text:
Philipp Burkart (Lebensdaten unbekannt) war ein deutscher Fußballspieler.

Karriere

Burkart, der vom Treiben der 40 bis 50 Engländer im Alter von 16 bis 20 Jahren, der – seit dem Jahr 1889 in der Dreisamstraße eröffneten – englische Kadettenanstalt in den Bann gezogen wurde, gehörte neben Ernst Schottelius, Felix Hunn und 11 weiteren Mitschülern zu den Gründungsmitgliedern des Freiburger FC, dem er bis 1908 angehörte. Die Liebe zum neuen Sport ließ sie in den ersten Semestern ihres Hochschulstudiums noch in Freiburg verweilen, ehe sie es in der Folgezeit an anderen Universitäten fortsetzten.

Er nahm mit der Mannschaft an der vom Verband Süddeutscher Fußball-Vereine ersten ausgetragenen Endrunde um die Süddeutsche Meisterschaft 1898/99 teil. Das am 8. Januar 1899 in Karlsruhe erreichte Finale wurde mit 6:1 gegen den 1. FC Pforzheim gewonnen.

Die in der Folgesaison in drei Kreisen ausgetragenen Meisterschaftsspiele beendete er mit seiner Mannschaft als Sieger des 3. Kreises, die jedoch später an der weiteren Teilnahme zugunsten des zuvor mit 0:2 unterlegenen Straßburger FV verzichtete. Zu Beginn der Endrunde 1900/01 unterlag er mit dem Freiburger FC dem späteren Süddeutschen Meister Karlsruher FV mit 0:4 auf eigenem Platz.

1902/03 scheiterte er mit seiner Mannschaft in den Ausscheidungsspielen im Bezirk Württemberg am Straßburger FV mit 3:5 wie auch im Gau Oberrhein in der Saison 1903/04. Die Folgesaison rangierte er mit seiner Mannschaft punktgleich hinter dem Meister der Gauliga Oberrhein, dem FC Mühlhausen 1893, der den besseren Torquotient aufwies.

1905/06 wurde eben jener Verein im Endspiel mit 5:1 besiegt, doch in der sich anschließenden Endrunde um die Südkreismeisterschaft belegte er mit den Freiburgern den dritten und letzten Platz, da die Spiele gegen den 1. FC Pforzheim mit 1:3 und den FC Stuttgarter Cickers mit 2:3 verloren wurden.

Seine sportlich erfolgreichste Zeit folgte mit der Saison 1906/07 an dessen Ende drei regionale Meisterschaften und die erstmals errungene Deutsche Meisterschaft standen. Nachdem er in dem ab 1903 installierten Gau Oberrhein als eine der regional höchsten Spielklassen innerhalb des Südkreises mit seiner Mannschaft als Meister hervorgegangen war, nahm er auch an der sich anschließenden Endrunde um die Südkreismeisterschaft teil, die ebenfalls gewonnen wurde und zur Teilnahme an der Endrunde um die Süddeutsche Meisterschaft berechtigte. Nachdem das Hin- und Rückspiel des Halbfinales gegen den 1. Hanauer FC 1893 jeweils mit 1:0 am 14. und 21. April 1907 gewonnen wurde, erreichte der Freiburger FC das Finale. Beim 1. FC Nürnberg, dem Sieger des Ostkreises, der per Freilos ins Finale eingezogen war, wurde am 28. April ein 1:1-Unentschieden erzielt, das Rückspiel am 5. Mai mit 3:1 gewonnen. Als Teilnehmer an der Endrunde um die Deutsche Meisterschaft bestritt er am 12. Mai in Nürnberg das mit 3:2 gewonnene Halbfinale gegen den VfB Leipzig und das am 19. Mai in Mannheim mit 3:1 gewonnene Finale gegen den BTuFC Viktoria 89; in beiden Spielen erzielte er jeweils zwei Tore.

In der Folgesaison ging er mit seiner Mannschaft abermals als Meister im Gau Oberrhein hervor, belegte jedoch in der sich anschließenden Endrunde um die Südkreismeisterschaft lediglich den dritten und letzten Platz. Dennoch nahm er und seine Mannschaft als Titelverteidiger an der Endrunde um die Deutsche Meisterschaft teil. Die am 3. Mai 1908 im heimischen Stadion ausgetragene Viertelfinal-Begegnung mit dem FC Stuttgarter Cickers wurde beim Stand von 1:0 der Heimmannschaft aufgrund der Absicht des vorzeitigen Verlassens seiner Mitspieler vom DFB annulliert und für den 17. Mai 1908 neu angesetzt; das Wiederholungsspiel, das auch er erneut bestritt, wurde mit 2:5 verloren.

