F. J. Crary

University of Colorado at Boulder, Boulder, Colorado, United States

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Publications (214)574.54 Total impact

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    ABSTRACT: The Saturn auroral campaign carried out in the spring of 2013 used multiple Earth-based observations, remote-sensing observations from Cassini, and in situ-observations from Cassini to further our understanding of auroras at Saturn. Most of the remote sensing and Earth-based measurements are, by nature, not continuous. And, even the in situ measurements, while continuously obtained, are not always obtained in regions relevant to the study of the aurora. Saturn kilometric radiation, however, is remotely monitored nearly continuously by the Radio and Plasma Wave Science instrument on Cassini. This radio emission, produced by the cyclotron maser instability, is tightly tied to auroral processes at Saturn as are auroral radio emissions at other planets, most notably Jupiter and Earth. This paper provides the time history of the intensity of the radio emissions through the auroral campaign as a means of understanding the temporal relationships between the sometimes widely spaced observations of the auroral activity. While beaming characteristics of the radio emissions are known to prevent single spacecraft observations of this emission from being a perfect auroral activity indicator, we demonstrate a good correlation between the radio emission intensity and the level of UV auroral activity, when both measurements are available.
    Icarus 01/2015; DOI:10.1016/j.icarus.2015.01.003 · 2.84 Impact Factor
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    ABSTRACT: Interchange injections events are commonly observed by the Cassini spacecraft in the region between about 6 and 12 Rs (1Rs = 60268 km) and even frequently beyond. In this study, thirteen examples of interchange injection events are identified in Cassini/CAPS data under special conditions such that time-of-flight (TOF) mass spectra could be obtained from entirely within the events. Using the TOF data to separate the main ion species H+, H2+, and W+, approximate densities of each species are calculated under the assumption that all distributions were isotropic. The light-ion density ratios, H2+/H+, in the injection events are not discernibly different from those ratios in control intervals from the ambient plasma. However, the water-group ratio, W+/H+, is significantly lower than ambient. Comparison of the measured density ratios with the range of values observed throughout Saturn's magnetosphere indicates that values of W+/H+ that are as low as those observed within the injection events are found primarily beyond L ~ 14 (where L is the equatorial crossing distance, in Rs, of a dipole field line), indicating that the injection events are delivering plasma from the outer magnetosphere, at times traveling at least 6 Rs.
    Journal of Geophysical Research: Space Physics 11/2014; 119(12). DOI:10.1002/2014JA020489 · 3.44 Impact Factor
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    ABSTRACT: We investigate the complex interaction between Saturn's magnetosphere and Titan's upper ionosphere using ion data acquired by the Cassini Plasma Spectrometer (CAPS) during the T40 encounter. Bounds on ion-group abundances at altitudes between ~2733 and ~12,541 km are determined by fitting mass spectra with model functions derived from instrument calibration data. The spectra are dominated by H+, H2+, H3+, and two hydrocarbon groups with mass ranges 12–19 and 24–32 amu, respectively. Notably, this constitutes the first reported observation of H3+ in Titan's exosphere. These measurements are discussed in the context of data from the CAPS Electron Spectrometer (ELS) and Cassini's Ion and Neutral Mass Spectrometer (INMS), which fortuitously sampled the ionospheric outflow during the T40 encounter at altitudes between ~2225 and ~3034 km [Westlake et al., 2012]. The CAPS data reveal a composition that is constitutively similar to that sampled by INMS, with hydrocarbon ions first observed as far as ~11,000 km from Titan and increasing by more than an order of magnitude along Cassini's inbound trajectory. In addition, we juxtapose the CAPS ion data with numerical results from three different interaction models and show that it is consistent with the location of the field-draping boundary described by Ulusen et al. [2012] and the Saturnward ion tail predicted by Sillanpää et al. [2006].
    Journal of Geophysical Research: Space Physics 11/2014; 120(1). DOI:10.1002/2014JA020499 · 3.44 Impact Factor
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    ABSTRACT: We present observations of significant dynamics within two UV auroral storms observed on Saturn using the Hubble Space Telescope in April/May 2013. Specifically, we discuss bursts of auroral emission observed at the poleward boundary of a solar wind-induced auroral storm, propagating at ~330% rigid corotation from near ~01 h LT toward ~08 h LT. We suggest these are indicative of ongoing, bursty reconnection of lobe flux in the magnetotail, providing strong evidence that Saturn's auroral storms are caused by large-scale flux closure. We also discuss the later evolution of a similar storm, and show that the emission maps to the trailing region of an energetic neutral atom enhancement. We thus identify the auroral form with the upward field-aligned continuity currents flowing into the associated partial ring current.
