text:
Q: Unable to access a file created in a web application This is my code which is used in a wcf service. It successfully generates the PDF, but after generating the document, the folder in which the PDF is generated gives the error: "access is denied"
The PDF is closed for the website, but for the continuous web service it is not closed.
string r = builder.ToString();
string pdfname = Fuhre + "_" + ProtokolType + "_" + GeraeteNr + "_" + r;

PdfWriter.GetInstance(document, new FileStream(@"C:\inetpub\wwwroot\protokoll_pdfs\"+pdfname+".pdf",FileMode.Create));
document.Open();
WebClient wc = new WebClient();
string htmlText = html;
//Response.Write(htmlText);
List<IElement> htmlarraylist = HTMLWorker.ParseToList(new StringReader(htmlText), null);
for (int k = 0; k < htmlarraylist.Count; k++)
{
   document.Add((IElement)htmlarraylist[k]);
}

pdflink1 = pdfname + ".pdf";
htmlpdflink =""+pdflink1;
document.Close();

A: You need to be careful to dispose of everything.
    using(var filesStream = new FileStream())
    {
        using(PdfWriter wri = PdfWriter.GetInstance(doc, fileStream))
        {
    ...
        }
    }

A: There are a few other objects (Stream, Document) you may want to close. A sample of how to perform the operation is shown below.
FileStream stream = new FileStream(filePath, FileMode.CreateNew);
Document doc = new Document(PageSize.A4, 24, 24, 24, 24);
PdfWriter writer = PdfWriter.GetInstance(doc, stream);

doc.Open();

//PDF writing operations here

writer.Flush();
doc.Close();
writer.Close();
stream.Close();

A: You want to serve a file to a browser and/or you want to save the file on disk.
In that case, you would benefit from creating the file in memory and then send the bytes to the browser as well as to a file on disk. This is explained in the answer to the following question: Pdf file not loading properly created by the servlet
The answer mentioned above is written in Java, so you'll have to adapt it.
You can do so by looking at other examples. For instance: Create PDF in memory instead of physical file
byte[] pdfBytes;
using(var mem = new MemoryStream())
{
    using(PdfWriter wri = PdfWriter.GetInstance(doc, mem))
    {
        doc.Open();//Open Document to write
        Paragraph paragraph = new Paragraph("This is my first line using Paragraph.");
        Phrase pharse = new Phrase("This is my second line using Pharse.");
        Chunk chunk = new Chunk(" This is my third line using Chunk.");
    doc.Add(paragraph);

    doc.Add(pharse);

    doc.Add(chunk);
}
pdfBytes = mem.ToArray();

}
Now you can write the pdfBytes to the Response object in your web application:
private void ShowPdf(byte[] strS)
{
    Response.ClearContent();
    Response.ClearHeaders();
    Response.ContentType = "application/pdf";
    Response.AddHeader("Content-Disposition", "attachment; filename=" + DateTime.Now);

    Response.BinaryWrite(strS);
    Response.End();
    Response.Flush();
    Response.Clear();
}

And you can reuse the bytes to write them to a File: Can a Byte[] Array be written to a file in C#?
File.WriteAllBytes(string path, byte[] bytes)

If the problem persist, then you know that it isn't caused by iTextSharp, because iTextSharp merely produces the bytes.

A: In addition to what everyone else said, I strongly recommend you break each process into multiple sections that don't interact and aren't even aware of each other. Then test each section independently as much as possible. For instance:
private void makePDF( filePath )
{
    //Create the PDF
}

private void main()
{
    //Make the PDF
    makePDF( "test.pdf" );

    //If this line fails then your makePDF code has an open handle
    File.Delete( "test.pdf" );
}

Then continue:
private void makePDF( filePath )
{
    //Create the PDF
}

private void emailPDF( filePath )
{
    //Email the PDF
}

private void main()
{
    //Make the PDF
    makePDF( "test.pdf" );
    emailPDF( "test.pdf" );

    //If this line fails now then your emailPDF code has an open handle
    File.Delete( "test.pdf" );
}

The important part if that you don't try 500 things all at once because that leads to "something is locking my file but I don't know what".


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text:
Postscripts From Quotidia Episode 1
May 21 2022 June 7, 2022
Postscripts From Quotidia Episode 1 Let Them Not Fade Away, Days Like This, The Hill
Welcome to Letters From Quotidia Postscripts Episode 1– a podcast by Quentin Bega for listeners who enjoyed that Irish phenomenon- the crack! in the 200 Letters and Postcards From Quotidia published between 11 January 2021 and 8 May 2022- Quotidia remains that space, that place, where ordinary people lead ordinary lives. But where, from time to time, they encounter the extraordinary.
So, what is a postscript? Well, my trusty internet dictionary tells me that it is 1) an additional remark at the end of a letter, for example, he added a postscript "Leaving tomorrow." Or, 2) an afterthought; that is, an extra piece of information about an event that is added after it has happened: for example, "as a postscript to this, Paul did finally marry". …and, of course, we wish them well! One or both of these definitions will apply to each the Postscripts. As to how many there will be- I don't know, but probably more than a few. As to how long each will be- I can't be sure but each one will, no doubt, be of between 15-25 minutes duration- give or take.
But why? I hear some cry. How much time do you have? I reply. Short answer is what I had to say when I set up my website on WordPress quite a while back: Quentin Bega was born in the middle of the last century, and then stumbled into the present one with something more to say. If you chance to visit Quotidia, a customs official, dressed in motley, will say to you: "Welcome to Quotidia- you don't need a passport to get in here… but if you have one, we will make sure your visa is stamped 'entry always permitted'".
One of the wonderful things about the writing game, is that you can, should you so choose, re-visit what you have previously produced, whether to amend, to add, to frankly contradict, or just generally blather on. Unlike life which remorselessly follows time's arrow- with no going back! So, this postscript is attached to Letters From Quotidia Episode 2: Let Them Not Fade Away.
I will use that old rhyme for newlyweds Something old, something new, something borrowed, something blue as a template for the Postscripts. The something old component will be a reprise of a song and/or verse extract from the original Letter. The something new will be an original song composition as well, obviously, as the new prose component of the Postscript. Something borrowed will comprise a cover of a song and/or verse borrowed from the great and the good. Something blue will be the predominant hue of the Postscripts.
As my wife reminds me: from our teenage years she was and is personified by the sunny vibe surrounding the song Build Me Up Buttercup by The Foundations whereas I was and am personified by the gloomier tones of Born Under a Bad Sign by Albert King. I presented an acoustic demo in the trailer to this postscript a while back but here it is as the something old component: [insert song]
I remember with fondness letters I exchanged over many years with my sister-in-law, Dympna before she died. We were great friends. She was ten years my senior, but we formed an immediate connection when we first met and when I was sixteen years old, we often shared a surreptitious cigarette in my mother's kitchen. The song you just heard describes those times. When, with my girlfriend, now wife, I visited Dympna and my brother Jim, a veterinarian in their home in County Cork in subsequent years we always had a great time listening to music, drinking Sherry from the wood, and playing poker.
After we moved to Australia in 1972, the correspondence struck up, Dympna writing on whatever spare paper surfaces that were to hand, be it quotes for drugs for ailing cows or sundry sheets of paper passing her way that had a blank surface. Her wonderfully parochial and incisive insights into matters of common interest to us both reminds me powerfully of the American poet I referenced in my second letter from Quotidia: Edgar Lee Masters, an American poet writing in the late 19th-early 20th Century.
Here is his poem, The Hill Where are Elmer, Herman, Bert, Tom and Charley,/The weak of will, the strong of arm, the clown, the boozer, the fighter?/All, all are sleeping on the hill./One passed in a fever,/One was burned in a mine,/One was killed in a brawl,/One died in a jail,/One fell from a bridge toiling for children and wife—/All, all are sleeping, sleeping, sleeping on the hill./ Where are Ella, Kate, Mag, Lizzie and Edith,/The tender heart, the simple soul, the loud, the proud, the happy one?—/All, all are sleeping on the hill./One died in shameful child-birth,/One of a thwarted love,/One at the hands of a brute in a brothel,/One of a broken pride, in the search for heart's desire;/One after life in far-away London and Paris/Was brought to her little space by Ella and Kate and Mag—All, all are sleeping, sleeping, sleeping on the hill./ Where are Uncle Isaac and Aunt Emily,/And old Towny Kincaid and Sevigne Houghton,/And Major Walker who had talked/With venerable men of the revolution? —All, all are sleeping on the hill.//They brought them dead sons from the war,/And daughters whom life had crushed,/And their children fatherless, crying —/All, all are sleeping, sleeping, sleeping on the hill./ I identified with Fiddler Jones when first I wrote episode 2 of Letters From Quotidia. I find that, now, years later, that identification is even stronger! And he gets pride of place, here in the final stanza of The Hill Where is Old Fiddler Jones/Who played with life all his ninety years,/Braving the sleet with bared breast,/Drinking, rioting, thinking neither of wife nor kin,/Nor gold, nor love, nor heaven?/Lo! he babbles of the fish-frys of long ago,/Of the horse-races of long ago at Clary's Grove,/Of what Abe Lincoln said/One time at Springfield.//
That this literary work is still of relevance, may I cite the following: On March 13, 2021, 'Spoon River Anthology' was presented as online verse reading by the Oxford University Dramatic Society. Wow! Good on them- I wish I could have heard that. I referenced, also, Van Morrison in the song Let Them Not Fade Away: he was the singer in "that Belfast band, Them" Here comes the something borrowed, my cover of his song- Days Like This. [insert song]
You know, the older you get the more gaps you perceive in your life. I have listened to Van the Man since the sixties and gone to see him sing jazz standards in Belfast in the 80s. I've also purchased vinyl records and CDs over the years, not to mention streaming lots of his songs- yet this is the first of his songs I have ever sung! Go figure. Way back when I started these podcasts, I queried how different was I from Procrustes, the monster of Greek legend, who fitted travellers to a bed where he cut off limbs or stretched to agonising death those who did not precisely fit the bed he had arranged for them. I asked then: Are not all artists Procrustes? Here am I, shaping a journalistic narrative around a series of songs by selecting and editing bits and pieces from the world of letters. But, unlike the original Procrustes, I hope that any idea for a song that is passing by survives the smith's hammer of my imagination as I struggle to shape it into something pleasing. So, I said then. And now, here I am again, chopping and stretching a story to fit my newest narrative bed. Am I a monster, or what?
I have to tell you: the pressure of composition makes me a rather sad monster, indeed. The something new component remains to be, at the time of writing this section of the postscript- actualised- is this really a word? I set myself a strict-ish regime of reading poetry for inspiration, especially from Edgar Lee Masters' Spoon River Anthology. After several days enjoyable but wearisome toil, I came up with a song that claims as its inspiration the poem by Edgar Lee Masters I recited earlier- The Hill. This completes the triad of components that comprise the Postscripts- it is something new.
So, you may judge for yourself- is this a truly inspired composition or is it just some Band-in-a-Box boilerplate I put together with the help of an Artificial Intelligence bot that I purchased from the dark web to boost my numbers in the relentless quest for clicks and comments and commendations? As always, you will be the judge. Here is The Hill. [insert song]
Technical Stuff: Microphone- Shure SM58; (for the podcast spoken content) Audio Technica AT 2020 front-facing with pop filter); Apogee 76K also used for songs and spoken text.
For recording and mixing down: 64-bit N-Track Studio 9 Extended used; Rubix 22 also used for mixing of microphone(s) and instruments. I use the Band in a Box/RealBand 2022 combo for music composition.

redpajama_set_name: RedPajamaCommonCrawl


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*Controlled test; not actual fire conditions.
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Send order list (model number, sizes, and quantity) to us, we will do invoice for you to check and pay.


