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references.bib
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@MISC{McClintock1993-fu,
title = "Optical design of the Ultraviolet Imaging Spectrograph for the
Cassini mission to Saturn",
author = "McClintock, William E",
journal = "Optical Engineering",
volume = 32,
number = 12,
pages = "3038",
year = 1993,
doi = "10.1117/12.149177"
}
@INCOLLECTION{Esposito2004-kr,
title = "The Cassini Ultraviolet Imaging Spectrograph Investigation",
booktitle = "The {Cassini-Huygens} Mission: Orbiter Remote Sensing
Investigations",
author = "Esposito, Larry W and Barth, Charles A and Colwell, Joshua E and
Lawrence, George M and McClintock, William E and Stewart, A I A
N F and Uwe Keller, H and Korth, Axel and Lauche, Hans and
Festou, Michel C and Lane, Arthur L and Hansen, Candice J and
Maki, Justin N and West, Robert A and Jahn, Herbert and Reulke,
Ralf and Warlich, Kerstin and Shemansky, Donald E and Yung, Yuk
L",
editor = "Russell, Christopher T",
abstract = "The Cassini Ultraviolet Imaging Spectrograph (UVIS) is part of
the remote sensing payload of the Cassini orbiter spacecraft.
UVIS has two spectrographic channels that provide images and
spectra covering the ranges from 56 to 118 nm and 110 to 190 nm.
A third optical path with a solar blind CsI photocathode is used
for high signal-to-noise-ratio stellar occultations by rings and
atmospheres. A separate Hydrogen Deuterium Absorption Cell
measures the relative abundance of deuterium and hydrogen from
their Lyman-$\alpha$ emission. The UVIS science objectives
include investigation of the chemistry, aerosols, clouds, and
energy balance of the Titan and Saturn atmospheres; neutrals in
the Saturn magnetosphere; the deuterium-to-hydrogen (D/H) ratio
for Titan and Saturn; icy satellite surface properties; and the
structure and evolution of Saturn's rings.",
publisher = "Springer Netherlands",
pages = "299--361",
year = 2004,
url = "https://doi.org/10.1007/1-4020-3874-7_5",
address = "Dordrecht",
isbn = "9781402038747",
doi = "10.1007/1-4020-3874-7\_5"
}
% The entry below contains non-ASCII chars that could not be converted
% to a LaTeX equivalent.
@ARTICLE{Ajello2005-jz,
title = "The Cassini Campaign observations of the Jupiter aurora by the
Ultraviolet Imaging Spectrograph and the Space Telescope Imaging
Spectrograph",
author = "Ajello, Joseph M and Pryor, Wayne and Esposito, Larry and
Stewart, Ian and McClintock, William and Gustin, Jacques and
Grodent, Denis and G{\'e}rard, J-C and Clarke, John T",
abstract = "We have analyzed the Cassini Ultraviolet Imaging Spectrometer
(UVIS) observations of the Jupiter aurora with an auroral
atmosphere two-stream electron transport code. The observations
of Jupiter by UVIS took place during the Cassini Campaign. The
Cassini Campaign included support spectral and imaging
observations by the Hubble Space Telescope (HST) Space Telescope
Imaging Spectrograph (STIS). A major result for the UVIS
observations was the identification of a large color variation
between the far ultraviolet (FUV: 1100--1700 {\AA}) and extreme
ultraviolet (EUV: 800--1100 {\AA}) spectral regions. This change
probably occurs because of a large variation in the ratio of the
soft electron flux (10--3000 eV) responsible for the EUV aurora
to the hard electron flux (∼15--22 keV) responsible for the FUV
aurora. On the basis of this result a new color ratio for
integrated intensities for EUV and FUV was defined
(4$\pi$I1550--1620 {\AA}/4$\pi$I1030--1150 {\AA}) which varied by
approximately a factor of 6. The FUV color ratio
(4$\pi$I1550--1620 {\AA}/4$\pi$I1230--1300 {\AA}) was more stable
with a variation of less than 50\% for the observations studied.
The medium resolution (0.9 {\AA} FWHM, G140M grating) FUV
observations (1295--1345 {\AA} and 1495--1540 {\AA}) by STIS on
13 January 2001, on the other hand, were analyzed by a spectral
modeling technique using a recently developed high-spectral
resolution model for the electron-excited H2 rotational lines.