    05/2014; 41(10). DOI:10.1002/2014GL060186
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    ABSTRACT: [1] The Cassini Langmuir Probe (LP) onboard the Radio and Plasma Wave Science experiment has provided much information about the Saturnian cold plasma environment since the Saturn Orbit Insertion in 2004. A recent analysis revealed that the LP is also sensitive to the energetic electrons (250–450 eV) for negative potentials. These electrons impact the surface of the probe and generate a current of secondary electrons, inducing an energetic contribution to the DC level of the current-voltage (I-V) curve measured by the LP. In this paper, we further investigated this influence of the energetic electrons and (1) showed how the secondary electrons impact not only the DC level but also the slope of the (I-V) curve with unexpected positive values of the slope, (2) explained how the slope of the (I-V) curve can be used to identify where the influence of the energetic electrons is strong, (3) showed that this influence may be interpreted in terms of the critical and anticritical temperatures concept detailed by Lai and Tautz (2008), thus providing the first observational evidence for the existence of the anticritical temperature, (4) derived estimations of the maximum secondary yield value for the LP surface without using laboratory measurements, and (5) showed how to model the energetic contributions to the DC level and slope of the (I-V) curve via several methods (empirically and theoretically). This work will allow, for the whole Cassini mission, to clean the measurements influenced by such electrons. Furthermore, the understanding of this influence may be used for other missions using Langmuir probes, such as the future missions Jupiter Icy Moons Explorer at Jupiter, BepiColombo at Mercury, Rosetta at the comet Churyumov-Gerasimenko, and even the probes onboard spacecrafts in the Earth magnetosphere.
    Journal of Geophysical Research: Space Physics 11/2013; 118(11). DOI:10.1002/2013JA019114 · 3.44 Impact Factor
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    ABSTRACT: Photochemically produced aerosols are common among the atmospheres of our solar system and beyond. Observations and models have shown that photochemical aerosols have direct consequences on atmospheric properties as well as important astrobiological ramifications, but the mechanisms involved in their formation remain unclear. Here we show that the formation of aerosols in Titan's upper atmosphere is directly related to ion processes, and we provide a complete interpretation of observed mass spectra by the Cassini instruments from small to large masses. Because all planetary atmospheres possess ionospheres, we anticipate that the mechanisms identified here will be efficient in other environments as well, modulated by the chemical complexity of each atmosphere.
    Proceedings of the National Academy of Sciences 02/2013; DOI:10.1073/pnas.1217059110 · 9.81 Impact Factor
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    ABSTRACT: We use measurements of the Cassini Plasma Spectrometer, the Magnetospheric Imaging Instrument and the Magnetometer of the Cassini spacecraft to analyse the structure and composition of the tail section of the induced magnetosphere of Saturn's moon, Titan. The orbital positions of the Titan flybys of Cassini are distributed over various Saturn Local Time regions, so the effects of multiple-source ionization can be studied. We included flybys TA-T78 into the analysis. For many of the encounters the position of the center of the tail differed from that derived from the nominal flow direction, depending on SLT. We compared this with hybrid simulations. We also examined how the different mass particles (m/q=1, 2, 16-19) were distributed in the tail section. During the many tail flybys Titan was close to the plasma sheet of Saturn (for example during T11, T15, T29, T36, T44) hence embedded in a tilted magnetic field and higher density plasma. The possible effects of the Kronian magnetodisk on Titan's tail are discussed.
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    ABSTRACT: Magnetic reconnection is an important process that occurs at the magnetopause boundary of Earth's magnetosphere because it leads to transport of solar wind energy into the system, driving magnetospheric dynamics. However, the nature of magnetopause reconnection in the case of Saturn's magnetosphere is unclear. Based on a combination of Cassini spacecraft observations and simulations we propose that plasma β conditions adjacent to Saturn's magnetopause largely restrict reconnection to regions of the boundary where the adjacent magnetic fields are close to anti-parallel, severely limiting the fraction of the magnetopause surface that can become open. Under relatively low magnetosheath β conditions we suggest that this restriction becomes less severe. Our results imply that the nature of solar wind-magnetosphere coupling via reconnection can vary between planets, and we should not assume that the nature of this coupling is always Earth-like. Studies of reconnection signatures at Saturn's magnetopause will test this hypothesis.