Women have been writing plays forever, haven't we?
So we can't help but feel frustrated that even though we buy, by far, the largest majority of theatre tickets out there, we are still largely underrepresented in the other side of the curtains.
Male playwrights write 37% of parts for women….
Wouldn't be great if we could arrive at 50/50… and for female playwriting and casting as well?
Let's imagine a world where telling stories for and about women is not a politically-charged act.
Where female lead characters do not need to be defined as 'strong women'.
Where what we see and love on stage is true to real-life and shows us how we are.
The plays listed below are all written and performed by women.
Some are quite established, but most are still in the early stages of their journey. They are all great work, all getting great audience or press reviews.
And especially, they strive to be honest, interesting, inspiring representations of women on stage.
They will all be at Brighton Fringe this May 2018.
As women, they have less help to get their shows produced, less access to funding, often less confidence, and yet here we are, creating great theatre … let's choose them?
Also, if you're coming to Brighton Fringe this year and want to see great shows, click here to download or '10 Must See Shows at Brighton Fringe Guide'.
'There's two rules: first, the person you choose must be dead. And second, you have to be dressed up to get in.' It's Thursday night in the Prince Arthur and their latest theme night is in full swing. Landlady Liz is run off her feet, whilst husband Barry struggles to get into his new costume. Elsewhere in London, a young woman from Edinburgh steps off a train, determined to make her dreams a reality. Fast-paced and irreverent, 'Marie' is a darkly comic new play inspired by the life of Mary Queen of Scots, but given a distinctly modern twist.
Like money? You'll love this show. Self-professed business guru Manyi visits from China to share top insights for a prosperous and powerful life. Come laugh, play, ponder and power up!
"Angela Yeoh is a powerhouse of charm and sensitivity… mesmerizing and amazingly clever… highly recommended to lift your spirits" **** (Adelaide Theatre Guide).
Going to Brighton Fringe 2018?
Want to make the of the Brighton Fringe this May, but confused about all the shows on offer? Download our free '10 Must-See Shows at Brighton Fringe Guide' , save time and plan a relaxing and exciting fringe with the best-reviewed productions hitting town this year!


text:
\section{Introduction} \label{sec:intro}
Galaxy cluster collision shocks occur when two galaxy clusters collide. These shocks are characterized by a relatively low sonic Mach number ($\, M_{\rm s}\,\sim\,1-4$) and an Alfv{\'e}nic Mach number ($\, M_{\rm A}$) of approximately an order of magnitude higher, leading to a plasma-$\beta$ (the ratio of thermal to magnetic energy) of approximately 100.
The nature of these shocks has been studied extensively through cosmological hydrodynamical simulations \citep{ Miniatietal:2000,Ryuetal:2003,Pfrommeretal:2006,Kangetal:2007,Skillmanetal:2008,Hoeftetal:2008,Vazzaetal:2009, Hongetal:2014,SchaalVolker:2015,Hongetal:2015}, but whether such shocks are capable of accelerating particles to relativistic speeds, thereby contributing to the cosmic ray (CR) spectrum, remains an open question.

Although there are indications for \emph{electron} acceleration in merging clusters \citep{vanWeerenetal:2010}, so far, studies of these shocks \citep[e.g.][]{PinzkePfrommer:2010,ZandanelAndo:2014,KangRyu:2018} have failed to find evidence of \emph{proton} acceleration.
If CR acceleration occurred, one would expect to find evidence in the form of diffuse gamma-radiation originating from the collision between CR protons and thermal protons, followed by neutral pion decay.
However, a study using the \emph{Fermi}-LAT instrument \citep{Ackermannetal:2016} failed to find evidence of such gamma-ray emission.
Computational studies indicate that if galaxy cluster collision shocks produce CRs at all, the energy fraction lost to the shock in the fashion is expected to be less than one-tenth of a percent \citep{Vazzaetal:2016}.

Further investigation of the possibility of CR acceleration in galaxy cluster shocks requires that we produce numerical models of the shock that include the necessary physical processes to follow particle acceleration.
Although the strong shock regime has been explored extensively, using PIC, PIC-hybrid and combined PIC-MHD codes \citep[e.g.][]{RiquelmeSpitkovsky:2010,Caprioli13,CaprioliSpitkovski:2014a,Caprioli14b,Guoetal:2014a,Guoetal:2014b,Caprioli15,Baietal:2015,paper1}, as well as the Vlasov-Fokker Planck method \citep{Reville12,Reville13}, the weak shock regime has so far been largely ignored.
\citet{Haetal:2018} used particle-in-cell (PIC) simulations that showed that, depending on the input parameters, low-Mach, high-$\beta$ shocks such as these can accelerate particles, depending on the exact sonic Mach number. For those shocks with $\, M_{\rm s}\,\simeq\,2.25$ or more, \cite{Haetal:2018} found both injection of supra-thermal particles near the shock, as well as the onset of diffusive shock acceleration (DSA), the process that allows particles to gain momentum through repeated shock crossings, also known as Fermi~I acceleration \citep[e.g.][]{Bell:1978,BlandfordOstriker:1978,Drury:1983}.
This process requires the presence of instabilities in the local magnetic field, which can reflect the particles toward the shock.
For shocks with a sonic Mach number of $\, M_{\rm s}\,<\,2.25$, \citet{Haetal:2018} found a small particle injection rate (approximately an order of magnitude lower than found for the higher Mach shocks), but no DSA.
Compared to the analytic prediction based on the Rankine-Hugoniot conditions \citep{EdmistonKennel:1984}, which placed the critical Mach number at $M_{\rm s}\approx1-1.1$, this critical Mach number (2.25) is significantly higher, which may help account for the lack of observed diffuse gamma-rays produced in low-Mach, high-$\beta$ ICM shock accelerated ions \citep{Ackermannetal:2016}.
However, the computational cost of the PIC method puts limits on the ability to follow the process over a long time and constrains the size of the spatial domain.
Therefore, these results do not show whether the DSA process in these shocks is adequate to propel particles to relativistic speeds.

In this paper we continue the investigation of particle acceleration in weak shocks, using a different method: the particle-in-MHD-cell (PI[MHD]C) technique \citep{Baietal:2015,paper1,Mignoneetal:2018,Baietal:2019}, using the same code that was previously used in \citet{vanmarleetal:2017,casseetal:2018,vanmarleetal:2018,paper1,vanMarleetal:2019,vanMarleetal:2019b,vanmarle:2020}.
This method allows us to take advantage of the computational efficiency of grid-based magnetohydrodynamics (MHD) while retaining the ability to follow individual, supra-thermal particles.
We take advantage of this by running all simulations in 2-D, which will allow us to study the behaviour of the shock front and evaluate whether the effectively 1-D nature of the original simulations done by \citet{Haetal:2018} created any artefacts.
Our simulations also follow the interaction over a more extended period, which enables us to judge how the growing instabilities influence that morphology of the gas.

\subsection{Requirements for diffusive shock acceleration}
The DSA process allows a shock to accelerate particles to high relativistic speeds. However, before this process can begin, there has to be an injection of supra-thermal particles near the shock itself.
This occurs at the shock front, with a fraction of the particles being reflected, rather than passing through the shock. The PI[MHD]C method cannot model this part of the process.
In a PI[MHD]C simulation, shocks are modelled with MHD, and therefore regarded as discontinuities.
The internal structure of the shock, which is far more complex  \citep[e.g.][and references therein]{Treumann:2009}, is not part of an MHD model.
Instead, we assume that the injection process is effective, and use a parametrized injection mechanism that determines what percentage of the gas passing through the shock becomes supra-thermal. We base our injection rates on the results by \cite{Haetal:2018}, which involved the use of PIC simulations, to determine the injection rate as a function of the sonic Mach number.

Once the supra-thermal particles have been injected, further acceleration depends on their ability to generate instabilities as they travel into the upstream medium.
If these instabilities are sufficiently strong, they will create deviations in the direction of the local magnetic field, which allows the magnetic field to reflect particles back toward the shock, starting the DSA process \citep{Sundbergetal:2016}. This process is self-sustaining and self-amplifying. The higher the momentum of the particles, the more effective they are at exciting instabilities, which, in turn, means that the efficiency of the acceleration process increases. However, the strength of the instabilities (and whether they occur at all) depends on the shock's sonic and Alfv{\'e}nic Mach numbers.