Erfolge
 Deutscher Meister 1907
 Süddeutscher Meister 1899, 1907
 Südkreismeister 1907
 Gaumeister Oberrhein 1906, 1907, 1908

Weblinks

Einzelnachweise

Fußballspieler (Freiburger FC)
Deutscher Meister (Fußball)
Deutscher
Geboren im 19. Jahrhundert
Gestorben im 20. Jahrhundert
Mann


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text:
Hinckley and Bosworth Borough Council
Works progressing on 2,500 home development approved six years ago say council
The borough council says the two projects are still in progress
Nick Dawson
And illustrative aerial perspective of the proposed plans for Barwell SUE.
Work is continuing behind the scenes on a 2,500 new home development outside Barwell that's been in the pipeline for almost six years.
The multi-million pound Barwell Sustainable Urban Extension (SUE) was first mooted over a decade ago, with plans to develop a 132.4 hectare site including 6.2 hectares of employment space, to the north and west of Barwell, over the course of more than 10 years.
The plans were approved in April 2013, subject to the satisfactory completion of a Section 106 deal.
Yet ground has yet to be cut on any part of the scheme.
Hinckley and Bosworth Borough Council said that works on both the Barwell and Earl Shilton SUEs "are still progressing".
Barwell SUE near Hinckley, Leicestershire. Taken from Stapleton Lane. 02/03/15
The Barwell SUE is expected to bring 6.2 hectares of employment space to the north and west of Barwell over the course of more than 10 years.
Proposals for the 132.4 hectare site include sports pitches, a pavilion building and changing rooms, areas of formal and informal open space and children's play areas.
The 'purple blocks' on Leicestershire council plan that show developers are looking to buy land near Burbage
There would also be landscaping, allotments and public realm works, pedestrian and cyclists connections and a so-called community hub made up of a primary school and a health centre, or alternatively a family pub and retail and commercial units.
With the long impasse of the Barwell SUE, progress has also been hampered on the Earl Shilton SUE, which would include 1,600 properties on a 200 acre site.
Birds-eye view of the proposed plans for Barwell SUE.
The Earl Shilton SUE is yet to reach the outline planning application stage despite years of talks stretching back as far as 2009.
The Earl Shilton SUE consortium (Barwood, Bloor Homes and Jelson Homes) previously claimed it is not viable for them to offer any affordable housing on the site.
Retro cafe and music bar is coming to site near Hinckley town centre
Council leader Mike Hall told The Hinckley Times in March 2018 that the consortium needed to make the scheme work or walk away.
The authority generally requests 20 per cent of any new development is offered as social housing either in conjunction with a housing association or through council rental.

redpajama_set_name: RedPajamaCommonCrawl


text:
\section{Introduction}\label{sec:intro}
Planet formation is not a 100\% efficient process and most, if not all, mature planetary systems contain a reservoir of comets and asteroids \citep[e.g.,][]{matthews2014}. When these bodies impact planets at high velocities (${\gtrsim}10\mathrm{~km/s}$), material can be ejected at velocities above the planetary escape velocity.  This debris can potentially end up on another planet; such an event explains how the SNC meteorites arrived from Mars \citep[e.g.,][]{gladman1996,worth2013}.   If life developed on the impacted planet, the exchanged material could harbor biological material or organisms that could inoculate the planet onto which it is accreted.  This process is referred to as litho-panspermia \citep{melosh1988,melosh2003}.

In our Solar System, transit times of impact ejecta between terrestrial planets are found to be $10^{6-7}\mathrm{~yr}$ in numerical simulations \citep[e.g.,][]{gladman1996,worth2013}, consistent with cosmic-ray exposure times reported for Martian meteorites found on Earth \citep{eugster2006}. Transit times may be much shorter in other planetary systems, where different orbital architectures result in very different dynamical evolution of ejected debris \citep{steffen2016}. The recently discovered TRAPPIST-1 system is particularly intriguing in this regard, as it consists of seven, nearly Earth-massed planets orbiting an M-type dwarf star. Three of those planets are believed to be within the habitable zone (HZ) and have rocky compositions \citep[e.g.,][]{gillon2016,gillon2017}. With orbital periods on order of days and orbital separations ${<}0.01\mathrm{~AU}$, the transport of material between these planets may be more rapid and efficient than in the Earth-Mars case. \citet{lingam2017} have argued, using an analytical model calibrated to our Solar System, that litho-panspermia could be 2 orders of magnitude faster in TRAPPIST-1 when compared to the Solar System.

In this Letter, we numerically investigate the efficiency and speed of potential litho-panspermia in the TRAPPIST-1 system. Specifically, we seek to quantify what fraction of material that is ejected from one of the HZ planets (e, f, or g) ends up on another planet, how long this material spends in space, and at what speeds it is accreted by another planet.

\begin{deluxetable}{ c  c c c c c c}[t]
\tabletypesize{\scriptsize}
\centering
\tablecaption{Planet properties used in our simulations.}
\tablewidth{0pt}
\tablehead{
\colhead{Planet} & \colhead{$a$}  & \colhead{$R$} & \colhead{$M$} & \colhead{$R_\mathrm{H}$} & \colhead{$v_\mathrm{esc}$} & \colhead{$v_\mathrm{K}$}\\
 & \colhead{$(\mathrm{AU})$}  & \colhead{$(R_\oplus)$} & \colhead{$(M_\oplus)$} & \colhead{$(R_\oplus)$} & \colhead{$(\mathrm{km/s})$} & \colhead{$(\mathrm{km/s})$}
}