    Geophysical Research Letters 04/2012; 39(8):8103-. DOI:10.1029/2012GL051372 · 4.46 Impact Factor
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    ABSTRACT: We present observations of CAPS electron and ion spectra during Titan distant tail crossings by the Cassini spacecraft. In common with closer tail encounters, we identify ionospheric plasma in the tail. Some of the electron spectra indicate a direct magnetic connection to Titan's dayside ionosphere due to the presence of ionospheric photoelectrons. Ion observations reveal heavy and light ion populations streaming into the tail. Using the distant tail encounters T9, T75 and T63, we estimate total plasma loss rates from Titan via this process.
    Journal of Geophysical Research Atmospheres 04/2012; 117(A5):8433-. DOI:10.1029/2012JA017595 · 3.44 Impact Factor
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    ABSTRACT: During three Cassini encounters with Saturn's satellite, Enceladus, the spacecraft crossed through the plume of water vapor and dust south of the satellite with a spacecraft orientation which allowed the Cassini Plasma Spectrometer (CAPS) to observe ions and nanograin dust particles associated with the plume. These measurements were made on the E3 (March 12, 2008), E5 (October 9, 2008) and E7 (November 2, 2009) encounters. Analysis of these results, using data from the CAPS ion mass spectrometer (IMS) and electron spectrometer (ELS), found cold ions at rest with respect to Enceladus [1], negative water group and water cluster ions [2], and both positively and negatively charged dust particles in the 0.5 to 2 nm (1000 to 20,000 AMU) size range [3,4]. We present previously unreported observations from the third CAPS sensor, the ion beam spectrometer (IBS). This sensor measured the flux of positive ion and nonoparticle on the same three encounters discussed, above. The IBS measurements differ from those of IMS in several, complementary respects. The IBS data covers a more limited energy range (a factor of 67, rather than nearly four decades) and does not, in the mode used during the encounters, provide any angular resolution. It does, however, acquire energy spectra with 1.4% rather than 17% energy resolution at 2-second rather than 4-second time resolution. The IMS and IBS sensors are co-aligned, but the IBS sensor's field of view is a factor of five narrower. The IBS data allows us to estimate the temperature and flow speed of the cold ions, and characterize structure which is not resolved by in the IMS data.
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    ABSTRACT: Discrete peaks near 24.1 eV are seen in electron spectra measured in Titan’s ionosphere by the ELS (Electron Spectrometer), part of the Cassini Plasma Spectrometer (CAPS), and are interpreted as photoelectrons. These photoelectrons are generated as a result of ionization of N2 by the strong solar He II (30.4 nm) line. They are generally observed in the dayside ionosphere, because this is where neutral N2 particles can be ionized by solar radiation. Coates et al. (2007) discussed initial observations of photoelectrons in Titan’s distant tail during the T9 encounter. Here, we describe additional photoelectron peak observations at large distances from Titan, where they are unlikely to have originated because of low neutral N2 densities. We consider the tail structures during the encounters T15, T17, and T40. We infer that the distant photoelectrons may have traveled to the observation sites by means of a magnetic connection from lower altitudes in the dayside ionosphere, where they could have been produced. This idea is supported by results of hybrid modeling. Thus photoelectrons may be used as tracers of magnetic field lines and further improve our understanding of Titan’s complex plasma environment.
    Journal of Geophysical Research Atmospheres 03/2012; 117. DOI:10.1029/2011JA017113 · 3.44 Impact Factor
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    ABSTRACT: During a close pass of Cassini through the plasma wake of Saturn's moon Dione on April 7, 2010 the Cassini Plasma Spectrometer (CAPS) detected molecular oxygen ions (O2+) on pick up ring velocity distributions, thus providing the first in situ detection of a neutral exosphere surrounding the icy moon. The density of O2+ determined from the CAPS data ranges from 0.01 to 0.09 /cm3 and is used to estimate the exosphere O2 radial column density, obtaining the range 0.9 to 7 × 1011/cm2 . CAPS was unable to directly detect pick up H2O+ from the exosphere but the observations can be used to set an upper limit to their density of ˜10 times the O2+ density.