\subsection{Layout}
This paper is structured as follows: In Sect.~\ref{sec:method} we discuss the numerical method as well as the general setup of the simulations. Next, we present a series of simulations, based on the models by \citet{Haetal:2018}, the results of which are shown in Sect.~\ref{sec-result}. Then, in Sect.~\ref{sec-longrun} we explore the long term effects of the particle acceleration process on a single, large-scale simulation.
Finally, in Sect.~\ref{sec-conclusions}, we discuss our results and future plans.
We also include a brief description of the equations used in our code in Appendix~\ref{sec-app1}, as well as an analytical approximation of the various time-scales involved in the perturbations in Appendix~\ref{sec-app2}.

\begin{figure*}
\centering
\mbox{
\includegraphics[width=\columnwidth]{Mach2p0_200.jpeg}
\includegraphics[width=\columnwidth]{Mach2p15_200.jpeg}}
\mbox{
\includegraphics[width=\columnwidth]{Mach2p25_200.jpeg}
\includegraphics[width=\columnwidth]{Mach2p5_200.jpeg}}
\caption{Morphology of the gas at the end of the simulation after $t\,=\,20\,000\,R_{\rm l}/c$, for $\, M_{\rm s}\,=,2.0$ (top left), $2.15$ (top right) and , $2.25$ bottom left), and $2.5$ (bottom right), showing, from top to bottom the magnetic field strength relative to the undisturbed upstream magnetic field, the relative density of the supra-thermal particles relative to the thermal gas density and the thermal gas density relative to the undisturbed upstream thermal gas density. The magnetic field lines are plotted on top of the thermal gas density plot. This figure zooms in on the shock, the actual simulation box extend from $x=-90$ to $x=90$. Although all simulations show a disturbance of the magnetic field strength (top panel), none show a significant disturbance of the \emph{direction} of the magnetic field lines, which is required for particle acceleration.}
\label{fig:results1}
\end{figure*}

\begin{figure*}
\centering
\mbox{
\includegraphics[width=\columnwidth]{Mach2p85_200.jpeg}
\includegraphics[width=\columnwidth]{Mach3p2_200.jpeg}}
\mbox{
\includegraphics[width=\columnwidth]{Mach3p5_200.jpeg}
\includegraphics[width=\columnwidth]{Mach4p0_200.jpeg}}
\caption{Similar to Fig.~\ref{fig:results1} but for simulations with for $\, M_{\rm s}\,=,2.85$ (top left), $3.2$ (top right) and , $3.5$ (bottom left), and $4.0$ (bottom right). Unlike the simulations with lower $\, M_{\rm s}$ these models show disturbance of the magnetic field lines, indicating that particle acceleration can take place.}
\label{fig:results2}
\end{figure*}

\section{Numerical method}
\label{sec:method}
\subsection{Code}
We use the combined PIC-MHD or Particle in MHD cells (PI[MHD]C) method described in \citet{Baietal:2015,paper1}. This method is based on the assumption that the gas can be treated as a primarily thermal gas, with a relatively small supra-thermal component. The thermal gas is treated as a fluid, using the MHD method, whereas the supra-thermal component is treated kinetically.

The interaction between the two components is treated in a self-consistent manner.
The force generated by the electromagnetic field of the thermal gas is part of the equation of motion of the particles, as is the opposite force on the thermal gas generated by the particles. Furthermore, the effect of a charge and current density resulting from the presence of the non-thermal particles is incorporated in the MHD-equations through a rewritten form of Ohm's law \citep{Baietal:2015},
\begin{equation}\label{Eq:Ohmslaw}
c\, \mathbf E = -\left((1-R)\, \mathbf v +R\, \mathbf u_{\rm part}\right)\times\, \mathbf B
\end{equation}
with $c$, the speed of light, $\, \mathbf E$ the electric field, $\, \mathbf v$ the thermal plasma velocity, $\, \mathbf u_{\rm part}$ the average velocity of the supra-thermal particles, obtained through interpolation, $\, \mathbf B$ the magnetic field and $R$ the supra-thermal particle charge density relative to the total charge density.
$\, \mathbf u_{\rm part}$ and the supra-thermal particle charge density are obtained by mapping the particle distribution in space and momentum space onto the grid at the start of each time step.
Time step control is maintained through the Courant{-}Friedrichs{-}Lewy (CFL) condition, which is applied to both the thermal gas and the particles to ensure numerical stability.

We consider the gas to be non-collisional. Therefore, there is no kinetic interaction between the particles, nor a friction force generated by the motion of the particles through the thermal gas. The only interaction between the thermal and supra-thermal components is through the electromagnetic field (the code does not include a CR-pressure term).

The main advantage of the PI[MHD]C approach is that it allows for faster calculations than either the PIC or the PIC-hybrid method, both of which require large particle populations to simulate the thermal gas, whereas the PI[MHD]C method achieves this by solving the MHD equations for the thermal gas, which is a less computationally expensive approach.

Our code is based on the {\tt MPI-AMRVAC} code \citep[e.g.][]{vanderHolstetal:2008,Keppensetal:2012}; a fully conservative, finite-volume MHD-code that solves the conservation equations of magnetohydrodynamics on an {\tt OCTREE}-based adaptive mesh \citep{ShephardGeorges:1991} and is MPI-parallel.
To this code we have added a new set of conservation equations \citep{paper1} that incorporates the effect of supra-thermal particles on the thermal gas and a Boris-pusher \citep{BirdsallLangdon:1991} to calculate the motion of the particles as a function of the electromagnetic field.
We have also added a constrained-transport module  based on \citet{BalsaraSpicer:1999} in order to guarantee a divergence-free magnetic field.
As in \citet{paper1} we use a {\tt TVDLF} solver, combined with a van~Leer flux limiter. This  combination provides us with a reliable and precise numerical scheme capable of capturing the small scale features of the plasma and the magnetic field.
The conservation equations, as implemented in this code, can be found in Appendix~\ref{sec-app1}. For a full description of the numerical method as implemented in this code, please refer to \citet{paper1}, as well as the description in \citet{Baietal:2015}.

\begin{table}
 \caption{Input parameters \label{tab:input}}
 \label{tab:anysymbols}
 \begin{tabular}{lcccc}
  \hline
Model name & $\, M_{\rm s}$ & $\, M_{\rm A}$ & $v_0/c$ & f$_{\rm inj}$ \\
  \hline
M2     & 2.0  & 18.2 & 0.027   & 0.003 \\
M2.15  & 2.15 & 19.6 & 0.0297  & 0.003 \\
M2.25  & 2.25 & 20.5 & 0.0315  & 0.0035  \\
M2.5   & 2.5  & 22.9 & 0.035   & 0.0035  \\
M2.85  & 2.85 & 26   & 0.0395  & 0.00375  \\
M3.2   & 3.2  & 29.2 & 0.052   & 0.004  \\
M3.5   & 3.5  & 31.9 & 0.057   & 0.007  \\
M4     & 4.0  & 36   & 0.066   & 0.009  \\
  \hline
 \end{tabular}
\end{table}

\subsection{Simulation setup}
As input conditions, we use the same models described in \citet{Haetal:2018}, focussing on the models M2-M4 listed in Table~1 of that paper. In those simulations a beam of plasma collided with a fixed wall, forming a shock that moved upstream into the beam. These simulations, which \citet{Haetal:2018} describe as {\emph{almost 1-D}, used an extremely narrow box that covers less than a single Larmor radius in the direction perpendicular to the flow because of the high computational cost of the PIC method, which made the use of a wider box impractical. As a result, they could not resolve any variations in the thermal plasma along the perpendicular axis. \citet{Haetal:2018} defined the physics  properties of the simulations by using a fixed starting temperature for the upstream gas of $10^8\,K$ and  plasma-$\beta\,=\,100$ for all simulations. With these two quantities fixed, \citet{Haetal:2018} chose the sonic Mach number of the shock as the free parameter that made  each simulation unique. They placed upstream magnetic field in the plane of the simulation at a 13$^o$ angle with the flow.}

Because of the difference in numerical method, rather than aiming a beam of plasma at a reflecting wall and tracing the shock as it moves back into the upstream medium, we start our simulations from the analytical solution of the Rankine{-}Hugoniot conditions. This approach  allows us to use the co-moving frame of the shock as rest-frame for our simulations, reducing the required size of the simulation box along the flow direction. Like models M2-M4 in \citet{Haetal:2018}, our simulations cover the parameter space ranging from a sonic Mach number of $\, M_{\rm s}\,=\,2-4$, with a constant plasma-$\beta\,=\,100$ and a fixed angle of $13^{\rm o}$ between the flow and the upstream magnetic field $B_0$.
We place field in the plane of the simulation, with the third component, which is orthogonal to the plane of the simulation, initialized at zero.
For the full set of input parameters, see Table~\ref{tab:input}, which uses the same units as in \citet{Haetal:2018}. This table lists the sonic and Alf{\'e}nic Mach numbers of the shock, the upstream velocity $v_0$ and the injection rate of supra-thermal particles. It should be noted that in this table $v_0$ is the flow-velocity in the rest-frame of the downstream medium, as used by \citet{Haetal:2018}, rather than the shock velocity, which follows from the Rankine-Hugoniot conditions.

At the start of the simulation, we consider the gas to be purely thermal with no supra-thermal component. During the simulation, we continuously inject supra-thermal particles directly downstream of the shock, at a rate derived from the PIC simulations in \citet[][Figure~5]{Haetal:2018}. (If the shock moves during the simulation, we track this  motion to ensure that new particles continue to be injected at the shock.)
Using these values allows us to avoid the main uncertainty in the PI[MHD]C method: the injection rate of the supra-thermal particles.
In two cases, we deviate from this pattern: the $\, M_{\rm s}\,=\,2$ and $2.15$ simulations. \citet{Haetal:2018} found only a negligible injection rate for these particular models.
Injecting supra-thermal particles at such a low rate would be pointless as it would merely confirm that without a
significant fraction of supra-thermal particles the thermal gas and the shock remain in the equilibrium derived from the Rankine-Hugniot conditions. Instead, we use the power-law shown in
\citet[][Figure~5]{Haetal:2018} to extrapolate an injection fraction of 0.003 ($0.3$\,percent of the total mass). This will allow us to determine whether any kind of DSA is possible at such a low Mach number, given the injection of a sufficient number of supra-thermal particles.

The charge-to-mass ratio of the particles reflects that of protons (we assume that all electrons are thermal) and is calculated so that a total of $1\times10^7$ particles is injected during the simulation. The total duration of each simulation equals 20\,000\,$\, R_{\rm l}/c$, where $\, R_{\rm l}=v_{\rm inj}/{B_0}$ the Larmor radius determined by the upstream magnetic field and the injection velocity $v_{\rm inj}$ and the upstream magnetic field $B_0$, and the injection starts at $t\,=\,1\,000\,\, R_{\rm l}/c$, to allow the thermal gas a brief period to relax from the analytical solution to a stable numerical solution. We inject the particles with a velocity $v_{\rm inj}$ of three times the pre-shock speed of the gas, isotropically distributed within the rest-frame of the post-shock thermal gas, conform the prescription used in \citet{paper1} and \cite{vanMarleetal:2019}.
During the injection process, mass, momentum and energy are conserved by removing an equivalent amount of mass, momentum and energy density from the thermal gas in the grid cell where each particle is injected.

