% DPSFORM.TEX -- DPS meeting abstract electronic form.
% Last Updated 27 JUNE 2002 JMJ

% DON'T remove the following comment; it identifies the form.
%
% Division for Planetary Sciences electronic abstract form.

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\documentstyle[11pt,aasab]{article}
\pagestyle{empty}
\meetingid{DPS02} 

% Style file is available at:
% http://www.aas.org/publications/baas/aasab.sty

% The following line ("\input epsf") is REQUIRED if you are 
% including an encapsulated PostScript file in your abstract, 
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%\runningident{}
%\session{0.00}
%\datesubmitted{}

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%  2.   contributed - strongly prefer ORAL
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\presentationtype{2}     % REQUIRED

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% first author should be spelled out between the braces 
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\firstname{Leslie}            % REQUIRED
\lastname{Young}             % REQUIRED

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\memberid{19570}		% REQUIRED 

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%\sponsor{}             % REQUIRED FOR NONMEMBERS

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\correspondentaddress{Southwest Research Institute\\1050 Walnut St. Suite 426\\B
oulder CO 80302} % REQUIRED

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\authorphone{303-546-6057}          % REQUIRED
       
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\sessionchair{yes}        % OPTIONAL

% Please indicate your membership status in the Division
% for Planetary Sciences. This information is REQUIRED.
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%     Options are:
%     1.    MEMBER of DPS
%     2.    NONmember (this must be your first time 
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\mailto{layoung@boulder.swri.edu}      %OPTIONAL

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% by the Web processing software as a URL, not as a
% LaTeX string.

%\URL{}	%OPTIONAL

% The next line ("\begin{document}") tells LaTeX that 
% you are ready to start typing in your abstract information.  
% DO NOT DELETE THIS LINE!

\begin{document}

% Now you can input the information dealing with the scientific
% content of your abstract.  The DPS category code is the numeric
% identification of the subject matter; it is used by the program
% organizers to keep related papers in sessions together.
% Choices are:
%
%     1.  Special Session on Mars Odyssey (invited)
%     2.  Mercury
%     3.  Venus
%     4.  Moon
%     5.  Mars: Atmosphere
%     6.  Mars: Surface, Interior, Satellites
%     7.  Asteroids: Discovery and Dynamics
%     8.  Asteroids: Physical Studies
%     9.  Outer planets: Atmospheric Dynamics, Clouds
%    10.  Outer planets: Chemistry, Thermal Structure
%    11.  Outer planets: Aurorae and Magnetospheres
%    12.  Io: Surface,Atmosphere, and Torus
%    13.  Europa: Surface,Atmosphere, and Torus
%    14.  Other Jovian Satellites
%    15.  Titan
%    16.  Planetary Rings
%    17.  Pluto, Charon and Triton
%    18.  Other Planetary Satellites
%    19.  Comets: Nuclei, Orbital Dynamics
%    20.  Comets: Comae, Tails, Solar Wind Interaction
%    21.  Centaurs and Kuiper Belt Objects
%    22.  Dust and Solar Wind
%    23.  Solar System Origin, Planet and Satellite Formation
%    24.  Extrasolar Planets and Systems
%    25.  Other Dynamics
%    26.  Laboratory Research
%    27.  Invited Talk
%    28.  Education
%    29.  Other (includes historical papers)
%    30.  Future Missions and Instruments (posters only)
%    31.  Laboratory investigations related to Cassini Mission

 
% Type in your ONE category code (the number only) between the 
% braces, e.g. "\sortcategory{5}". Note that Education, History
% and Invited Papers are exempt from the one paper per meeting
% rule.

\sortcategory{17}            % REQUIRED

% The title of your abstract should be typed in mixed case
% between the braces next to the word "\title", 
% e.g., "Large-Scale Topography on Main-Belt Asteroids."