\startdata
b& 0.011 & 1.09 & 0.85 & 5.5 & 9.9 & 80 \\
c& 0.015 & 1.06 & 1.38 & 8.8 & 13 & 68 \\
d& 0.021 & 0.77 & 0.41 & 8.4 & 8.2 & 58 \\
e& 0.028 & 0.92 & 0.62 & 13 & 9.2 & 50 \\
f& 0.037 & 1.04 & 0.68 & 17 & 9.0 & 44 \\
g& 0.045 & 1.13 & 1.34 & 26 & 12 & 40 \\
h& 0.063 & 0.76 & 0.40 & 25 & 8.1 & 34
\enddata
\tablecomments{Based on the TRAPPIST-1 system as described in \citet{gillon2017}. The Hill sphere radius is calculated as $R_\mathrm{H}=a(M/3M_\star)^{1/3}$, the escape velocity $v_\mathrm{esc}=\sqrt{2GM/R}$, and the Keplerian orbital velocity $v_\mathrm{K} = \sqrt{GM_\star/a}$.}
\label{tab:setup}
\end{deluxetable

\section{Simulation setup}\label{sec:setup}
We simulated the trajectories of impact ejecta from their moment of ejection until accretion onto a planet using the {\texttt{SyMBA}} $N$-body integrator\footnote{Part of the {\texttt{Swifter}} software package, available at \url{http://www.boulder.swri.edu/swifter/}}. This package accounts for the  gravitational interactions between massive bodies (planets and the star) and the gravitational interactions from (all) massive bodies onto test particles (ejecta), but neglects interactions among the test particles and other forces (e.g., radiation pressure, Poynting-Robertson drag). We use a time-step of 0.1 days (1/15th of the orbital period of TRAPPIST-1b), with {\texttt{SyMBA}} automatically switching to a smaller time-step during close encounters \citep{duncan1998,levison2004}.

The semi-major axes of the orbits of the TRAPPIST-1 planets are listed in Table \ref{tab:setup} along with their radii, masses, and Hill sphere radii. Because the eccentricities and inclinations of the TRAPPIST-1 planets are believed to be very small (\citet{gillon2017} constrain the eccentricities to be ${<}0.085$ and the mutual inclinations to be ${\lesssim}0.2^\circ$), we place the planets on circular and co-planar orbits at the start of our simulations. Over the course of the simulations, interactions between the planets raise the eccentricities of the planetary orbits to $e \lesssim10^{-2}$, consistent with the upper limits given by \citet{gillon2017}. In theory, for eccentric orbits, there will be differences in the trajectories of ejecta released at different times during the planet's orbit \citep[e.g.,][]{jackson2014}. Comparing aphelion and perihelion, the difference in heliocentric distance and orbital velocity $\Delta r/a \approx \Delta v / v_\mathrm{K} \approx2e$, so we do not expect significant variations for $e \lesssim10^{-2}$.

The starting positions of the planets (i.e., their initial true anomalies) are chosen at random\footnote{We ran multiple simulations with different starting positions and found no significant differences in the outcomes.}.  At $t=0$, the three planets that are most likely to be in the HZ (e, f, and g) isotropically eject material at a velocity $v_\mathrm{ej}$ that, in the absence of interactions with other massive bodies, allows them to reach infinity with a remaining velocity $\hat{v}_\infty \equiv v_\infty/v_\mathrm{esc}$. We will consider ejection velocities\footnote{The ejection velocity normal to the planet's surface can be related through the velocity at infinity by $v_\mathrm{ej} = (1+\hat{v}_\infty)v_\mathrm{esc}$.} that result in $0 \leq \hat{v}_\infty \leq 2$.

This range covers ejection that is so slow the material barely escapes the planet ($\hat{v}_\infty=0$), and high-velocity ejection of material that is launched from the surface at 3 times the planetary escape from the surface ($\hat{v}_\infty=2$). While material can be ejected at even higher velocities, we expect the majority of large, mass-dominating, and lightly-shocked ejecta to be just above $\hat{v}_\infty=0$ (see Section \ref{sec:implications}). Moreover, at $\hat{v}_\infty>2$, the ejection velocity will become comparable to the local Keplerian velocity, causing the ejected material to escape the TRAPPIST-1 system on a hyperbolic orbit \citep{jackson2014}.

To simulate the ejecta, $10^4$ mass-less test particles are released from each planet in the HZ at 0.1 planetary radii above the surface. Ejecta that reaches a heliocentric distance $r<5\times10^{-4}\mathrm{~AU}$ is assumed to be accreted by the primary, and bodies that reach $r>1\mathrm{~AU}$ are taken to be ejected from the system. The simulations are stopped after $10^4\mathrm{~yr}$ (${\sim}300{,}000$ orbits of planet g) because most material has been accreted by then (see Section \ref{sec:results}) and we are focusing on the fastest transport.

