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%% Sample TeX file for the HRMS Dijon 2023 abstracts
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\documentclass[11pt]{article}

\usepackage{hrms}  %% Page settings, style ... for the HRMS abstract book.

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\title{LINE-BROADENING AND SHIFT RATES OF ALKALI-METAL VAPOR PERTURBED BY NOBLE GAS ATOMS}

%% Note that \author and \address macros must be paired.
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\author{\FirstName K. \LastName MYNENI,
  \FirstName J. N. \LastName BLAKELY}
\address{U.S. Army DEVCOM, Aviation and Missile Center, Charles M. Bowden Laboratory, Redstone Arsenal, AL 35898, USA}

%% The \FirstName and \LastName macros are mandatory for each author
%% to make sure that the author index is properly auto-generated.
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%% Add or remove \author and \address pair(s) below to suite your needs
\author{\FirstName N. F. \LastName ALLARD}
\address{GEPI, Observatoire de Paris, PSL Research University, UMR 8111, CNRS, Sorbonne Paris Cit\'e, 61, Avenue de l Observatoire, 75014 Paris, France,
and Institut d Astrophysique de Paris, UMR7095, CNRS, Universit\'e Paris VI, 98bis Boulevard Arago, 75014 Paris, France}

\author{\underline{\FirstName G. \LastName GUILLON}}
\address{Laboratoire Interdisciplinaire Carnot de Bourgogne, UMR6303, CNRS, Universit\'e de Bourgogne-Franche-Comt\'e, 9, Avenue Alain Savary, 21078 Dijon Cedex, France}

\author{\FirstName F. A. \LastName NARDUCCI}
\address{Department of Physics, Naval Postgraduate School, Monterey, CA 93943}

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%% Place below other \usepackage{ ... }, if you need other packages.
%% See http://www.tug.org/texlive/doc.html for a description of available packages.

%% The macros below will change the page head and foot.
%% Please, do not modify the content of the \fancyhead macro nor the \fancyfoot line.
\usepackage{fancyhdr}
\pagestyle{fancy}
\fancyhead[C]{{\footnotesize \textit{HRMS, 28th Colloquium, Dijon, France,
  Aug. 28 - Sept. 1, 2023}}}
\fancyfoot[C]{}
\renewcommand{\headrulewidth}{0.6pt}
\renewcommand{\footrulewidth}{0.6pt}

%% The hyperref package allows to include hyperlinks in a document.
%% See the instructions for abstract submission for more details.
%% WARNING: Make sure that this package comes LAST since it re-defines many LaTeX macros.
\usepackage[colorlinks=true,urlcolor=blue,linkcolor=blue,citecolor=blue]{hyperref}
\voffset -.65 cm

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\category {1,8}
\begin{document}

\maketitle  %% This will also build the list of author(s) and addresse(s).

%% Index macro(s): see the abstract samples and the instructions
%% Remove the %% to account for the index item(s)
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%% Place the body of your abstract below.

The measurement and theory of the perturbation of radiation emitted or absorbed by an alkali-metal atom in the presence of a partial 
pressure of noble gas atoms has important applications both for precision-frequency microwave and optical sources needed for quantum 
sensing, and for the study of conditions in stellar atmospheres for certain types of white and brown dwarf stars, and exoplanets. 
Variation in the pressure and temperature of the ambient conditions prescribes the relevant theoretical model of atomic collisions for 
describing the effect on the emission profiles or absorption profiles of the alkali-metal atom's resonance lines. Under low pressures
of perturbing noble gas atoms, below 1bar, and at temperatures not far from room temperature, e.g. the conditions in alkali-metal vapor 
cells used as frequency standards, atomic collisions cause broadening and frequency shift of the resonance lines. In contrast, for a noble gas 
such as helium at pressures of hundreds of bars, and at temperatures of several thousand Kelvin, the shape of the spectral line wings are 
substantially modified. We report quantum scattering calculations, using ab initio interatomic potentials for the interaction of the 
alkali-metal $+$ noble gas atom, to obtain the temperature-dependence of the line broadening and shift rates for the sodium D1 and D2 resonance 
lines in the presence of helium (Na-He), and for the Rb D2 line in the presence of argon (Rb-Ar). We also compute the high-pressure, 
high-temperature Na-He D2 resonance line shape, far into the wings, using a unified semi-classical theory, for comparison with observed spectral 
features from astrophysical sources.


\end{document}