\title{Triton's atmosphere in 1989: new lab data, new profiles}               % REQUIRED

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%
%    R.W. Milkey, D. K. Kovalsky (AAS), C.D. Biemesderfer (NOAO),
%    R.J. Hanisch (STScI), J.M. Johnson, Jr. (AAS), NICMOS Team
%
% would be specified like this:
%
%    \authorsurname{Milkey}
%    \authorgivenname{R.W.}
%    \authorsurname{Kovalsky}
%    \authorgivenname{D.K.}
%    \authoraffil{AAS}
%    \authorsurname{Biemesderfer}
%    \authorgivenname{C.D.}
%    \authoraffil{Seagoat}
%    \authorsurname{Hanisch}
%    \authorgivenname{R.J.}
%    \authoraffil{STScI}
%    \authorsurname{Johnson, Jr.}
%    \authorgivenname{J.M.}
%    \authoraffil{AAS}
%    \teamname{NICMOS}
%    \teamtype{Team}
%
%  If you are the sole author of the abstract, your author list
%  would look like this:
%
%     \authorsurname{Binzel}
%     \authorgivenname{R.P.}
%     \authoraffil{MIT}
%
%  Type in your author, affiliation and team information below, 
%  in the braces. Note that you can add in as many "\author" 
%  "\affil" and "\team" lines as it takes to complete your author list.

\authorsurname{Young}
\authorgivenname{L.A.}
\authoraffil{SwRI}

\authorsurname{Stark}
\authorgivenname{G.}
\authoraffil{Wellesley College}

\authorsurname{Vervack, Jr.}
\authorgivenname{R.J.}
\authoraffil{JHU/APL}

%\teamname{}
%\teamtype{}

% The abstract itself belongs in a LaTeX abstract environment, which is
% set up by these two statements.
%
%    \begin{abstract}
%    \end{abstract}
%
%  DO NOT DELETE THESE TWO LINES!

\begin{abstract}

When Voyager 2 flew by Triton in 1989, it observed a warm ($\sim$100\ K)
thermosphere near altitudes of $\sim$450-700 km from N$_2$ continnuum absorption during the
UVS occultation (e.g., Broadfoot et al. 1989 Science 246, 1459), and a colder
($\sim$38 K) lower atmosphere below $\sim$150 km from phase delay of the radio
occultation (e.g., Gurrola 1995, PhD Thesis, Stanford). Models have attempted to
bridge the missing 400 km, spanning four decades of pressure
 (e.g.,  Stevens et al. 1992 GRL 19, 669;
Yelle et al. 1991, Icarus 89, 347). The
observations needed to fill this 400-km altitude gap lie in the 80-100
nm region of the Voyager UVS occultation data, where N$_2$ bands dominate
the opacity. The line strengths were previously unavailable, but have
been recently measured.

Using N$_2$ ionization and dissociation cross sections (Heubner et
al. 1991 A\&SS 195, 1), N$_2$ photoabsorption cross sections
between 95.2 and 98.5 nm region (Stark et al. 1992 JCP 97, 4809;
Stark et al. 2000 ApJ 531, 321; Ubachs et al. 1997 Chem. Phys. Lett. 268, 201), and 
the X-band phase delay of the radio occultation (Gurrola 1995), we can derive 
line-of-sight number densities from 0-20 km and 140-740 km.  Four
absorption bands were included in the photoabsorption
cross section files: $b(3) \leftarrow X(0)$,
$b(4) \leftarrow X(0)$, $c_3(0) \leftarrow X(0)$, and $c'_4(0) \leftarrow X(0)$.
The cross section models
are based on band $f$-value measurements, line width measurements, Voigt
profiles, and H\"{o}nl-London factors.  

A preliminary profile suggests that the heating source in
Triton's middle and upper atmosphere occurs at a much lower
altitude than assumed by previous models.  Details of the modeling and
its implications will be discussed.


This work was funded by NASA Planetary Atmosphere grant NAG5-12023. 
\end{abstract}

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\end{document}

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