While there are considerable uncertainties in the planetary masses as derived from transit timing variations \citep{gillon2017}, it is beyond the scope of this study to address in detail the effects these uncertainties have on the results obtained in Section \ref{sec:results}. However, we are confident our main conclusions are robust because the important quantities scale with planet mass relatively weakly, e.g., $v_\mathrm{esc}\propto M^{1/2}$ and $R_\mathrm{H}\propto M^{1/3}$.

\begin{figure}[]
\centering
\includegraphics[clip=,width=.95\linewidth]{fig1a.pdf}\\
\includegraphics[clip=,width=.95\linewidth]{fig1b.pdf}\\
\includegraphics[clip=,width=.95\linewidth]{fig1c.pdf}
\caption{Examples of 3D trajectories (and 2D projections) ejecta take after being released from different planets, showing re-accretion onto the same planet (A), outward transport (B) and inward transport (C). Green and red markers show the location and trajectory of ejection and accretion.}
\label{fig:indiv}
\end{figure}

\begin{figure*}[t]
\centering
\includegraphics[clip=,width=.9\linewidth]{fig2.pdf}
\caption{Left to right: the fate of ejecta released from planets e, f, and g at different velocities (see text). Letters indicate accretion onto the primary (A) and the seven planets (b through h), X indicates ejection from the TRAPPIST-1 system, and `-' represents ejecta that is still in orbit after the simulated $10^4\mathrm{~yr}$. The blue shaded area corresponds roughly to the HZ.}
\label{fig:fateplot}
\end{figure*}

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

\subsection{Individual trajectories}
To illustrate the the possible scenarios, Fig. \ref{fig:indiv} shows three trajectories taken by particles ejected from planets e, f, and g at different velocities. In Fig. \ref{fig:indiv}A, material ejected from planet e at a velocity equal to the escape velocity ($\hat{v}_\infty=0$) is re-accreted onto the same planet within several years. In Fig. \ref{fig:indiv}B, a particle is ejected at a higher velocity from planet f, and eventually ends up on planet g after ${\sim}80\mathrm{~yr}$. Finally, in Fig. \ref{fig:indiv}C, ejecta released at a high velocity from planet g is eventually accreted by planet d. Generally, higher ejection velocities result in more variation in the eccentricity and inclination of ejecta orbits as the `kick' in velocity these bodies get upon release increases relative to the local Keplerian velocity \citep{jackson2014}.

\subsection{Fate of ejected material}
In Fig. \ref{fig:fateplot}, we plot the outcomes of $10^4$ individual ejecta trajectories for material ejected from planets e, f, and g, at different ejection velocities. Letters indicate (re-)accretion onto the planets and the primary, and the two right-most columns include material that was still in orbit at the end of the simulation or that was ejected from the TRAPPIST-1 system.

Focusing first on relatively slow ejection ($\hat{v}_\infty=0$), we find that re-accretion onto the same planet is the dominant outcome. Nonetheless, between ${\sim}45{-}60\%$ of the ejected bodies end up somewhere else, even at these relatively low ejection velocities. In particular, material exchange within the HZ is relatively common (especially between f and g).

At somewhat higher ejection speeds, the distributions in Fig. \ref{fig:fateplot} become broader, with less material being re-accreted by the source planet. In fact, for $\hat{v}_\infty=0.5$, the dominant outcome for material released by planet f (middle panel) is accretion by planet g. Accretion onto b, c, and d also becomes more common, as ejecta that is released at higher velocities is more likely to reach highly-eccentric (but bound) orbits that cross the inner parts of the system (see Fig. \ref{fig:indiv}). Qualitatively similar behavior is seen for ejecta originating from Mars and Earth in the Solar System \citep[][Fig. 1]{melosh2003}.

Lastly, for $\hat{v}_\infty=2$, ejection from the TRAPPIST-1 system is the dominant outcome, with almost $50\%$ of material released from planet g at these velocities leaving the system on very short timescales. This (virtually instantaneous) ejection from the planetary system occurs when the sum of the ejection velocity and the Keplerian velocity exceeds $\sqrt{2}v_\mathrm{K}$, in which case the test particle is released on an unbound orbit \citep{jackson2014}.

\begin{figure*}[t]
\centering
\includegraphics[clip=,width=.95\linewidth]{fig3.pdf}
\caption{Cumulative accretion histories over time. The ejection velocity increases from left to right, and the three rows correspond to ejection by planets e (top), f (middle), and g (bottom). Re-accretion onto the planet of origin is shown by the thickest line, the dashed curve shows complete ejection from the system, and the dotted line shows the sum of all contributions. At the end of the simulations, ${\lesssim}10\%$ of the material released at $t=0$ is still in orbit (see Fig. \ref{fig:fateplot}).}
\label{fig:cumuplot}
\end{figure*}