For our simulations, we use a 2-D grid, spanning 180$\, R_{\rm l}$) along the x-axis (parallel to the flow) by 30$\, R_{\rm l}$ along the z-axis (perpendicular to the flow). At the coarsest level, our grid has one grid cell per Larmor-radius, and we allow three additional levels of refinement. Each level doubles the effective resolution. Therefore, at maximum resolution, we have eight grid cells per Larmor radius.
For comparison with PIC or di-hybrid simulations, we need to keep in mind that the particle injection velocity is three times the upstream bulk velocity in the rest-frame of the shock. Therefore $\, R_{\rm l}$, as defined in this paper, is three times the Larmor radius of the upstream thermal gas.
Within five Larmor radii of the shock, we enforce the highest level of refinement at all times to ensure that both the shock itself and the particle motion near the shock remain fully resolved.
Vector quantities (velocity, electromagnetic field) have three components, making our models effectively 2.5-D. When calculating the charge and current density resulting from the particle distribution, we map the charge and current of each particle onto the four surrounding cell-centres.

\begin{figure}
\centering
\mbox{
\includegraphics[width=\columnwidth]{para_SED_2_2p25_new.png}}
\caption{Normalized spectral energy distribution, as a function of the Lorentz factor ($\gamma$), for the total particle population of the simulations with sonic Mach numbers 2-2.25 at $t\,=\,20\,000\,R_{\rm l}/c$. None of these SEDs show any evidence for DSA.}
\label{fig:parased1}
\end{figure}

\begin{figure}
\centering
\mbox{
\includegraphics[width=\columnwidth]{para_SED_2p5_3p2_new.png}}
\caption{Similar to Fig.~\ref{fig:parased1} but for the simulations with sonic Mach numbers 2.5-3.2. These simulations show evidence of DSA, but only for part of the particle population.}
\label{fig:parased2}
\end{figure}

\begin{figure}
\centering
\mbox{
\includegraphics[width=\columnwidth]{para_SED_3p5_4_new.png}}
\caption{Similar to Figs.~\ref{fig:parased1}-\ref{fig:parased2} but for the simulations with sonic Mach numbers 3.5 and 4. These simulations show clear evidence of DSA but only for part of the particle population. The slopes are approaching the expected power law index.  For comparison we have added the analytically predicted slope for the $M_S\,=\,4$ shock ($s\,=\,1.64$).}
\label{fig:parased3}
\end{figure}

\section{Parameter space}
\subsection{2-D Morphology of the gas}
\label{sec-result}
The response of the thermal gas and the magnetic field to the injection of the supra-thermal particles varies according to the sonic Mach number, as shown in Figs.~\ref{fig:results1}-\ref{fig:results2}, shows a clear trend. Each panel shows the magnetic field strength relative to the undisturbed upstream magnetic field strength ($B_{\rm 0}$) (top), the supra-thermal gas density ($\rho_{\rm p}$) relative to the thermal gas density (middle) and thermal gas density relative to the undisturbed upstream thermal gas density ($\rho_{\rm 0}$) (bottom) as well as the magnetic field lines. Although the simulations are run in the shock rest-frame (determined from the analytical solution), the shocks tend to move over time.
The injection process removes a small but noticeable fraction of the thermal gas pressure in the downstream medium, which would lead the shock to start moving in the downstream direction.
Depending on the strength of the instabilities, this trend can be reversed if the downstream magnetic field amplification becomes sufficiently strong to counteract this effect by increasing local magnetic pressure.
The low-Mach simulations ($\, M_{\rm s}\,\leq\,2.5$) show a disturbance of the magnetic field strength, but not of the magnetic field lines, even though we have artificially enhanced the injection rate for the $\, M_{\rm s}\,=\,2-2.15$ shocks.
As a result, even though the magnetic field is influenced by the presence of supra-thermal particles, no DSA can be expected to occur. In contrast, the (relatively) high-Mach simulations ($\, M_{\rm s}\,\geq\,3.2$) show disturbance of both the field lines and the field strength, indicating that DSA can take place. In between these two extremes lies a regime that shows some distortion of the field lines, but only locally, with some field lines showing twists, while others do not.
Even in those cases where the perturbations are relatively strong, they tend to be weaker than  perturbations found for comparable models of high-Mach, low-$\beta$ shocks \citep{paper1}.
The magnetic field amplification tends to be of the order of $2-4$, not exceeding one order of magnitude even for the $\, M_{\rm s}\,=\,4.0$ model. For comparison, the $\, M_{\rm s}\,=\,30.0$, $\beta\,=\,1$ shocks in \citet{paper1} showed amplification of 15-25, depending on the angle between the flow and the magnetic field.

This result can be compared qualitatively to the results found by \citet{Haetal:2018}, which determined that the instabilities in the lower Mach simulations are resonant-streaming instabilities \citep{Bell:1978}, whereas the higher Mach models display both resonant and non-resonant streaming \citep{Bell04} characteristics.
This behaviour is consistent with the results of \citet{Caprioli14b}, which determined that the transition between resonant and non-resonant streaming instabilities lies around an Alf{\'e}nic Mach number of $\, M_{\rm A}\,\simeq\,30$.
The critical Mach number, below which no significant instabilities occur, seems to lie somewhat higher than what was found by \citet{Haetal:2018}, who put it at ($\, M_{\rm s}\,\simeq\,2.25$) This can be explained by the nature of the injection mechanism, which, in our case, is isotropic in the post-shock medium, whereas, in reality, the particle injection velocity and direction is a more complicated issue that depends on the exact conditions of the shock.
Furthermore, our models show a transition region ($2.5\,\geq\,\, M_{\rm s}\,\geq\,3.2$), rather than a single critical Mach number.
This is the result of having a fully 2-D model, rather than one that is effectively 1-D In a 1-D model, the magnetic field is either perturbed or not, whereas a 2-D model allows for variations along the plane of the shock. As will be seen in Sect.~\ref{sec-parased}, these variations also influence  the particle spectral energy distribution (SED).

The instabilities lack the filamentary structure that is characteristic of the high-Mach, low-$\beta$ simulations \citep[e.g.][]{paper1,vanMarleetal:2019}.
Such filaments require a relatively stiff magnetic field that can resist the forces that are acting upon it.
In a high-$\beta$ plasma, the magnetic field is powerless to resist either the distorting force exerted by the particles (assuming a sufficiently high injection rate) or the thermal pressure.
As a result, a local instability will tend to grow in all directions, distorting the magnetic field, rather than conforming to the direction of the field lines.

How the perturbations in the upstream medium depend on the sonic Mach number can be explained by a comparison of three different time-scales: The perturbing time-scale, which depends on the force acting on the magnetic field, determines how quick the instabilities grow. The sonic and magnetic time-scales determine how quickly the thermal gas can respond.
As long as the sonic and magnetic time-scales are shorter than the perturbing time-scale, the instabilities cannot grow. On the other hand, if the perturbing time-scale is shorter than both the sonic and magnetic time-scales, the instabilities will continue to grow because the thermal gas cannot compensate in time.
In between these two extremes lies a regime where the perturbing time-scale is shorter than the magnetic time-scale, which allows the variations in magnetic field strength to grow, but longer than the sonic time-scale, which means that any perturbation in the direction of the field lines is counteracted by the thermal pressure.
(N.B. This only applies to the high-$\beta$ regime. In gas with a plasma-$\beta\,<\,1$, the situation would be reversed.) An analytical approximation of the various time-scales is presented in Appendix~\ref{sec-app2} but should be treated with caution because it depends on many factors, which tend to vary over time.
This time-scale dependence explains the behaviour of the high-$\beta$ simulations.
In the case of the $\beta\,=\,1$ simulations, which have been more common in the past, the thermal gas either shows a clearly perturbed magnetic field, or it shows no instabilities at all because the 'in-between' regime does not exist. The larger the gap between the sonic and Alf{\'e}nic speeds, the more opportunities there are for a 'partial instability' to occur where only the field strength varies, whereas the field direction remains constant.

For most simulations, the plane of the shock remains almost undisturbed, in contrast to the high-Mach shocks shown in \citet[e.g.][]{Baietal:2015,paper1,vanMarleetal:2019}, where ram-pressure variations in the upstream medium, resulting from the filamentary structure of the instabilities, caused the corrugation and eventually the complete distortion of the shock front. For low-Mach shocks, the variation in the total pressure that the shock experiences is much smaller and both time- and space-dependent. As a result, the shocks show little to no corrugation.

\subsection{Spectral distribution of supra-thermal particles}
\label{sec-parased}
The momentum distribution for particles accelerated through diffusive shock acceleration is given by
\begin{equation}
\label{eq:mom}
f(p)~\propto~p^{-q}
\end{equation}
with $q\,=\,3r_{\rm c}/(r_{\rm c}-1)$ and $r_{\rm c}$ the compression ratio of the shock \citep{BlandfordOstriker:1978}.
For non-relativistic particles where the particle energy $E_{\rm i}$ scales with the momentum as $E_{\rm i}\,\propto\,p_{\rm i}^2/m_{\rm i}$.
This results in a spectral energy distribution that can be represented by
\begin{equation}
\label{eq:gammamin1}
\frac{\partial N}{\partial\gamma}~\propto~(\gamma-1)^{-s},
\end{equation}
with $s\,=\,(q-1)/2$ and $\gamma$ the Lorentz factor. However, should the particles attain relativistic speeds the energy/momentum relationship changes until, at high relativistic speeds, it becomes $E_{\rm i}\,\propto\,p_{\rm i}$.

The SEDs for the particles, shown in Figs.~\ref{fig:parased1}-\ref{fig:parased3} in our simulations can be classified into three distinct groups. Like \citet{Haetal:2018}, we find no evidence for DSA for the lowest sonic Mach numbers ($\, M_{\rm s}\,=\,2.0-2.25$, Fig.~\ref{fig:parased1}).
The particles show no sign of significant acceleration, as was already predicted from the morphology of the gas and the magnetic field. Neither is there any sign that the particles adhere to a power-law spectrum, which would appear as a straight line in a log-log plot. Instead, the particle energies have spread out around the injection speed, indicating that although some particles have been accelerated, others have actually been decelerated. Simulations of high-Mach shocks \citep{paper1,vanmarle:2020} also show that a fraction of the injected particles loses decelerate, triggering instabilities in the thermal plasma at the expense of their own energy. However, in high-Mach shocks, once the instabilities have been triggered, subsequent interactions between the magnetic field accelerate particles through the DSA process.
For the $\, M_{\rm s}\,=\,2.0-2.25$ simulations shown here, no significant acceleration occurs because the instabilities dissipate almost immediately.
The end result is a particle energy distribution that starts to resemble that of a thermal plasma.
However, because the particles do not collide directly, they cannot actually become thermalized.
The behaviour at low-Mach numbers is particularly meaningful in light of the artificially enhanced injection rate that we have adopted for the models with $\, M_{\rm s}\,=\,2.0-2.15$.
Despite the high injection rate of supra-thermal particles, there is no evidence of DSA.
Clearly, under these conditions, the shock is incapable of accelerating CRs.

