena, California. Today, JPL is one of NASA's flagship centers, but NASA didn't even exist when Explorer 1 lifted off; the space agency was officially established six months later, on July 29, 1958, and began operations on Oct. 1 of that year.
Members of the Explorer 1 team hoist a model of the satellite during a postlaunch news conference in 1958. From left: William Pickering, then-director of the Jet Propulsion Laboratory; James Van Allen, Explorer 1 principal investigator; and Wernher von Braun, chief of guided missile development operations for the Army Ballistic Missile Agency at Redstone Arsenal in Huntsville, Alabama.
Explorer 1 zoomed around Earth on a highly elliptical, 114-minute-long path that took it as close as 220 miles (354 kilometers) to Earth, and as far away as 1,563 miles (2,515 km). The satellite kept operating for nearly four months, blinking out when its batteries died on May 23, 1958. And it finally fell back to Earth on March 31, 1970, burning up in the atmosphere after completing more than 58,000 orbits, NASA officials said.
And, of course, NASA ended up making good on President John F. Kennedy's famous promise to put boots on the moon by the end of the 1960s. We'll celebrate the 50th anniversary of Apollo 11's spectacular achievement in July 2019.


This custom clothing retailer wanted to update their corporate office to be more inviting for clientele and to foster a better work environment for their employees.
Front of house updates included new flooring and paint. Custom built-ins for tie displays were also installed. Back of house improvements included new finishes and new low-panel workstations, which encourage collaboration between staff by opening the view throughout the office.


text:
Battery & Power Accessories
Does Jackery Have A Lithium Battery
The company is owned and managed by an ex-Apple Engineer who worked on the iPhone's batteries. The company was founded in 2012 and sold its first lithium power station in 2015. The lithium batteries are light and store a lot of charge. In 2015, the company was the first to manufacture off-grid lithium battery. The device is priced at $999. The device generates power using a pure sinewave inverter. This is safer for sensitive equipment, such as medical equipment, and can provide more than 10 hours of battery power.
The Jackery is a great design and easy to read. The LCD display shows the input, output, type of charging, and other information. It is easy to read, making it a great choice for those who don't know much about electronics. It is a great portable backup in case of emergencies. The unit also has a large capacity, which is good for those who have several electrical devices in their home.
The Jackery Explorer 1000 is an excellent choice for anyone who needs to keep their electronic equipment running for hours or even days. It is roughly the size of a microwave, and can provide a steady stream of power. The Jackery is quieter than portable generators powered by gas and can be used in emergency situations. The Jackery's user-friendly interface and rugged exterior makes it an ideal choice for any situation. The company is confident about its product and its design. Its customers can rely on it for their electrical needs.
The Jackery has an innovative design. Its LCD display is easy to read, and displays important information such as input and output voltage and temperature. You can also recharge the unit using a 120V outlet. The Jackery is not suitable for most high-powered electric appliances. It consumes 220-VAC, which is excessive for the unit. When fully charged, it can keep running for five hours or more.
The Jackery solar generator is a versatile tool for the outdoor life. It can charge a phone, laptop, and other devices. It also has a battery backup system. The system includes a Jackery solar panel. It can be used anywhere there is sunlight to charge your electronics. It is compatible with any outlet. The solar panel can be installed anywhere in your home. Its design and function make it a popular choice for people living in remote areas.
In addition to its innovative design, the Jackery solar generator also features a convenient LCD display. The large LCD screen displays information such as temperature, input voltage, charging time, and other useful information. The device also offers an integrated charging dock for your devices. If you're not sure whether your current device can work with the charger, be sure to check with the manufacturer. Some models include a backup battery. These models also come with LED flashlights that can be used for lighting up your space.
The Jackery solar generator offers many benefits. It is compact and can be stored anywhere. It can also charge your batteries. The device has multiple USB ports and an LCD screen that shows the input and output voltage. It also allows you to read the details of the battery. The LCD display will show you the charge time, type, and temperature of the unit. It will also display a detailed description of the charging time.
The Jackery solar generator features a foldable design and a user-friendly LCD display. Its large LCD screen makes it easy to use outdoors. Its panels fold up for storage and can be stored and folded away when not in use. It can charge the entire unit in just 5 hours and can continue running for as long as you need. If you want to buy a solar generator, consider this product.
The Jackery Explorer 1000 portable solar generator has a large battery that can run your electronic gear for hours or days. Its size makes it easy to carry and is about the size of a microwave. Its powerful battery can provide a steady supply of power and is quieter than portable generators powered by gas. Its robust exterior and many ports make it easy to use. It can charge your mobile phone, computer, and other electronic devices.
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Jackery Power Station 240 Vs 300
How Do You Charge Jackery Portable Charger
Solar-Power-Cable Jackery Solar Power Cable For E880/1000
Jackery 1000 Vs Bluetti
The Jackery Explorer 1000
Jackery Giant+ Premium 12000
Jackery Portable Charger Flashlight
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1-3 volunteers (maximum of 3) will provide enrichment activities for the children at the Crisis Nursery. The activities should be designed to enrich each child's experience and creativity and to reduce stress. Activities can include games, sports, arts and crafts, music, creative movement, puppetry, dance, etc. We strongly suggest a combination of activities. We have supplies and suggestions on site.
Children at the nursery have been exposed to chronic stress. Large muscle movement activities are encouraged to help release tension and to promote positive social interactions.
Volunteers must be 12 or older. Volunteers under age 16 must be accompanied by an adult age 21 or older.


text:
Q: Chrome dev tools exact computed value for CSS rules Is there anyway for instance I can get the exact pixel value (with decimal places) of a font to show in Chrome dev tools?
In Firebug (below) when I define a % value it shows the exact computed value in pixels up to 4 decimal places.

In Chrome dev tools (below) it only shows a whole number value.

In essence I want to be able to see in dev tools ► font-size: 13.7167px;
Thanks!

A: Yes, you simply need to view Computed Style under Chrome Dev Tools.
Dev Tools -> Elements -> Computed Style

A: In Chrome it may not give you the exact pixel value for one character, but it will give you the exact pixel size for the chunk of text if you look in computed under "width"