\subsection{Time spent `en route'}
In Fig. \ref{fig:cumuplot}, we show the cumulative accretion histories for all bodies in the system for the 9 simulations shown in Fig. \ref{fig:fateplot}. In all low-velocity cases (left column), $10\%$ of the ejected mass returns `home' within ${\sim}1\mathrm{~yr}$. Transport to other planets however is also remarkably fast. Focusing on the HZ planets, the routes\footnote{In this notation f-g should be read as `from f to g'.} f-g, g-f,  f-e, and g-e stand out as being particularly fast for $\hat{v}_\infty=0$, transferring between $1{-}10\%$ of ejecta within $100\mathrm{~yr}$. When $\hat{v}_\infty$ increased to $0.5$ and $2.0$, both re-accretion onto the planet of origin and transport to other planets become significantly slower and much less material is (re-)accreted in the first $100\mathrm{~yr}$. It is also interesting to look at accretion onto b and c, the inner two planets. In all three low-velocity cases, these two bodies accrete least of the material, and do so relatively late. At the highest ejection velocities however, planets b or c dominate the accretion, even out-pacing re-accretion onto the body of origin.

\subsection{Impact velocities}
For organisms to survive re-entry, (relatively) low impact velocities onto the accreting planet are required. Using the final approach of to-be-accreted ejecta (see Fig. \ref{fig:indiv}) we can calculate the (approximate) impact velocity of material. Fig. \ref{fig:vimp} shows the distribution of impact speeds of material ejected from planet e at $\hat{v}_\infty=0$ relative to planetary escape and orbital velocities. For transport within the HZ, the most common impact velocities are $10{-}20\mathrm{~km/s}$, within a factor of $2$ of the target escape velocity (Table \ref{tab:setup}). This reflects the fact that most ejecta was released on almost circular and co-planar orbits (Fig. \ref{fig:indiv}A), i.e., the ejection velocity was small compared to the local Keplerian velocity. Reaching b or c requires a more eccentric orbit, and therefore usually results in a considerable contribution of the orbital velocity to $v_\mathrm{imp}$. For increasing $\hat{v}_\infty$, the impact velocity distribution shift to higher velocities, with average impact velocities for transport within the HZ reaching $\langle v_\mathrm{imp} \rangle \approx40\mathrm{~km/s}$ for $\hat{v}_\infty=2$. Note that the impact velocities shown in Fig. \ref{fig:vimp} correspond to the ejecta's final approach to the targeted planet and do not take in to account potential slowing down of material by the planet's atmosphere.

\begin{figure}[t]
\centering
\includegraphics[clip=,width=.9\linewidth]{fig4.pdf}
\caption{Normalized distribution of impact velocities onto different planets for ejecta released from planet e at $\hat{v}_\infty=0$. The shaded area indicates the range of planetary escape velocities and the dotted vertical lines represent $v_\mathrm{K}$ for planets b through h.}
\label{fig:vimp}
\end{figure}

\section{Implications for (litho-)panspermia}\label{sec:implications}
Comparing the results of Fig. \ref{fig:cumuplot} to typical transfer timescales of $10^{6-7}\mathrm{~yr}$ in the Solar System \citep{gladman1996,worth2013} reveals just how well the proximity of the TRAPPIST-1 planets to each other facilitates material exchange. If the probability of surviving inter-planetary transfer is inversely proportional to the duration of the journey \citep[e.g.,][]{lingam2017}, this indicates the efficiency of litho-panspermia could be $4{-}5$ orders of magnitude more efficient. In addition, the radiation environment (at X-ray and UV wavelengths) around M-stars is expected to be harsh and highly variable \citep{scalo2007}, so short transit times might well be a prerequisite for successful litho-panspermia.

Because the size-/velocity-frequency distribution of the impactor population bombarding the habitable zone of Trappist is unknown, it is impossible to translate our estimates of ejecta flux (Fig. \ref{fig:cumuplot}) into mass flux (kg/yr) of life bearing rock mass. However, using the inner Solar System as a template, we expect the mean impact velocities on TRAPPIST-1 e-g are ${\sim}2$ times the escape velocities of those planets, making it likely that some amount of lightly shocked \citep{melosh1985,johnson2014}, unsterilized \citep[e.g.,][]{mastrapa2001,stoffler2007} material will be transferred between planets every time a large enough impact occurs. Moreover, because both the cumulative amount of mass ejected per impact $M({>} v_\mathrm{ej}) \propto v_\mathrm{ej}^{-4}$ \citep{shuvalov2011,johnson2014} and the mean size of ejected fragments $\langle \ell_\mathrm{frag} \rangle \propto v_\mathrm{ej}^{-2/3}$ \citep{melosh1988} generally decrease with ejection velocity, we expect that material ejected just above escape velocity (i.e., for $\hat{v}_\infty$ close to or just above 0) will constitute most of the mass transferred between planets, and will especially dominate the component of transferred mass in large enough fragments that life can survive both irradiation during transfer and heating during re-entry.