At the other end of the scale ($\, M_{\rm s}\,=3.5-4$, Fig.~\ref{fig:parased3}) the particles SEDs show clear evidence for DSA. Both SEDs show evidence that the energy distribution is starting to follow  a straight line in the log-log plot, indicating adherence to a power-law with a fixed index between $(\gamma-1)\,=\,0.03-0.06$ for the $\, M_{\rm s}\,=\,3.5$ shock and  $0.04-0.08$ for the $\, M_{\rm s}\,=\,4$ shock. For the latter, the expected slope, following from the compression ratio  would be $s\,\sim\,1.64$ according to Eq.~\ref{eq:gammamin1}. We have included an indicator of that expected slope in the plot for comparison.

For the intermediate Mach numbers (Fig.~\ref{fig:parased2}, the SEDs show a combination of these two extremes.
Although there is evidence for DSA, in the form of an extended tail at high energies, there is also a peak around the injection energy, clearly indicating that not all particles are participating in the acceleration process.
That some particles can avoid participating in the DSA process is partially the result of the behaviour of the magnetic streamlines described in Sect.~\ref{sec-result}.
Depending on the injection location, particles may either encounter instabilities on its journey upstream or not, giving the particles a chance to escape from the system without being accelerated. Adherence to a power-law index is barely visible, except in the $\, M_{\rm s}\,=\,3.2$ case, and even there only for a very short interval, although this is partially a result of the limited size of the simulation box. As the particles gain momentum, they will travel further away from the shock before being reflected. If they reach the upper or lower x-boundary before being reflected, they escape from the system. Although these simulations give us a good indication whether DSA is possible at all, in order to estimate its efficiency as well as the maximum possible energy, we will need to increase the size of the simulation box. (See Sect.~\ref{sec-longrun}).

\begin{figure*}
\centering
\mbox{
\includegraphics[width=\columnwidth]{Mach3p2_050_longbox.jpeg}
\includegraphics[width=\columnwidth]{Mach3p2_100_longbox.jpeg}}
\mbox{
\includegraphics[width=\columnwidth]{Mach3p2_150_longbox.jpeg}
\includegraphics[width=\columnwidth]{Mach3p2_200_longbox.jpeg}}
\caption{Similar to Figs.~\ref{fig:results1}-\ref{fig:results2}, but for the $\, M_{\rm s}\,=\,3.2$ model with an extended simulation box, showing the area near the shock. These figures show the area near the shock at $t\,=\,5\,000$ (top left), 10\,000 (top right)
15\,000 (bottom left) and 20\,000 $R_{\rm l}/c$ (bottom right). The large distortion of the magnetic field is clearly visible. }
\label{fig:results3}
\end{figure*}

\begin{figure}
\centering
\mbox{
\includegraphics[width=\columnwidth]{longbox_sed.png}}
\caption{Total particle SED at the same moments in time as \ref{fig:results3} for the  $\, M_{\rm s}\,=\,3.2$ model with an extended simulation box. Over time, the SED matches the expected power-law index and shows that DSA can accelerate particles to relativistic speeds.
The $q\,=\,4.4$ line demonstrates the power-law slope expected for a Mach 3.2 shock.}
\label{fig:longboxSED}
\end{figure}

\begin{figure}
\centering
\mbox{
\includegraphics[width=\columnwidth]{Bangle.png}}
\caption{Angle between the flow and the magnetic field at the shock as a function of the location along the z-axis at the same moments in time as in Fig.~\ref{fig:results3}. The shock, which started out as quasi-parallel, occasionally becomes semi-perpendicular as a result of the instabilities in the upstream medium.}
\label{fig:Bangle}
\end{figure}

\begin{figure}
\centering
\mbox{
\includegraphics[width=\columnwidth]{MS.png}}
\caption{Sonic mach number at the shock as a function of the location along the z-axis at the same moments in time as in Figs.~\ref{fig:results3} and \ref{fig:Bangle}. Whereas the shock started at $\, M_{\rm s}\,=\,3.2$, it varies over time between approximately 2.7 and 3.4.}
\label{fig:machnumber}
\end{figure}

\section{The large box model}
\label{sec-longrun}
In order to explore the long term effects of the instabilities as well as to determine the maximum particle energy that can be achieved in this fashion, we repeat the simulation with a sonic Mach number of 3.2 with a far more extended box, which has a size of $2400\,\times\,15\, R_{\rm l}$, compared to the $180\,\times\,30\, R_{\rm l}$ box of the previous simulations. (We have reduced the size of the bow along the z-axis by half in order to reduce computation time.)
For this simulation, we use a minimum resolution of $4800\,\times\,30$ grid points and allow two additional levels of refinement in order to achieve the same effective resolution as in the models described in Sect.~\ref{sec-result}. The result, in a series of snapshots, is presented in Fig~\ref{fig:results3}, which shows the morphology of the gas and the magnetic field near the shock at $t\,=\,5\,000$ ), 10\,000, 15\,000, and 20\,000 $R_{\rm l}/c$.
As for the smaller box model, this simulation shows that at Mach 3.2, the upstream magnetic field becomes distorted, facilitating the DSA. As can be seen in Fig.~\ref{fig:results3}, the box size along the z-axis is still large enough that it does not interfere with the maximum wavelength of the instabilities and allows for variation along the plane of the shock.

\subsection{The particle SED}
\label{sec-parasedlong}
Figure~\ref{fig:longboxSED} (right panel) shows the particle SED the total particle populations at the same moments in time as Fig.~\ref{fig:results3}.
Because the particles are entering the relativistic regime, where the relationship between energy and momentum changes, we show the SED as a function of normalized momentum $p=\gamma v$. Using the Lorentz factor would no longer produce a straight line in the log-log plot. For a $\, M_{\rm s}\,=\,3.2$ shock, the power-law index can be expected to be approximate $q\,=\,4.4$, according to Eq.~\ref{eq:mom}. We have added a slope indicator in the plot for comparison. The slope matches reasonably well, though not perfectly.
However, we should keep in mind that the power-law index depends on the compression ratio of the shock.
For the $\, M_{\rm s}\,=\,3.2$ shock, the compression ratio is expected to be a factor 3.1, based on the Rankine-Hugoniot conditions. However, as will be seen in Sect.~\ref{sec-distort}, the sonic Mach number is not a constant in time owing to the instabilities in the upstream medium.

The extreme length of the simulation box ensures that the particles can continue to be part of the acceleration process, rather than escaping from the simulation, allowing them to reach much higher velocities.
The SED shows adherence to a power-law up to approximately eight times the injection momentum, reaching a Lorentz factor of approximately 1.8, which, for protons, is the equivalent of a total energy of $E_{\rm tot}\,=\,\gamma mc^2\,=\,1.6$\,GeV.
Such protons, if they were to interact with thermal protons, would be able to produce gamma-radiation. Beyond this point, the SED drops off, and, from the time evolution, it is clear that running the simulation longer will not change the energy at which the DSA ceases to be effective.

\subsection{Distortion of the upstream medium}
\label{sec-distort}
As the instabilities grow in size, they start to change the nature of the shock.
The angle at which the magnetic field enters the shock varies considerably, both in time and space, as shown in Fig.~\ref{fig:Bangle}, which shows the angle between the flow and the magnetic field directly ahead of the shock at different moments in time. \citet{Haetal:2018} found that the angle of the magnetic field with the shock does not greatly influence the particle injection rate, as long as the shock qualifies as quasi-parallel.
Similarly, \citet{Fangetal:2019} found comparable ion SEDs for shocks varying between 15$^{\rm o}$ and 45$^{\rm o}$.
However, this relies on the magnetic field remaining quasi-parallel. As can be seen in Fig.~\ref{fig:Bangle}, which shows the angle between the flow and the magnetic field ahead of the shock, this can no longer be assumed because the magnetic field becomes quasi-perpendicular at certain times, depending on the position along the shock front. How this will influence the injection rate is a complex question.
\citet{Haetal:2018} found that a quasi-perpendicular shock could give particles a limited acceleration through the shock-drift acceleration (SDA) process, but found no evidence for DSA. This result coincides with the results found by \citet{CaprioliSpitkovski:2014a} for higher Mach shocks, whereas \citet{paper1} found that DSA could occur in quasi-perpendicular shocks, assuming a sufficiently high injection rate.
However, none of the above results genuinely apply to a situation in which only part of the shock is quasi-perpendicular and then only at certain times.
A further effect of the increased instabilities in the upstream gas is a change in the sonic Mach number of the shock, shown in Fig.~\ref{fig:machnumber} for the same moments in time as in Fig.~\ref{fig:Bangle}. As the magnetic field becomes distorted, the flow in the thermal gas starts to compress the loops in the magnetic field as they approach the shock. The compression of the magnetic field, in turn, increases the local magnetic field strength, which, combined with the magnetic tension as the curvature of the magnetic field lines increases allows the magnetic field to resist the pressure effectively. This causes variations in the local gas temperature and flow-velocity, changing the Mach number.
The influence of the sonic Mach number on the injection rate is shown quite clearly by \cite{Haetal:2018}, though we should keep in mind that this was for simulations with a fixed plasma-$\beta$, something that does not apply to our simulations as a result of the changes in the upstream morphology.

\section{Conclusions}
\label{sec-conclusions}
We have investigated the behaviour of low-Mach, high-$\beta$ shocks and their ability to accelerate particles through the DSA process, using the PI[MHD]C method.
For small scale simulations, our results bear a close similarity to those obtained by \citet{Haetal:2018} with PIC simulations, allowing for the inherent uncertainty caused by the fact that we have to assume a particle injection rate. Rather than finding a 'critical Mach number', at which the shocks go from not accelerating particles at all to clear evidence of DSA, we find that there is a transitional zone between approximately $\, M_{\rm s}\,\approx\,2.5-3.2$. For shocks with Mach-numbers below this zone, no acceleration takes place, even when stimulated with an artificially high injection rate, while above this zone the shocks show clear evidence of DSA.
Within the transitional zone, some particle acceleration will occur, but the SEDs show deviation from the expected power-law index.
It is likely that within this region the efficiency of DSA will depend strongly on input conditions, which, in turn, means that some galaxy cluster shocks in this parameter space will be able to accelerate CRs, whereas others will not, depending on local circumstances.

