A look into the viability of GOAs as type I chondrule precursor material within the new heating parameters of the fly by model.
\begin
Discover why over 20 million people worldwide trust Overleaf with their work.
%---------------------------------------------------------------------------
% PACKAGES AND OTHER DOCUMENT CONFIGURATIONS
%---------------------------------------------------------------------------
\documentclass[final]{beamer}
\usepackage{gensymb}
\usepackage{textcomp}
\usepackage[scale=1.24]{beamerposter} % Use the beamerposter package for laying out the poster
\usetheme{confposter} % Use the confposter theme supplied with this template
\setbeamercolor{block title}{fg=purple,bg=white} % Colors of the block titles
\setbeamercolor{block body}{fg=black,bg=white} % Colors of the body of blocks
\setbeamercolor{block alerted title}{fg=white,bg=purple} % Colors of the highlighted block titles
\setbeamercolor{block alerted body}{fg=black,bg=purple!10} % Colors of the body of highlighted blocks
% Many more colors are available for use in beamerthemeconfposter.sty
%---------------------------------------------------------------------------
% Define the column widths and overall poster size
% To set effective sepwid, onecolwid and twocolwid values, first choose how many columns you want and how much separation you want between columns
% In this template, the separation width chosen is 0.024 of the paper width and a 4-column layout
% onecolwid should therefore be (1-(# of columns+1)*sepwid)/# of columns e.g. (1-(4+1)*0.024)/4 = 0.22
% Set twocolwid to be (2*onecolwid)+sepwid = 0.464
% Set threecolwid to be (3*onecolwid)+2*sepwid = 0.708
\newlength{\sepwid}
\newlength{\onecolwid}
\newlength{\twocolwid}
\newlength{\threecolwid}
\setlength{\paperwidth}{48in} % A0 width: 46.8in
\setlength{\paperheight}{38.4in} % A0 height: 33.1in
\setlength{\sepwid}{0.024\paperwidth} % Separation width (white space) between columns
\setlength{\onecolwid}{0.22\paperwidth} % Width of one column
\setlength{\twocolwid}{0.464\paperwidth} % Width of two columns
\setlength{\threecolwid}{0.708\paperwidth} % Width of three columns
\setlength{\topmargin}{-0.75in} % Reduce the top margin size
%---------------------------------------------------------------------------
\usepackage{graphicx} % Required for including images
\usepackage{booktabs} % Top and bottom rules for tables
%---------------------------------------------------------------------------
% TITLE SECTION
%---------------------------------------------------------------------------
\title{The Flyby Model of Chondrule Formation: an Investigation into the Viability of
Granoblastic Olivine Aggregates as Type I Chondrule Precursor Material} % Poster title
\author{Ian K. Bania} % Author(s)
\institute{Department of Physics and Astronomy, Colgate University\\
Advisors: William Herbst, James P. Greenwood\\
Department of Astronomy and Department of Earth and Environmental Sciences, Wesleyan University} % Institution(s)
%----------------------------------------------------------------------------
\begin{document}
\addtobeamertemplate{headline}{}
{\begin{tikzpicture}[remember picture,overlay]
\node [shift={(-10cm,-11.5cm)}] at (current page.north east) {\includegraphics[height=7cm]{Colgate_University_Seal.png}};
\end{tikzpicture}
\begin{tikzpicture}[remember picture,overlay]
\node [shift={(-20cm,-11.5cm)}] at (current page.north east) {\includegraphics[height=7cm]{Wesleyan_University_Shield.png}};
\end{tikzpicture}
\begin{tikzpicture}[remember picture,overlay]
\node [shift={(-112.5cm,-11.5cm)}] at (current page.north east) {\includegraphics[height=7cm]{NASA_logo.png}};
\end{tikzpicture}
\begin{tikzpicture}[remember picture,overlay]
\node [shift={(-102.5cm,-11.5cm)}] at (current page.north east) {\includegraphics[height=7cm]{nsf_logo.png}};
\end{tikzpicture}}
\begin{frame}[t] % The whole poster is enclosed in one beamer frame
\begin{columns}[t] % The whole poster consists of three major columns, the second of which is split into two columns twice - the [t] option aligns each column's content to the top
\begin{column}{\sepwid}\end{column} % Empty spacer column
\begin{column}{\onecolwid} % The first column
%----------------------------------------------------------------------------
% LEFT
%---------------------------------------------------------------------------
\begin{block}{Introduction}
