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\shorttitle{Updated Opacities for DSEP}
\shortauthors{Boudreaux et al.}
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\begin{document}

\title{Correlations between Ca II H\&K Emission and the Gaia M dwarf Gap}

\correspondingauthor{Emily M. Boudreaux}
\email{emily.m.boudreaux.gr@dartmouth.edu,\\emily@boudreauxmail.com}

\author[0000-0002-2600-7513]{Emily M. Boudreaux}
\affiliation{Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA}

\author[0000-0001-9828-3229]{Aylin Garcia Soto}
\affiliation{Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA}

\author[0000-0003-3096-4161]{Brian C. Chaboyer}
\affiliation{Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA}

\received{}
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\accepted{}
\submitjournal{ApJ}


\begin{abstract}
  The Gaia M dwarf gap, also known as the Jao Gap, is a novel feature
  discovered in the Gaia DR2 G vs. BP-RP color magnitude diagram. This gap
  represents a 17 percent decrease in stellar density in a thin magnitude band around the
  convective transition mass ($\sim 0.35 M_{\odot}$) on the main sequence.
  Previous work has demonstrated a paucity of Hydrogen
  Alpha emission coincident with the G magnitude of the Jao Gap in the solar
  neighborhood. The exact mechanism which results in this paucity is as of yet
  unknown; however, the authors of the originating paper suggest that it may
  be the result of complex variations to a star's magnetic topology driven by
  the Jao Gap's characteristic formation and breakdown of stars' radiative
  transition zones. We present a follow up investigating another widely used
  magnetic activity metric, Calcium II H\&K emission. Ca II H\&K activity
  appears to share a similar anomalous behavior as H$\alpha$ does near the Jao
  Gap magnitude. We observe an increase in star-to-star variation of magnetic
  activity near the Jao Gap. This increase may be due to stochastic disruptions
  to the magnetic field originating from the periodic mixing events
  characteristic of the convective kissing instabilities which drive the
  formation of the Jao Gap.

\end{abstract}

\keywords{Stellar Evolution (1599) --- Stellar Evolutionary Models (2046)}

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\acknowledgments{
  This work has made use of the NASA astrophysical data system (ADS). We would
  like to thank Elisabeth Newton, Aaron Dotter, and Gregory Feiden for their
  support and for useful discussion related to the topic of this paper.
  Additionally, we would like to thank Keighley Rockcliffe, Kara Fagerstrom,
  and Isabel Halstead for their useful discussion related to this work. We
  acknowledge the support of a NASA grant (No. 80NSSC18K0634). 
}
\acknowledgments

% \begin{acknowledgments}
% 	This work has made use of the NASA astrophysical data system (ADS). We
% 	would like to thank Elisabeth Newton, Aaron Dotter, and Gregory Feiden for
% 	their support and for useful discussion related to the topic of this paper.
% 	We would like to thank our reviewer for their critical eye and their
% 	guidance to investigate to effects of the mixing length on the Gap
% 	Location. Additionally, we would like to thank James Colgan and the Los
% 	Alamos T-1 group for their assistance with the OPLIB opacity tables and
% 	support for the public release of \texttt{pyTOPSScrape}. We acknowledge the
% 	support of a NASA grant (No. 80NSSC18K0634). 
% \end{acknowledgments}

\software{
	The Dartmouth Stellar Evolution Program (DSEP) \citep{Dotter2008},
	\texttt{BeautifulSoup} \citep{richardson2007beautiful},
	\texttt{mechanize} \citep{chandra2015python},
	\texttt{FreeEOS} \citep{Irwin2012},
	\texttt{pyTOPSScrape} \citep{Boudreaux22},
  \texttt{lightkurve} \citep{LightkurveCollaborationLightkurve2018},
  \texttt{stella} \citep{FeinsteinStella2020},
  \texttt{starspot} \citep{AngusRuthAngus2021,Angus2023}
}


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