The STIS FUV data were analyzed with a model that considered the
Lyman band spectrum (B $\Sigma$u+1$\rightarrow$X$\Sigma$g+1) as
composed of an allowed direct excitation component (X
$\Sigma$g+1$\rightarrow$B$\Sigma$u+1) and an optically forbidden
component (X
$\Sigma$g+1$\rightarrow$EF,GK,HH\textasciimacron{},…$\Sigma$g+1
followed by the cascade transition
$\Sigma$g+1$\rightarrow$B$\Sigma$u+1). The medium-resolution
spectral regions for the Jupiter aurora were carefully chosen to
emphasize the cascade component. The ratio of the two components
is a direct measurement of the mean secondary electron energy of
the aurora. The mean secondary electron energy of the aurora
varies between 50 and 200 eV for the polar cap, limb and auroral
oval observations. We examine a long time base of Galileo
Ultraviolet Spectrometer color ratios from the standard mission
(1996--1998) and compare them to Cassini UVIS, HST, and
International Ultraviolet Explorer (IUE) observations.",
journal = "Icarus",
volume = 178,
number = 2,
pages = "327--345",
month = nov,
year = 2005,
url = "https://www.sciencedirect.com/science/article/pii/S0019103505002320",
keywords = "Spectroscopy; Jupiter magnetosphere; Jupiter atmosphere;
Ultraviolet observations",
issn = "0019-1035",
doi = "10.1016/j.icarus.2005.01.023"
}
@ARTICLE{Hansen2006-un,
title = "Enceladus' water vapor plume",
author = "Hansen, Candice J and Esposito, L and Stewart, A I F and Colwell,
J and Hendrix, A and Pryor, W and Shemansky, D and West, R",
abstract = "The Cassini spacecraft flew close to Saturn's small moon
Enceladus three times in 2005. Cassini's UltraViolet Imaging
Spectrograph observed stellar occultations on two flybys and
confirmed the existence, composition, and regionally confined
nature of a water vapor plume in the south polar region of
Enceladus. This plume provides an adequate amount of water to
resupply losses from Saturn's E ring and to be the dominant
source of the neutral OH and atomic oxygen that fill the
Saturnian system.",
journal = "Science",
volume = 311,
number = 5766,
pages = "1422--1425",
month = mar,
year = 2006,
url = "http://dx.doi.org/10.1126/science.1121254",
language = "en",
issn = "0036-8075, 1095-9203",
pmid = "16527971",
doi = "10.1126/science.1121254"
}
% The entry below contains non-ASCII chars that could not be converted
% to a LaTeX equivalent.
@PHDTHESIS{Steffl2005-te,
title = "The Io plasma torus during the Cassini encounter with Jupiter:
Temporal, radial and azimuthal variations",
author = "Steffl, Andrew Joseph",
editor = "Bagenal, Fran",
abstract = "During the Cassini spacecraft's flyby of Jupiter (1 October 2000
to 31 March 2001), the Ultraviolet Imaging Spectrograph (UVIS)
produced an extensive dataset consisting of several thousand
spectrally-dispersed images of the lo plasma torus. The temporal,
radial, and azimuthal variability of the to plasma torus during
this period are examined. The total EUV power radiated from the
torus is found to be ∼1.7 $\times$ 1012 W with variations of
25\%. Several events were observed during which the torus
brightened by 20\% over a few hours. Significant changes in the
composition of the torus plasma were observed between 1 October
2000 and 11 November 2000. The composition and electron
temperature of the torus plasma as a function of radial distance
were derived from a scale of the midnight sector of the torus.
The radial profile during the Cassini epoch shows significant
differences from the Voyager era. The Io torus is found to
exhibit significant azimuthal variations in ion composition. This
compositional variation is observed to have a period of 10.07
hours 1.5\% longer than the System III rotation period of
Jupiter. While exhibiting many similar characteristics, the
periodicity in the UVIS data is 1.3\% shorter than the ``System
IV'' period. The amplitude of the azimuthal variation of S II and
S IV varies between 5--25\% during the observing period, while
the amplitude of the variation of S III and O II remains in the
range of 2--5\%. The amplitude of the azimuthal compositional
asymmetry appears to be modulated by its location in System III
longitude. The observed temporal variability is reproduced by
models of the torus chemistry that include a factor of 3 increase
in the rate of oxygen and sulfur atoms supplied to the extended
neutral clouds that are the source of the torus plasma coupled
with a ∼35\% increase in the amount of riot electrons in the Io
torus. The observed azimuthal variability of the Io torus is well
matched by models incorporating a primary source of hot electrons
that slips 12.2°/day relative to the System III coordinate system
and a secondary source of hot electrons that remains fixed in
System III.",
year = 2005,
url = "https://colorado.idm.oclc.org/login?url=https://www.proquest.com/dissertations-theses/io-plasma-torus-during-cassini-encounter-with/docview/305005964/se-2",
address = "Ann Arbor, United States",
school = "University of Colorado at Boulder",
language = "en",
isbn = "9780542044076"
}