\small{Chondritic meteorites represent some of the oldest physical samples the scientific community currently has available to study, dating to just a few million years younger than the solar system. The $\sim.1 mm$ spheres known as chondrules are composed predominantly of silicates and account for a significant volume of their host chondrites. Chondrites are unique from other meteorites in that they are undifferentiated--in principle this means they have maintained the same composition and structure since their formation.}
\begin{figure}
\fbox{\includegraphics[width=0.8\linewidth]{accretion.jpg}}
\caption{Artist's impression of a molten planetesimal surrounded by debris. \cite{brandon}.}
\end{figure}
\small{One way chondrules are classified is by their iron oxide content, with FeO poor chondrules known as type I. Moreover type Ia chondrules are rich in Olivine, and type Ib in pyroxene. While 'nebular' models have fallen out of prevalence in favor of a 'planetary' ones, the question of chondrule formation is still a very open one. The \textbf{flyby model} proposes that chondrules are formed within small collections of pre-chondrule dust during close encounters with magmatically-active planetesimals. We attempt to show that during these close flybys, material is heated radiatively by exposure to liquid lakes of molten magma at the surface of radioactively heated planetesimals. Furthermore, I investigate granoblastic olivine aggregates' (\textbf{GOAs}) viability as type Ia chondrule precursor material within the heating and cooling constraints of the flyby model. \textbf{GOAs} are collections of olivine exhibiting anhedral, phaneritic and equigranular texture. In my experiments I use 100hr sintered olivine as an analogue for \textbf{GOAs} within precursor material.}
\begin{figure}
\includegraphics[width=0.9\linewidth]{planE.pdf}
\caption{Plan E heating curve, used to simulate the 'flyby' of a molten planetesimal.}
\end{figure}
\end{block}
%----------------------------------------------------------------------------
\end{column} % End of the first column
\begin{column}{\sepwid}\end{column} % Empty spacer column
\begin{column}{\twocolwid} % Begin a column which is two columns wide (column 2)
%----------------------------------------------------------------------------
% MIDDLE
%----------------------------------------------------------------------------
\begin{alertblock}{SEM Imaging}
\begin{figure}
\fbox{\includegraphics[width=0.35\linewidth]{_1_1.png}}
\fbox{\includegraphics[width=0.35\linewidth]{_1_2.png}}
\fbox{\includegraphics[width=0.35\linewidth]{_2_1.png}}
\fbox{\includegraphics[width=0.35\linewidth]{_2_3.png}}
\caption{Backscattered electron imaging, each site with three points of elemental analysis. Top: sample{[1]}, without iron. Bottom: sample{[2]}, with iron.}
\end{figure}
\end{alertblock}
%----------------------------------------------------------------------------
\begin{columns}[t,totalwidth=\twocolwid] % Split up the two columns wide column again
\begin{column}{\onecolwid} % The first column within column 2 (column 2.1)
%----------------------------------------------------------------------------
%----------------------------------------------------------------------------
\begin{block}{Experimental Methodology}
\small{In order to simulate a $7.5 km$ orbital encounter with a completely molten planetesimal of radius $100 km$, surface temperature $2150 K$, and density $3 g\cdot cm^{3}$, I used a Deltech VT-31 tube furnace to heat two charges ({[1]} and {[2]}) contained in platinum tubes up to peak temperatures of $\sim1650 K$. These heating parameters are known as 'Plane E'. The identical samples were composed of a 1:1 combination of \textbf{San Carlos olivine} which had been ground to $<43 \mu m$, pressed into $\sim6 mm$ disks and sintered for 100 hours at $1350\degree C$ and then broken into pieces, and a 3:7 mix of \textbf{plagioclase} and \textbf{Bamble enstatite}, ground to $<63 \mu m$. For sample{[2]}, $\%10$ iron fillings were added by weight.}
\begin{figure}
\fbox{\includegraphics[width=0.48\linewidth]{sinter.JPG}}
\fbox{\includegraphics[width=0.48\linewidth]{material.jpg}}
\caption{Left: San Carlos olivine, crushed after sintering at $1350\degree C$ for 100 hours. Right: 4x optical microscope image of the components of sample{[2]}: Ol., iron, Pl.+En. mix.}
\end{figure}
\end{block}
%----------------------------------------------------------------------------
\end{column} % End of column 2.1
\begin{column}{\onecolwid} % The second column within column 2 (column 2.2)
