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\begin{document}

\title{Pluto-References}



\author[1]{cihat kurt}%
\affil[1]{Texas A\&M University}%


\vspace{-1em}



  
  \date{May 14, 2024}


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\sloppy


\subsection*{From~\hyperref[csl:1]{(Cheng et al., 2017)}}

{\label{916329}}\par\null

New Horizons re- sults showed that the 1988 occultation light curve
inflection is pri- marily explained by the thermal gradient model: the
steep near- surface temperature gradient ~2--5 K/km is present, the\selectlanguage{ngerman}
{Pluto ra-dius is 1189.9 ±0.4 km}, and\selectlanguage{english} th{e vertical optical depth of
Pluto haze is only ~0.013} ( Gladstone et al. 2016 )

\par\null

"The haze in Pluto's atmosphere is optically thin, with the

brightness approximated as

\par\null

\selectlanguage{english}\textbf{\emph{I/F = ~ P ( θ ) n σs/4 [?] (2 πRH) (1)}}

\par\null

( Gladstone et al., 2016 ) where P ( \selectlanguage{greek}θ\selectlanguage{english}) is scattering phase function at
phase angle \selectlanguage{greek}θ, \selectlanguage{english}n is number density of haze particles, \selectlanguage{greek}σ\selectlanguage{english}s is the scat-
tering cross section, R is Pluto radius, and H is scale height.

The phase function is a key diagnostic of physical properties including
size, shape, and composition (refractive index). The brightness ver- sus
phase angle is considered here, by comparing I / F obtained in back
scatter and forward scatter geometries as listed in Table 1 . As haze
can be accurately measured only off the limb of Pluto, these
observations were made over various locations on Pluto dur- ing the 19 h
time span of Table 1 . The phase function was com- piled using only haze
observations over the day side limb at simi- lar northern latitudes (
\textgreater{} 40 \selectlanguage{ngerman}°)."~

\textbf{Comment:~}So the haze phase function obtained here could be
accpeted to be in consistent to a degree with itself at different phase
angles, because as discussed in this paper there is spatial variation in
the haze distribution in plutos atmosphere.

\par\null

\emph{From Table 4 and equation 1 the haze properties are calulcated
based on the assumption that they are either spherical mie particles or
fractals aggregates of spheres. In eand equation 1 the haze properties
are calulcated based on the assumption that they are either spherical
mie particles or fractals aggregates of spheres.}~~

\par\null\selectlanguage{english}
\begin{figure}[H]
\begin{center}
\includegraphics[width=0.70\columnwidth]{figures/Annotation-2019-11-21-144148/Annotation-2019-11-21-144148}
\caption{{This is a caption
{\label{259258}}%
}}
\end{center}
\end{figure}

\emph{Either case, the haze properties are assumed to beconstant
througout the lowest 50 km of the atmosphere to find the best fitting
haze model to the observation. The figure 20 assumes spherical haze
particles whereas figure 21 assumes fractal aggregates.~}

\emph{}\selectlanguage{english}
\begin{figure}[H]
\begin{center}
\includegraphics[width=0.70\columnwidth]{figures/Annotation-2019-11-21-1441481/Annotation-2019-11-21-144843}
\caption{{This is a caption
{\label{945944}}%
}}
\end{center}
\end{figure}\selectlanguage{english}
\begin{figure}[H]
\begin{center}
\includegraphics[width=0.70\columnwidth]{figures/Annotation-2019-11-21-1441482/Annotation-2019-11-21-1441482}
\caption{{This is a caption
{\label{733171}}%
}}
\end{center}
\end{figure}

Although they concluded that the for the lowest altitudes ( where I/F
peaks) spherical particles fit better and for the rest aggregates fit
better than spherical particles, there is still a problem. They assumed
that the aggregates have a contstant fractal number, which is equal to
2. It is not realistic to assume a sudden change from fractal particles
to the spherical particles near the lowest haze layer. One possible
scenario is a gradual increase in the fractal number of haze particles
reaching near 3 near the surface. In another words, as the aggregates
grow they may become increasingly compact becoming spherical . Another
possibility, some material condenses over the surface of the aggregate
particles. Condenstation may increase towards the surface. Similar
mechanism also suggested for Titan's haze particle at the lowest 30 Km
of the Titan's atmosphere.~~

\subsection*{}

{\label{590546}}\par\null

\subsection*{From~\hyperref[csl:2]{(Gladstone \& Young, 2019)}}

{\label{590546}}

Pluto's atmosphere is most similar to Titan's---with the photochem-
istry of supervolatile nitrogen and hydrocarbons resulting in a kind of
factory for cold haze production

\subsection*{More Compact aggregates at lower
30km}

{\label{120582}}

"Lower down, the atmospheric temperature reaches a maximum of~~110 K
around 30 km altitude (Hinson et al., 2017). Some evolution as~haze
particles settle through this warm zone seems inevitable. The~
temperature is high enough to cause sublimation of more volatile
hydrocarbons and nitriles that condensed onto the haze particles higher~
up in the atmosphere, but only if they condensed rather than being~more
strongly adsorbed or even chemically bonded into the macro~molecular
tholin (e.g., Luspay-Kuti et al., 2017).~ Sublimation loss would~

shrink the haze particles and slow their settling, as well as modifying
their compositions by distilling off the more volatile constituents. 110
K~ also exceeds the zero pressure melting points of some of the
constituent hydrocarbon species, specifically C2H4 (104 K), C2H6 (90 K),
and C3H6~ (88 K). Unmelted species may partly dissolve into those that
do melt,~ and melting point depression can be expected in such mixtures
(for instance, the CH4eC2H6 eutectic melting point is 18 K below the
melting points of the pure species; Hanley et al. (2017)). Partial
melting~ could allow particles to evolve from fractal aggregate shapes
into more~ compacted spherical forms, due to surface tension, with
implications~ for their scattering properties and settling rates. Warmed
haze particles~ might also be more sticky and could coalesce into even
larger aggregates if they contact one another."

\selectlanguage{english}
\FloatBarrier
\section*{References}\sloppy
\phantomsection
\label{csl:1}{Haze in Pluto{\textquotesingle}s atmosphere}. (2017). \textit{Icarus}, \textit{290}, 112–133. \url{https://doi.org/10.1016/j.icarus.2017.02.024}

\phantomsection
\label{csl:2}{New Horizons Observations of the Atmosphere of Pluto}. (2019). \textit{Annual Review of Earth and Planetary Sciences}, \textit{47}(1), 119–140. \url{https://doi.org/10.1146/annurev-earth-053018-060128}

\end{document}