Over longer time-scales, the growing instabilities in the upstream medium observed in simulations with sonic Mach number of >3 deviate from the results by \citet{Haetal:2018}. This deviation takes the form of varying Mach numbers at the shock, as well as a severely distorted magnetic field. Once the simulation reaches this point, the fixed injection rate is no longer a valid assumption.
In the long run, this effect is likely to cause a considerable change in the efficiency of CR production. Even those shocks that have a sufficiently high Mach number will end up exciting such severe instabilities that the Mach number starts to vary. Only if this causes the injection rate to be sufficiently reduced, which is certainly possible if the Mach number drops, the instabilities will fade, which will eventually allow the shock to return to its original strength, at which point the process will repeat itself.
Furthermore, the power-law index of the particle SED depends directly on the compression ratio  of the shock.
Owing to the instabilities, this will become increasingly variable over time, limiting our ability to quantify the energy loss through cosmic rays, which is unlikely to be a constant factor. Further investigation, in particular regarding the injection efficiency as a function of Mach-number, plasma-$\beta$, and magnetic field angle, is required before such an analysis becomes possible.

These simulations demonstrate that large-scale, multi-D simulations are required in order to thoroughly investigate the behaviour of shocks in the presence of supra-thermal particles. While 1-D simulations can tell us much about the structure of the shock itself as well as the injection process, the long term evolution of the instabilities that enable the acceleration process is a fundamentally multi-D problem on scales that exceed the Larmor radius of the injected particles. This requires us to use simulation boxes that can capture the large-scale variations in the thermal plasma perpendicular to the flow and extend sufficiently to allow for repeated particle acceleration events.

Future developments will have to include a scheme that adjusts the injection rate as a function of shock conditions. However, this is not an easy task because the shock conditions do not only vary over time but depend on the location along the shock front as well.
Furthermore, the velocities of the thermal gas in this kind of shock is approaching the point where a relativistic treatment of the thermal gas becomes necessary. A new version of the PI[MHD]C code, which allows for the combination of a relativistic thermal gas with non-thermal particles, is currently undergoing testing.

Whether there is merit to repeating these simulations in 3-D is an open question. \citet{vanMarleetal:2019} showed for a high-Mach model that the morphology of the thermal gas and the magnetic field did not change significantly between 2-D and 3-D models, but that the SED of the 3-D model showed a marked decrease in acceleration efficiency. However, that was for a shock that became severely distorted over time, something that is not the case for the low-Mach models. As it is, the computational cost of a 3-D model, particularly a 3-D model large enough to resolve the instabilities and follow the acceleration of particles to high velocities, remains prohibitive.

\section*{Acknowledgements}
This work was supported by the National Research Foundation (NRF) of Korea through grant 2016R1A5A1013277 and by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the  Ministry of Education, Science and Technology (2018R1D1A1B07044060). This work was supported by the National Research Foundation (NRF) of Korea through grant 2016R1A5A1013277 and by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the  Ministry of Education, Science and Technology (2018R1D1A1B07044060). This work is supported by the ANR-19-CE31-0014 GAMALO project.

The author wishes to thank Prof. D. Ryu, Prof. H. Kang and J.-H. Ha for their valuable comments and discussions.

The author thanks the anonymous reviewer for their many helpful comments

\section*{Data availability}
Data available on request.

\bibliographystyle{yahapj}

redpajama_set_name: RedPajamaArXiv


Petersham Nurseries020 8940 5230work Garden CentreInternationally prized garden centre, Petersham Nurseries is a tranquil oasis and seedbed of inspiration.
They invite you to dine in our glasshouse restaurant, browse plants in our nursery, find antiques and gifts in our shop, or sit, wander and enjoy seasonal food and homemade cakes in our teahouse.
Internationally prized garden centre, Petersham Nurseries is a tranquil oasis and seedbed of inspiration.
Petersham Nurseries have created a place of calm, away from the bustle of London, somewhere that respects and is in tune with nature and positive living.


text:
Q: NA values when trying to return a numeric vector from character vector I have a column from a dataframe that I want to read into R and am trying to extract.
AB_lst <- read.csv("tableOut.csv", stringsAsFactors = FALSE)
AB_mass <- AB_lst$StructCalc
AB_mass_numeric <- as.numeric(AB_mass)

I want AB_mass_numeric to be a numeric vector but whenever I wright the above code I get
warning message: NAs introduced by coercion
when I do head(AB_mass) the output looks like:
"370.104704 ..." "365.173393 ..." "312.062840 ..." "266.151261 ..." "372.120355 ..." "210.088660 ..."