%----------------------------------------------------------------------------
%----------------------------------------------------------------------------
\begin{block}{Results}
\begin{table}
\begin{tabular}{l l l l l l l l l}
\toprule
\textbf{Point } & \textbf{O} & \textbf{Mg} & \textbf{Si} & \textbf{Fe} & \textbf{Ni} & \textbf{Al} & \textbf{Ca} & \textbf{Sr}\\
\midrule
{[1]}1a & 51.28 & 28.84 & 16.57 & 2.31 & - & - & - & - \\
{[1]}1b & 61.60 & 2.78 & 25.98 & - & - & 6.53 & 3.12 & - \\
{[1]}1c & 51.09 & 29.48 & 16.43 & 2.99 & - & - & - & - \\
{[1]}2a & 60.12 & 5.71 & 21.01 & 3.42 & - & 5.35 & 2.73 & 1.66 \\
{[1]}2b & 55.71 & 27.50 & 16.79 & - & - & - & - & - \\
{[1]}2c & 53.80 & 19.70 & 21.92 & 4.58 & - & - & - & - \\
{[2]}1a & 54.33 & 29.28 & 16.39 & - & - & - & - & - \\
{[2]}1b & 61.63 & 3.62 & 22.52 & 1.90 & - & 5.69 & 2.97 & 1.66 \\
{[2]}1c & - & - & - & 90.63 & 9.37 & - & - & - \\
{[2]}3a & 55.27 & 25.27 & 19.46 & - & - & - & - & - \\
{[2]}3b & 61.61 & 3.44 & 23.26 & 1.41 & - & 5.59 & 2.86 & 1.82 \\
{[2]}3c & 54.36 & 27.98 & 14.33 & 2.19 & - & - & - & 1.14 \\
\bottomrule
\end{tabular}
\caption{Elemental compositions for point samples by atomic percent.}
\end{table}
\small{After heating, charges were thin sectioned, mounted polished, and analyzed using \textbf{backscattered electron imaging}. Within both samples, both composition and texture vary to the extreme based on location within the chondrule. Furthermore the sintered olivine did not fully melt and diffuse into the rest of the sample.}
\end{block}
%----------------------------------------------------------------------------
\end{column} % End of column 2.2
\end{columns} % End of the split of column 2
\end{column} % End of the second column
\begin{column}{\sepwid}\end{column} % Empty spacer column
\begin{column}{\onecolwid} % The third column
%----------------------------------------------------------------------------
% RIGHT
%----------------------------------------------------------------------------
\begin{block}{Discussion}
\small{These results show that with these heating parameters, \textbf{GOAs} are not a possible type Ia chondrule precursor within the \textbf{flyby model}. However, it is still possible that given longer heating and higher peak temperatures, \textbf{GOAs} could still fill this role. Within the \textbf{flyby model} it is possible to achieve this with closer encounters and larger planetesimal radii.}
\begin{figure}
\fbox{\includegraphics[width=0.48\linewidth]{sample1.png}}
\fbox{\includegraphics[width=0.48\linewidth]{sample2.png}}
\caption{4x optical microscope images of sample{[1]} (left), and sample{[2]} (right).}
\end{figure}
\end{block}
%----------------------------------------------------------------------------
% REFERENCES
%----------------------------------------------------------------------------
\begin{block}{References}
\nocite{*} % Insert publications even if they are not cited in the poster
\small{\bibliographystyle{unsrt}
\bibliography{ian.bib}}
\end{block}
%----------------------------------------------------------------------------
% ACKNOWLEDGEMENTS
%----------------------------------------------------------------------------
\begin{block}{Acknowledgements}
\small{\rmfamily{Dr. Greenwood, Mr. Zareski and Dr. Herbst were all crucial for this project. I am very grateful of them for their invaluable direction and mentorship. Moreover I am very thankful towards the Keck Northeast Astronomy Consortium for providing me with this research opportunity and the accompanying funding. Finally, this work would not have been possible without the Emerging Worlds research grant from NASA.}} \\
\end{block}
%----------------------------------------------------------------------------
%----------------------------------------------------------------------------
\begin{alertblock}{Contact Information}
\begin{itemize}
\item Observatory: \href{http://observatory.colgate.edu/}{http://observatory.colgate.edu/}
\item Web: \href{http://www.colgate.edu/academics/departments-and-programs/physics-astronomy}{http://www.colgate.edu/academics/\\
departments-and-programs/physics-astronomy}
\item Email: \href{mailto:ibania@colgate.edu}{ibania@colgate.edu}
\end{itemize}
\end{alertblock}
%----------------------------------------------------------------------------
\end{column} % End of the third column
\end{columns} % End of all the columns in the poster
\end{frame} % End of the enclosing frame
\end{document}