\section{Summary}\label{sec:summary}
We have performed $N$-body simulations of the TRAPPIST-1 system to study the fate of impact ejecta released by the three planets that are most likely to be in the habitable zone (e.g., Fig. \ref{fig:indiv}). Our main findings are:

\begin{enumerate}

\item{Material exchange between planets in the TRAPPIST-1 system is very efficient for ejection velocities close to and just above the planetary escape velocity, with $20{-}40\%$ of material ejected at these velocities eventually accreting onto another HZ planet (Fig. \ref{fig:fateplot}).}

\item{Comparing transport timescales between e, f, and g to those of the Mars-Earth route in our own Solar System, we conclude that transferring solids between habitable zone planets in TRAPPIST-1 is up to $4{-}5$ orders of magnitude faster (Fig. \ref{fig:cumuplot}).}

\item{Transport between planets f and g stands out as being particularly fast and effective, with some material being transferred within $10\mathrm{~yr}$ of being released (Fig \ref{fig:cumuplot}).}

\item{The velocities with which transferred material impacts other HZ planets are low ($10{-}20\mathrm{~km/s}$) for material ejected just above escape velocity (Fig. \ref{fig:vimp}); only slightly above the accreting planet's $v_\mathrm{esc}$.}

\end{enumerate}

\noindent As we are poised to learn more about the properties of these alien worlds \citep[e.g.,][]{barstow2016,dewit2016}, our results suggest that, as is the case in the Solar System, we should consider the possibility of frequent material exchange between (adjacent) planets in the TRAPPIST-1 system, life-bearing or sterile.

\acknowledgments
The authors thank A. Loeb and M. Lingam for fruitful discussions and the anonymous reviewer for constructive feedback that helped improve the manuscript. This material is based upon work supported by the National Aeronautics and Space Administration under Agreement No. NNX15AD94G for the program ``Earths in Other Solar Systems." The results reported herein benefitted from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate.

redpajama_set_name: RedPajamaArXiv


The following article describes required steps when configuring Rational Lifecycle Engineering Manager (RELM) in federated topology architecture. For this article to be easily understood familiarity with RELM, System & Software Engineering solution (SSE), Jazz and Open Services for Lifecycle Collaboration (OSLC) technologies is assumed.
To complete RELM cross tooling configuration it is required to add data source providers to RELM index engine that is Lifecycle Query Engine (LQE). Online documentation is available for understanding how to complete this task. For more details please refer to Register applications as Data Source Providers: single JTS, and Register applications as Data Source Providers: multiple JTS server .
In this article you will find additional, not documented details discovered and collected while completing such configuration in federated topology environment.
SSE solution is a collection of tools connected using RESTfull and OSLC APIs. Deployment architecture of SSE tools can be varied according to various factors including ease of installation, performance consideration, security constraints and more. In federated topology each tool is installed on a dedicated machine (physical or virtual) along with web server and dedicated Jazz Team Server (JTS) application foundation.
TRS internal consumer license is required for each application that is also Data Source Provider. However, such license is not provided out of the box. How to get it?
As suggested in this article, use jts_user as internal functional user when creating consumer (inbound) keys.
Creating OSLC friendship is done in the administration section of each data source provider application. Due to different internal architecture, for RDM application you have to create friendship in the administration section of the underlying JTS application.