Why is this error happening and how can I fix it so I have a vector of type numeric with these values? I think the problem has something to do with the "..." but I am not exactly sure. An example of AB_lst is below.
X     CAS.RN                                         Name       Formula          Mass
1 2 28458-24-4                    (+)-Averufanin; Avermutin    C20 H18 O7 370.353 g_mol
2 3 23402-09-7                           (+)-Brevianamide A C21 H23 N3 O3 365.426 g_mol
3 4  1162-65-8 (-)-Aflatoxin-B1; Aflatoxin B; Aflatoxin FB1    C17 H12 O6 312.274 g_mol
4 5 26057-70-5                             (-)-Avenaciolide    C15 H22 O4 266.333 g_mol
5 6  5803-62-3                                (-)-Averantin    C20 H20 O7 372.369 g_mol
6 7 20421-31-2                            (-)-Canadensolide    C11 H14 O4 210.226 g_mol
                                                                                Sources
1                                                                                [F] Aspergillus versicolor
2                                                                                [F] Penicillium brevicompactum, P. viridicatum
3                         [F] Aspergillus flavus, A. parasiticus, P.puberulum, P.sp., Asp.sulphureus, P. ostianus; "MunissiMUF2
4 [F] Aspergillus avenaceusIsolation extraction with (EtOAc, 3, filt.) chromatogr. with (Sil-G, ) crystallizat. with (Et2O-Hex)
5                                                                               [L] [F] Aspergillus versicolor; Solorina crocea
6  [F] Penicillium canadense, Aspergillus tamariiIsolation chromatogr. with (Sil-G, Benz-EtOAc) ion exchange with (XAD-2, MeOH)
                                                                                C.NMR
1                                                                                SIM (187.0 S C2 +-4.3 96*) (181.9 S C8 +-1.5 192*) (164.9 S C18 +-1.4 31*) (164.1 S C10 +-1.443*) (162.8 S C9 +-0.5 11*) (161.0 S C6 +-1.9 26*) (135.9 S C7 +-9.8 217*) (135.9 S C4 +-9.8 217*) (119.7 S C5+-0.6 9*) (118.9 S C1 +-9.8 141*) (109.2 S C3 +-1.2 43*) (108.7 D C12 +-2.3 18*) (108.6 D C15 +-0.6 34*)(108.4 D C14 +-2.0 31*) (74.8 D C11 +-1.9 6*) (74.8 D C22 +-0.2 5*) (32.4 T C26 +-1.2 51*) (28.9 T C24 +-1.08*) (23.3 T C25 +-0.1 5*) (20.9 Q C27 +-1.9 52*)
2                                                                                SIM (203.4 S C11 +-1.6 Int) (173.7 S C10 +-0.0 1*) (170.3 S C3 +-1.4 Int) (160.5 S C15 +-0.2 8*)(134.7 D C27 +-3.3 98*) (124.6 D C23 +-0.1 9*) (124.5 D C26 +-6.4 338*) (120.2 S C13 +-0.4 8*) (111.8 D C24+-0.2 9*) (69.8 S C5 +-0.0 1*) (69.0 S C2 +-1.6 Int) (65.2 S C1 +-1.6 Int) (55.5 D C7 +-1.7 Int) (44.2 T C19 +-0.01*) (31.2 S C9 +-4.0 Int) (31.1 T C14 +-0.0 1*) (29.7 T C20 +-0.0 1*) (28.7 T C12 +-1.7 Int) (25.4 T C25 +-0.0 1*)(12.5 Q C22 +-9.8 Int) (12.5 Q C21 +-9.8 Int)
3 SIM-EXP (117.0 - 117.0, 1) (176.5 - 176.9, 2) (161.0 - 161.4, 3) (152.5 - 152.2, 4) (103.7 - 104.8, 5)(107.5 - 107.4, 7) (165.3 - 164.5, 8) (113.2 - 113.0, 10) (154.7 - 155.6, 11) (47.8 - 47.7, 12) (90.6 - 90.3, 13)(200.6 - 200.7, 14) (29.0 - 28.9, 15) (144.8 - 145.1, 18) (102.3 - 102.5, 19) (35.0 - 34.9, 20) (56.4 - 55.8, 23) ;SIM-EXP (117.0 - 117.0, 1) (176.9 - 176.5, 2) (161.4 - 161.0, 3) (152.2 - 152.5, 4) (104.9 - 103.7, 5) (107.4 -107.5, 7) (164.5 - 165.3, 8) (113.0 - 113.2, 10) (155.6 - 154.7, 11) (47.7 - 47.8, 12) (90.3 - 90.6, 13) (200.7 -200.6, 14) (28.9 - 29.0, 15) (145.1 - 144.8, 18) (102.5 - 102.3, 19) (34.9 - 35.0, 20) (55.9 - 56.4, 23)
4                                                                                SIM (173.4 S C5 +-3.0 Int) (168.3 S C4 +-0.7 Int) (134.0 S C6 +-2.4 Int) (121.8 T C11 +-0.1 2*) (72.9D C8 +-0.6 Int) (71.8 D C1 +-3.8 Int) (40.2 D C2 +-2.1 Int) (30.9 T C15 +-3.4 4300*) (29.2 T C18 +-3.0 4236*)(28.8 T C17 +-3.4 27891*) (28.5 T C16 +-3.1 1809*) (27.1 T C13 +-3.8 3*) (24.9 T C12 +-1.1 Int) (23.9 T C14 +-3.7 5242*) (14.7 Q C19 +-4.0 6903*)
5                                                                                SIM (187.0 S C2 +-4.3 96*) (181.9 S C7 +-1.5 192*) (164.9 S C16 +-1.4 31*) (164.1 S C10 +-1.443*) (162.8 S C9 +-0.5 11*) (161.0 S C6 +-1.9 26*) (135.9 S C5 +-9.8 217*) (135.9 S C4 +-9.8 217*) (121.7 S C8+-0.0 1*) (118.9 S C1 +-9.8 141*) (109.2 S C3 +-1.2 43*) (108.7 D C11 +-2.3 18*) (108.6 D C13 +-0.6 34*)(108.4 D C12 +-2.0 31*) (67.8 D C17 +-0.0 1*) (31.9 T C23 +-3.5 8*) (31.0 T C26 +-2.6 430*) (25.7 T C24 +-0.35*) (23.9 T C25 +-3.7 5242*) (14.7 Q C27 +-4.0 6903*)
6                                                                                SIM (171.5 S C2 +-1.0 Int) (170.0 S C5 +-1.5 Int) (133.8 S C6 +-0.7 Int) (124.0 T C11 +-0.0 Int) (79.3D C8 +-1.1 Int) (74.0 D C3 +-1.4 Int) (47.3 D C1 +-7.9 Int) (30.2 T C12 +-0.3 Int) (27.1 T C13 +-0.1 4*) (23.1 TC14 +-4.4 148*) (14.7 Q C15 +-4.0 6903*)
                     C.NMR.Struct
1                   simulated ...
2                   simulated ...
3 simulated ...; experimental ...
4                   simulated ...
5                   simulated ...
6                   simulated ...
                                                                                H.NMR
1
2
3 CDCl3: (2.56, H4) (3.34, H5) (6.38, H9) (6.75, J=7.0, H13) (4.72, J=7.0, 3.0, H14) (5.42, J=3.0,3.0,H15) (6.40, H16) (3.93, H17)
4
5                                                                                [3513]
6
                                                       MS.Spectra UV.A UV.B
1
2
3 (312, 100%, M+) (284) (269) (256) (241) (227) (199) (185) (171)
4
5
6
                                                                                UV.N
1
2
3 MeOH: (220, 25600) (265, 13400) (362, 21800) (EtOH): (223, 25600) (265, 13400) (362, 21800)
4                                                                          MeOH: (210, 10000)
5
6                                                                          MeOH: (210, 1OOOO)
                                       UV
1
2
3 220 265 362 ...; 223 265 362 ...; light
4                                 210 ...
5
6                                 210 ...
                                                                   IR.Spectra
1
2
3 KBr (1754) (1701) (1615) (1595) (1429) (1356) (1229) (1130) (977) (824) ...
4
5
6
                       Toxicity                            Solubility
1
2
3 LD50 = (1, peros) hepatotoxic      good in MeOH, Chl, hardly in Hex
4                                     good in MeOH, Et2O, hardly in W
5
6                               good in EtOAc, Chl, hardly in W, base
                                                                 Activity
1
2
3 (B.subt., 15) (S.aureus, ) (Mycob.sp., ) (Fungi, 10) (Nocardia sp., 20)
4                              (B.subt., 200) (Phyt.fungi, 1)(antibiotic)
5                                                (bacteria, +) (fungi, -)
6                                                (Phyt.fungi, ) (Fungi, )
                                               Appearance    MeltingP                    TLC
1                                                                -271
2                                                         (175)-(180)
3     fluorescence emission 425 nm; white, yellow, cryst.   (268-269)
4 (+)-form; also (-)-form, (+-)- form found white, cryst.      (54-6)
5                                                             (233-4) (0.48, EtOAc_cHex 1:1)
6                                           white, cryst.    (46-7.5)
      StructCalc                     Group
1 370.104704 ...
2 365.173393 ...
3 312.062840 ...        aflatoxin, neutral
4 266.151261 ... dilactone deriv., neutral
5 372.120355 ...
6 210.088660 ... dilactone deriv., neutral
                                                                      Remarks
1                                                   *C,H also (+-)-form found
2
3 *C (see H),H,I,M (see I),U EXP = 2nd val in CDCl3: C-OMe_COO were exchanged
4
5                                                                        *H,M
6                                                              also (+-)-form
                                                                                References
1                                                                                Thomson II, 487; Horak, R. et al., J. Chem. Soc., Perkin Trans. 1 (1985) 345
2                                                                                Williams, R. M. et al., J. Am. Chem. Soc., 111(8), 3064-5 1989
3 Cole_Cox, 15; Nature,192,1096,1961; 198,1056,1963; Endeavour 22,75,1963; JACS,85,1706, 1963;87, 882, 1965; Forsch., 31, 118, 1974; Exp., 23,187,1967; J. Bact.,93,59,1967; Appl. Micr.,14,403,1966; Z. Allg.Mikr.,12,593,1972; Bioch.J., 114,289,1969; Bact. Rev.,41, 822,1977;30,460,1966; CA,89,36786;CR Ser. D,285,201, 1978; AAC,16,277,1979
4                                                                                JCS,5385,1963; Nature,203,1382,1964; JACS,91,7208,1969;95, 7923,1973;97,3870,1975;JOC,38,2489,1973; CC,538,1973; Aust. J. Chem.,18,373,1965
5                                                                                Thomson II, 483; Townsend, Craig A., Tetrahedron Lett. 1986, 27(8), 887-8; Turner II, 187,188, 191
6                                                                                TL,727,1968,3233,1978; Tsuboi, S. et al., J. Org. Chem., 51 (1986) 4944
                                 CA                                REG
1                          DA:A-915             28458-24-4; 73346-80-2
2  DA:B-138; 120:186930; 110:189072                         23402-09-7
3 DA:A-096; 108:218732k; 114:97857t                          1162-65-8
4                          DA:A-904 26057-70-5; 16993-42-3; 20223-76-1
5             DA:A-905; 105:133600d                          5803-62-3
6                          DA:C-013                         20421-31-2
                                                                                ChemClass
1  no charge; oxygen heterocycle; carbocycle; aromatic; alicycle; large ring; fused rings; 6ring;
2       no charge; nitrogen heterocycle; carbocycle; aromatic; alicycle; large ring; fused rings;
3  no charge; oxygen heterocycle; carbocycle; aromatic; alicycle; large ring; fused rings; 5ring;
4 no charge; oxygen heterocycle; alicycle; large ring; fused rings; 5ring; 8ring; ester; lactone;
5        no charge; carbocycle; aromatic; large ring; fused rings; 6ring; 10ring; 14ring; ketone;
6 no charge; oxygen heterocycle; alicycle; large ring; fused rings; 5ring; 8ring; ester; lactone;
                                               Opt.Rot X.1
1
2                                    aD25: (+413 EtOH)
3 (-480, DMF) (-559, Chl); aD25 (-562, c=0.115, CHCL3)
4                        aD25:(-41.6, Chl) (-41, EtOH)
5                            aD22 (-178, c 0.37, EtOH)
6                                       aD:(-141, Chl)

Thanks in advance

A: If you remove those trailing periods from the character vector StructCalc you should get success:
StructCalc <- as.numeric( gsub("[ ][.]+", "", StructCalc) )

If you take out all the periods, then you loose the "decimal place".
> sc <- scan(what="",sep=",")
1: 370.104704 ...
2: 365.173393 ...
3: 312.062840 ...
4: 266.151261 ...
5: 372.120355 ...
6: 210.088660 ...
7:
Read 6 items
> sub("[ ][.]+","",sc)
[1] "370.104704" "365.173393" "312.062840" "266.151261" "372.120355" "210.088660"
> as.numeric(sub("[ ][.]+","",sc))
[1] 370.1047 365.1734 312.0628 266.1513 372.1204 210.0887

> print( as.numeric(sub("[ ][.]+","",sc)), digits=16)
[1] 370.104704 365.173393 312.062840 266.151261 372.120355 210.088660

A: It looks like the three dots are the issue. You can clean it up with:
a = "1 ..."
as.numeric(a)
# Doesn't work #

