[showyourwork] overleaf sync

src/tex/ms.tex

@@ -45,18 +45,6 @@
 \section{Introduction}
 \label{sec:intro}
 
-\begin{figure}[ht!]
-    \script{random_numbers.py}
-    \begin{centering}
-        \includegraphics[width=\linewidth]{figures/random_numbers.pdf}
-        \caption{
-            Plot showing a bunch of random numbers.
-        }
-        \label{fig:random_numbers}
-    \end{centering}
-\end{figure}
-
-
 Coronal loop models to date have fixed the elemental abundances both in space and time, using typically coronal abundances in quiescent loops or photospheric abundances in flare loops.  These abundances are used to calculate the bolometric radiative loss rate that directly impacts the cooling of the plasma.  Many recent X-ray observations of flares, however, clearly show that elemental abundances are not fixed and vary with time over the duration of the flare \citep{mondal2021, delzanna2021, mithun2022, nama2023, suarez2023, woods2023, rao2023, kepa2023}.  Similar observations have also found that the abundances of active regions (ARs) vary relatively quickly as well \citep{mondal2023}.
 
 There are two general mechanisms that could likely cause the change in elemental abundances: (1) preferential acceleration of ions, not neutrals, in the chromosphere, and (2) flows.