text:
Membership Donation
Honor/Memory Donation
Family Recognition
Gun Violence Prevention
HIV Advocacy
Trans Action
Voter Mobilization
Council of Leaders
Statewide Sponsors
Nikole Parker, TransAction Florida Project Coordinator
Nikole Parker is the TransAction Florida Project Coordinator, assisting with Equality Florida's statewide Transgender Inclusion Initiative. She also currently works for the onePULSE Foundation as the Stakeholder & Community Relations Manager. Nikole has sat on various non-profit boards within the community, including the LGBT+ Center Board of Directors, the Orlando United Assistance Center Advisory Board, TransAction Advisory Council, Spektrum Health Board of Directors and Peer Support Space Board of Directors. In addition to her work with the onePULSE Foundation, Nikole co-leads the work of the Orlando Trans Collective, a collaborative group of transgender and gender non-conforming leaders of color who focus on community building and advocacy efforts for the Central Florida transgender community. In 2018, Nikole was honored with the Humanitarian of the Year award by the Miss Glamorous Pageant. Nikole was also was recognized as one of Watermark's Most Remarkable People of 2018 for her work with the onePULSE Foundation and her ongoing advocacy and empowerment of the transgender community. In 2019, Nikole was recognized by Congressman Darren Soto for LGBT+ Pride Month and her biography was read into the Congressional Record. She hopes to encourage open dialogue on transgender issues and educate individuals from the community on healthy and safe ways to undergo a transition, finding self-care practices and providing resources so black market hormones and unsafe lifestyles can be avoided.
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I would like to take this opportunity to remind county residents that with the coming of spring we also have the increased chances for tornado's and severe thunderstorms and to provide some information to help keep everyone a little safer.
When Brown County is placed in a "TORNADO WARNING" by the National Weather Service OR when a trained storm spotter identifies tornadic activity, the Brown County Sheriff's Office will sound the sirens in Hiawatha and Powhattan–the other areas of the county will be notified as quickly as possible and suggested they do likewise. This policy will allow dispatch the authority to warn residents ASAP and save valuable time. Since 1986 all or a portion of Brown County has been placed under a tornado warning less than 2 times each year as an average. My main concern is and always will be the safety of Brown County residents.
I have talked with several different meteorologists and have been informed that when atmospheric conditions are favorable for severe thunderstorms, a severe thunderstorm may move into or develop over any part of the county and tornadic thunderstorms my not be confined to just one part of the county. Not one of the meteorologists could assure me that if a tornado warning was issued in the southern part of Brown County, tornado activity would not affect other parts of the county. So in order to give residents as much time as possible to take cover, I have implemented the tornado policy to take care of all Brown County as a whole.
*Tornado's can form very rapidly with little or no warning at all.
*Super-cell thunderstorms can produce large violent tornado's and usually residents will have time to take cover but not always.
*Rain wrapped tornado's may NOT be visible from the ground and are very difficult to spot at night.
*Tornado's can change directions without warning.
Outdoor tornado sirens are meant to be a warning device for people who are outdoors, so if you are in your home when the tornado sirens are activated, you may not be able to hear them.
We are encouraging everyone in the county to have multiple means of getting severe weather watch and warning notifications, The public is encouraged to own a battery operated ALL HAZARDS NOAA Weather Radio which broadcasts severe weather information directly from the National Weather Service. If commercial power is lost due to a storm, batteries will allow the radio to be activated and wake you up in the middle of the night. In addition, we also urge residents to listen to local TV and radio media for the latest on severe weather coverage. Calling trees are also a good idea so friends and relatives can contact each other to make sure they are all aware of severe weather approaching. Residents also need to know where to take cover in the event a tornado is spotted in our area. Families need to practice where they will go to in order to stay safe. Also look out after your elderly neighbors who live alone or those with medical or health conditions that may need extra assistance. This is what it's all about, people helping each other.
Several years ago I took the opportunity to speak with most of the mayors in Brown County and asked them where a storm shelter would located be in their areas in case the tornado sirens sounded and they needed to take cover. Some did not have and plans in place and took the initiative to do so and identified churches or other buildings in their community for the safety of their citizens. We still encourage everyone to keep doing this. One of my main concerns is the safety of those not knowing what to do or where to go should we have a tornado in our county.
We also offer the basement of the Brown County Sheriffs Office as a storm shelter for those in need. Over the past several years we have had quite a number of citizens that have taken refuge in our facility and will continue to offer this as an option for those seeking shelter during severe thunderstorms, tornado's, blizzard conditions etc.
I am very proud to have the opportunity to work with all of the emergency responders we have in Brown County. These dedicated men and women respond at all hours of the night and day to many different emergencies in our county and work together to help provide us with a safer place to live. We all owe them a big THANK YOU!!!.
If anyone has any questions or concerns, please come by or contact me at the Sheriffs office.


Benchtop instrument for testing small and medium sized workpieces. Also known as Profile Projectors, Shadowgraphs or Optical Comparators.
Vertical, rotatable crosshair lines screen.
Easy-to-operate coordinate measuring stage with coarse and fine adjustment.
Direct and clear, easy-to-read XY digital display at eye level ensures safe and error-free measurement.
Halogen transmitted and incident illumination are integrated into the housing.
Provided with a protractor as a standard, switchable for sexagesimal degree or decimal degree reading. Resolution: 1' or 0.01'.
XY position and cursor angle display provided.
Resolution - 0.001mm / .0001" .
Function ZERO setting +/- direction, RS-232C interface.
Accessories Include: 10X projection lens, Measuring stage for PJ010F-200, 3 x halogen lamp (24 V / 150 W), Protective hood, Light shield, Half-silvered mirror for 10 X projective lens, Half silvered mirror for 20X projective lens.


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Below is a listing of 20" - 28" LCD and LED TVs that we feel comfortable in recommending for 2019/2020. Many of these TVs have been reviewed either this year or the determination made from last years review of the previous model. In our testing we look for consistency in a brand and model series in many categories such as picture quality, appearance and the presence or not of other features such as internet connectivity.