b = gsub("[.]", "", a)
as.numeric(b)
# works #

redpajama_set_name: RedPajamaStackExchange


text:
Photo, Print, Drawing A society of patriotic ladies, at Edenton in North Carolina
[ digital file from original print ]
Download: JPEG (5.5 KB) GIF (16.1 KB) JPEG (51.3 KB) JPEG (133.3 KB) TIFF (76.1 MB)
[ digital file from color film copy transparency ]
Download: JPEG (6.7 KB) GIF (16.5 KB) JPEG (52.9 KB) JPEG (162.3 KB) TIFF (4.9 MB)
[ digital file from b&w film copy neg. ]
Download: JPEG (5.3 KB) GIF (18.8 KB) JPEG (54.8 KB) TIFF (1.6 MB)
A society of patriotic ladies, at Edenton in North Carolina
Print shows satire of American women from Edenton, North Carolina, pledging to boycott English tea in response to Continental Congress resolution in 1774 to boycott English goods.
Robert Sayer and John Bennett (Firm), publisher
Dawe, Philip, artist
London : Printed for R. Sayer & J. Bennett, 1775 March 25.
- Women--Political activity--North Carolina--Edenton--1770-1780
- Tea--North Carolina--Edenton--1770-1780
- Boycotts--American--North Carolina--Edenton--1770-1780
- United States--History--Revolution, 1775-1783--Women
Cartoons (Commentary)--British--1770-1780.
Mezzotints--British--1770-1780.
Cartoons (Commentary)--British--1770-1780
Mezzotints--British--1770-1780
- Plate V.
- Attributed to P(hilip?) Dawe, BMC no. 5284B.
- Catalogue of prints and drawings in the British Museum. Division I, political and personal satires, v. 5, no. 5284
- Forms part of: British Cartoon Prints Collection (Library of Congress).
- Published in: The American Revolution in drawings and prints; a checklist of 1765-1790 graphics in the Library of Congress / Compiled by Donald H. Cresswell, with a foreword by Sinclair H. Hitchings. Washington : [For sale by the Supt. of Docs., U.S. Govt. Print. Off.], 1975, no. 681.
- Published in: Eyes of the nation : a visual history of the United States / Vincent Virga and curators of the Library of Congress ; historical commentary by Alan Brinkley. New York : Knopf, 1997.
- Published in: American women : a Library of Congress guide for the study of women's history and culture in the United States / edited by Sheridan Harvey ... [et al.]. Washington : Library of Congress, 2001, p. 183.
- Exhibited: "Steeped in History : The Art of Tea" at the Fowler Museum, University of California, Los Angeles, 2009.
1 print : mezzotint.
Call Number/Physical Location
PC 1 - 5284B (A size) [P&P]
Library of Congress Prints and Photographs Division Washington, D.C. 20540 USA http://hdl.loc.gov/loc.pnp/pp.print
ppmsca 19468 //hdl.loc.gov/loc.pnp/ppmsca.19468
cph 3g04617 //hdl.loc.gov/loc.pnp/cph.3g04617
cph 3a15070 //hdl.loc.gov/loc.pnp/cph.3a15070
Library of Congress Control Number
Reproduction Number
LC-DIG-ppmsca-19468 (digital file from original print) LC-USZC4-4617 (color film copy transparency) LC-USZ62-12711 (b&w film copy neg.) LC-USZCN4-208 (color film copy neg.)
Rights Advisory
No known restrictions on publication.
https://lccn.loc.gov/96511606
MARCXML Record
MODS Record
Dublin Core Record
American Women: A Gateway to Library of Congress Resources for the Study of Women's History and Culture in the United States (269)
Cartoon Prints, British (984)
Prints and Photographs Division (1,028,255)
Library of Congress Online Catalog (1,359,292)
Photo, Print, Drawing
Dawe, Philip
Cartoons (Commentary)
Mezzotints
The American Revolution - John Bull and Uncle Sam: Four Centuries of British-American Relations
The Library of Congress believes that many of the papers in the British Cartoon Prints collection are in the public domain or have no known copyright restrictions and are free to use and reuse. Researchers should watch for documents that may be copyrighted (for example, published in the United States less than 95 years ago, or unpublished and the author died less than 70 years ago).
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Credit Line: Library of Congress, Prints and Photographs Division, Cartoon Prints, British.
Rights Advisory: No known restrictions on publication.
Reproduction Number: LC-DIG-ppmsca-19468 (digital file from original print) LC-USZC4-4617 (color film copy transparency) LC-USZ62-12711 (b&w film copy neg.) LC-USZCN4-208 (color film copy neg.)
Call Number: PC 1 - 5284B (A size) [P&P]
Access Advisory: ---
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Robert Sayer And John Bennett , Publisher, and Philip Dawe. A society of patriotic ladies, at Edenton in North Carolina . United States Edenton North Carolina, 1775. London: Printed for R. Sayer & J. Bennett. Photograph. https://www.loc.gov/item/96511606/.
Robert Sayer And John Bennett, P. & Dawe, P. (1775) A society of patriotic ladies, at Edenton in North Carolina . United States Edenton North Carolina, 1775. London: Printed for R. Sayer & J. Bennett. [Photograph] Retrieved from the Library of Congress, https://www.loc.gov/item/96511606/.
Robert Sayer And John Bennett , Publisher, and Philip Dawe. A society of patriotic ladies, at Edenton in North Carolina . London: Printed for R. Sayer & J. Bennett. Photograph. Retrieved from the Library of Congress, <www.loc.gov/item/96511606/>.
The patriotick barber of New York, or the Captain in the suds 1 print : mezzotint ; 35.3 x 25 cm (plate), 42.2 x 27.4 cm (sheet) | Cartoon shows a New York barber refusing to finish shaving a customer after learning of his...
Contributor: Dawe, Philip - Robert Sayer and John Bennett (Firm)
The alternative of Williams-burg 1 print : mezzotint ; 36.9 x 27.7 cm. | Print shows a "Virginian loyalist" being forced to sign a document, possibly issued by the Williamsburg Convention, by a club-wielding mob of...
The Bostonian's paying the excise-man, or tarring & feathering 1 print : mezzotint. | Print shows five men forcing a tarred and feathered customs officer to drink from a teapot, a bucket and a liberty cap are on the ground at...
Contributor: Robert Sayer and John Bennett (Firm)
The Bostonians in distress 1 print : mezzotint. | Print shows Bostonians held captive in a cage suspended from the "Liberty Tree." Three British sailors standing in a boat feed them fish from a basket labeled...
The able doctor, or, America swallowing the bitter draught 1 print : etching. | Cartoon shows Lord North, with the "Boston Port Bill" extending from a pocket, forcing tea (the Intolerable Acts) down the throat of a partially draped Native female...
The Seat of war in New England, by an American volunteer, with the marches of the ... Scale ca. 1:450,000. Hand colored. Prime meridian: Boston. Relief shown by hachures. Includes "Plan of Boston Harbour, from an actual survey" and "Plan of the town of Boston with the attack on...
The historic tea-party of Edenton, A digital reproduction made from a copy held by the University of Michigan is available from the University of Michigan's Making of America Web site.
Contributor: Dillard, Richard
The historic tea-party of Edenton, October 25th, 1774. An incident in North Carolina connected with British ... Also available in digital form.
The seat of action, between the British and American forces; or, An authentic plan of the ... Scale ca. 1:215,000. Hand colored. Has watermarks. LC Maps of North America, 1750-1789, 1146 Available also through the Library of Congress Web site as a raster image. Vault AACR2
Contributor: Holland, Samuel - Robert Sayer and John Bennett (Firm)
A general map of the middle British colonies, in America. Containing Virginia, Maryland, the Delaware counties, ... Scale ca. 1:2,300,000. Hand colored. Relief shown pictorially. "The seat of the war in the middle British colonies, containing Virginia, Maryland, the Delaware counties, &ca." From the author's The American military pocket...
Contributor: Pownall, Thomas - Robert Sayer and John Bennett (Firm)


text:
Extinct Attractions, Disney California Adventure, Themed areas in Disney parks
2012 (banner name disbanded)
Grizzly Peak Airfield
Golden State was one of Disney California Adventure's original four themed areas, or districts. The sprawling area was divided into six sub-areas, which were themed around several aspects of California and its history: its aviation history (Condor Flats), its national parks (Grizzly Peak Recreational Area), its agricultural industry (Bountiful Valley Farm), its wine industry (Golden Vine Winery), San Francisco (The Bay Area), and Monterey's Cannery Row (Pacific Wharf). Parts of the area were transferred to other lands over the years, and the name was retired in 2012.
The original area of Golden State included all of present-day Grizzly Peak, Pacific Wharf, and Condor Flats, and portions of present-day Paradise Pier, A Bug's Land, and Cars Land.
1 Former Attractions
2 Attractions Open Today
3 Former Restaurants
4 Former Shops
Former Attractions
Golden Dreams (2001–2008)
Mission Tortilla Factory (2001–2011)
Seasons of the Vine (2001–2008)
Attractions Open Today
The Bakery Tour (2001-) (relocated to Pacific Wharf)
Grizzly River Run (2001-) (Also Parts of Grizzly Peak)
Redwood Creek Challenge Trail (2001-) (Also Parts of Grizzly Peak)
Soarin' Around the World (2001-) (Also Parts of Grizzly Peak)
Walt Disney Imagineering Blue Sky Cellar (2008-) (relocated to Pacific Wharf)
Former Restaurants
Taste Pilot's Grill (2001-2015)
Former Shops
Condor Flats Fly 'n' Buy
Red Car Trolley
Disney Animation Building (Animation Academy • Turtle Talk with Crush) • Disney Junior Dance Party! • Monsters, Inc. Mike & Sulley to the Rescue! • Mickey's PhilharMagic
Grizzly River Run • Redwood Creek Challenge Trail • Soarin' Around the World
Seasonal: Villains Grove
Pacific Wharf
The Bakery Tour • Walt Disney Imagineering Blue Sky Cellar
Radiator Springs Racers • Mater's Junkyard Jamboree • Luigi's Rollickin' Roadsters
Seasonal: Haul-O-Ween • Mater's Graveyard JamBOOree • Luigi's Honkin' Haul-O-Ween • Mater's Jingle Jamboree
Paradise Gardens Park
Goofy's Sky School • Silly Symphony Swings • Golden Zephyr • Jumpin' Jellyfish • The Little Mermaid: Ariel's Undersea Adventure
Incredicoaster • Inside Out Emotional Whirlwind • Jessie's Critter Carousel • Pixar Pal-A-Round • Toy Story Midway Mania! • Games of Pixar Pier
Avengers Campus (Opening in 2021)
Avengers Quinjet (Opening in 2022) • The Sanctum (Opening in 2021) • Guardians of the Galaxy - Mission: BREAKOUT! • Web Slingers: A Spider-Man Adventure (Opening in 2021)
Seasonal: Guardians of the Galaxy - Monsters After Dark
Current Entertainment
Seasonal: Disney's Celebrate America • World of Color: Seasons of Light • World of Color: Villainous • Frightfully Fun Parade
Former Attractions and Entertainment
A Bug's Land (Flik's Flyers • Francis' Ladybug Boogie • Heimlich's Chew Chew Train • It's Tough to Be a Bug! • Princess Dot Puddle Park • Tuck & Roll's Drive 'Em Buggies) • Hyperion Theater (Aladdin: A Musical Spectacular • Frozen: Live at the Hyperion) • California Screamin' • Disney Junior - Live on Stage! • Golden Dreams • King Triton's Carousel of the Sea • Luigi's Flying Tires • Maliboomer • Mission Tortilla Factory • Muppet*Vision 3D • Paint the Night • Superstar Limo • The Twilight Zone Tower of Terror • Who Wants to Be a Millionaire – Play It! • S.S. Rustworthy • Disney's LuminAria • Disney's Electrical Parade • Disney's Eureka! A California Parade • Block Party Bash • Pixar Play Parade • Condor Flats (Paradise Pier • Golden State)
Seasonal: World of Color: Winter Dreams • World of Color: Celebrate! - The Wonderful World of Walt Disney
Disney's Grand Californian Hotel & Spa • Disney's Paradise Pier Hotel
Retrieved from "https://disney.fandom.com/wiki/Golden_State?oldid=4073300"
Extinct Attractions
Themed areas in Disney parks


text:
Santa Maria Assunta is a Renaissance-style, Roman Catholic parish church located in the town of Arrone, province of Terni, region of Umbria, Italy.

History
The church has a sober 15th-century white marble facade. The interior, including the apse. The interior contains various frescoes, including the following works:
Madonna del Rosario (1609) attributed to Giuseppe Bastiani
Madonna and Child with Saints Peter and John the Evangelist, attributed to Francesco Cozza
Annunciation, Adoration by Shepherds, Dormition of the Virgin, and Coronation of Virgin (1516) by Vincenzo Tamagni and Giovanni di Pietro da Spoleto
Frescoes in the apse (1544) by Jacopo Siculo
The main altar triptych by the Maestro di Arrone (1487) was stolen in 1971.

References

15th-century Roman Catholic church buildings in Italy
Churches in the province of Terni
Renaissance architecture in Umbria

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