We never want to define ourselves in a way that puts us in a corner, ever-evolving and free to experiment with our food. If there's one area of our restaurant where we would say is akin to our vagabond soul it would be with Mexcal. Unlike tequila, Mezcal has is be made 100% from Agave. It's considered to be a 'mestizo' (man of mixed race) beverage. When the Spanish brought their knowledge of distillation, they discovered that pulque distilled produced a sweeter beverage and Mezcal was born. Traditional Mezcal is produced in small, artisanal batches. We travel to Mexico to bring you special finds, serving it neat in jicaras or xicalli in Nahuatl which have been used for thousands of years in Mexico.
Our respect for Mezcal is akin to the respect you have for 'Padrinos.' Mezcal is Rojo Gusano's godfather in many ways, showing us the way by its' history. It embraces its hybrid history and creating its own identity with unmistakable Mexican flavor and unexpected variety and depth. Served traditionally, our collection of Mezcal is meant to be savored and sipped, brought to you from best and most innovative distilleries in Mexico. Our cocktails seek to honor that spirit, we insist on showcasing the Mezcal in each creation all the while transforming the nature of each with flavors that have inspired us from all over the world.
We travel for Mezcal, explore some of our latest finds.
Phenomenal is the best word to describe Rojo Gusano, everything on the menu is delicious so you cant go wrong with whatever you order and the service is great. My favorite are the chorizo tacos and empanadas (all of them). As far as drinks I love the Mezcaladas and make sure to take a few shots of mezcal as well, ask the bartender, they will give you great mezcal suggestions.
It's a beachside taqueria marooned in Albany Park with beer-braised pork shank, spicy pumpkin seed guacamole, and no shortage of mezcal.


text:
Investigation grinds to halt as implicated parties point fingers
By Corruption Watch 01 Jun 2018, 12:19
By Kwazi Dlamini
When Corruption Watch undertakes an investigation, we do so because we deem the case to be in the public interest, and one that could have a significant impact. However, in cases when, for instance, access to important information is withheld, our chances of successfully resolving the matter are diminished.
In an e-mail sent to us in April 2018, the Gauteng Department of Education (GDE) denied any wrongdoing by any of the individuals implicated in financial irregularities at Cyrildene Primary School. The irregularities were uncovered by the school governing body (SGB) when they took up duties in 2015, and were pursued by the whistle-blower, an SGB member. After his findings on the mismanagement of funds were shunned by the school, the whistle-blower decided to report the matter to Corruption Watch for further investigation.
The report submitted to Corruption Watch alleged numerous irregularities within Cyrildene Primary School in Johannesburg – including irregular accounting processes, the school operating four bank accounts which is a clear violation of section 37(3) of the South African Schools Act, and unauthorised payments made to staff members, which violates section 38A of the Act. The report also revealed that an amount of R1.7-million was unaccounted for, and ledger accounts were missing from the school's 2014 annual financial statements.
All the above irregularities were outlined in the internal audit report conducted by the Cyrildene SGB. The GDE then hired an external firm – Outsourced Risk and Compliance Assessment (ORCA) – to conduct a forensic investigation into the matter.
Investigation results differ – or do they?
In its e-mail to us, the GDE said the forensic report conducted by ORCA was attended to by relevant stakeholders including the whistle-blower, who was not satisfied with the outcome. In the midst of denying all the allegations in the internal audit report, however, the GDE did acknowledge that the school had four bank accounts and was advised by the department to cut these down to just one account.
According to the GDE's e-mail, the clearing investigation conducted by ORCA on behalf of the department was not aligned to the view of the internal audit report but it was pursued after a formal complaint was lodged with the department by the same whistle-blower. The investigators took into consideration and engaged with the audit report during the process. Corruption Watch requested a copy of the ORCA forensic report from William Makgabo of the GDE, in terms of the Promotion of Access to Information Act (Paia). After 30 days had lapsed without hearing from the GDE, we deemed such lack of response a refusal in terms of Section 27 of Paia.
Hence we were unable to determine whether the ORCA report and the internal audit report had different findings.
The correlation between the two investigations was one of the questions we asked of the GDE:
Why has the GDE continued to withhold the forensic report?
What were the findings by ORCA in relation to the irregularities raised in the internal audit report?
Were any individuals implicated of wrongdoing in the forensic report?
If any individuals were implicated of wrongdoing, what remedial action has been recommended?
For the most part, these questions were not answered. The GDE, in its e-mail, claimed the reason for withholding the ORCA forensic report was because it had been already discussed by all the relevant stakeholders.
The department also revealed that the implicating report was later withdrawn in writing after the whistle-blower was requested to provide evidence supporting his allegations. "The whistle-blower was also extensively engaged and was requested to provide evidence supporting his allegations," said the GDE in its e-mail response.
The report conducted by ORCA on behalf of the department also found that the allegations of missing R1.7-million were unfounded; in the wake of this report the whistle-blower still upheld his findings noted in the internal audit report and said that since the GDE failed to provide any document of evidence to support these ORCA findings, this means they are hiding something.
"The whistleblower did not accept the outcome of the investigation by the Department and he persisted with his allegations despite that he was unable to provide evidence of such. He appeared disgruntled and motivated by his private interests at the school," replied the GDE, via e-mail.
The case is now at a stalemate, because we do not have the information we need in order to reach a conclusion. However, we decide to publish cases like these in the hopes that parties concerned will reconsider their reluctance to co-operate.
Tags: Corruption Watch, school governing body, SGB, South Africa, whistle-blower, schools corruption, Cyrildene Primary School
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