    Geophysical Research Letters 02/2012; 39(3):3105-. DOI:10.1029/2011GL050452 · 4.46 Impact Factor
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    ABSTRACT: The Cassini-Huygens mission to Saturn launched in October 1997. The Cassini Plasma Spectrometer (CAPS) is an in-situ instrument and is one of 12 instruments on the orbiter. Cruise science (beyond instrument checkout periods and periodic maintenance) was approved, and over 870 days of data were collected prior to the start of the prime mission. Prime mission operations started in January 2004 and continued through end of June 2008. Given the success of the Cassini mission at Saturn, an extended mission, the Equinox Mission, was approved for an additional two years, ending September 2010. The continuing success of the Equinox mission led to approval of a second extended mission called the Solstice Mission. The Solstice mission has approval through September 2012 with pending approval through July 2017. The Cassini Plasma Spectrometer (CAPS) has generated a wealth of science data and we have over 240 publications. In addition, the CAPS scientists participate in conferences, inter-team collaborations, and community outreach. Collection of data has not been without instrument related challenges. This paper will discuss a few of the in-flight instrument related anomalies experienced by CAPS including timing difference between the engineering model and the flight model, actuator related anomalies, and a latched bit. The analysis will cover how the anomalies were discovered, the techniques used to diagnose the problems in-flight, fixes that were implemented, how the anomalies affected operation of the instrument and collection of science, and lessons learned from the process.
    IEEE Aerospace Conference Proceedings 01/2012; DOI:10.1109/AERO.2012.6187401
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    ABSTRACT: There have been three Cassini encounters with the south-pole eruptive plume of Enceladus for which the Cassini Plasma Spectrometer (CAPS) had viewing in the spacecraft ram direction. In each case, CAPS detected a cold dense population of heavy charged particles having mass-to-charge (m/q) ratios up to the maximum detectable by CAPS (similar to 10(4) amu/e). These particles are interpreted as singly charged nanometer-sized water-ice grains. Although they are detected with both negative and positive net charges, the former greatly outnumber the latter, at least in the m/q range accessible to CAPS. On the most distant available encounter (E3, March 2008) we derive a net (negative) charge density of up to similar to 2600 e/cm(3) for nanograins, far exceeding the ambient plasma number density, but less than the net (positive) charge density inferred from the RPWS Langmuir probe data during the same plume encounter. Comparison of the CAPS data from the three available encounters is consistent with the idea that the nanograins leave the surface vents largely uncharged, but become increasingly negatively charged by plasma electron impact as they move farther from the satellite. These nanograins provide a potentially potent source of magnetospheric plasma and E-ring material.
    Journal of Geophysical Research Atmospheres 01/2012; 117(A5). DOI:10.1029/2011JA017218 · 3.44 Impact Factor
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    ABSTRACT: The failure of Titan to live up to its anticipated role as main Nitrogen source for the magnetospheric plasma of Saturn was compensated by the output of the geysering satellite Enceladus located well inside the region of closed flux tubes. It was soon found by various researchers(Smith, Johnson inter alia) that the output of Enceladus was adequate to provide the N+ seen throughout the inner and outer magnetosphere. Recently, however, textit{Cassini/CAPS} data have shown that Rhea appears to be an independent source of Nitrogen plasma (vid. Reisenfeld et al. COSPAR 2011). In this study, we investigate the hypothesis that all the icy satellites in the inner magnetosphere are sources of N+. We find that for the case of Dione there is strong evidence for the existence of indigenous Nitrogen at the satellite with enhanced density around the orbit as well. The case of Tethys is ambiguous because of the dearth of Cassini/CAPSdata at the sole targeted encounter. Enhanced density and a significant N+ fraction are observed around the orbit but comparison to the immediate environment of the satellite is not possible.
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    ABSTRACT: A recent survey of the bulk plasma ion properties observed by the Cassini CAPS instrument over roughly the first 4 1/2 years of its mission in orbit around Saturn [Thomsen et al., 2010] is expanded to consider the dependence of several of the parameters on local time as well as radial distance. The moments (density, temperature, flow velocity) of the plasma distributions below 50 keV have been computed by numerical integration of the observed counts in the "Singles" (non-mass-resolved) data, partitioned into species on the basis of concurrent determinations of the composition from the Time-of-Flight data. Moments are presented for three main species: H+, W+ (water-group ions), and ions with m/q=2. One noteworthy finding is a tendency for nightside temperatures in the inner magnetosphere (r<13 Rs) to be appreciably higher than the dayside temperatures, an asymmetry that may be a consequence of an average convection pattern, fixed in local time, in Saturn's inner magnetosphere. Such a pattern is consistent with a number of other lines of evidence from several different Cassini instruments.
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    ABSTRACT: Cassini observations have shown that the magnetospheric plasma environment near Titan is highly variable (Rymer et al. [2009] and Simon et al. [2010]). While variability is evident at timescales from minutes to days, Arridge et al. [2008] show that there is a strong periodicity at 20 Rs with period ~10.8 hours associated with plasma sheet motion at the canonical Saturn rotation period. Cassini Ion and Neutral Mass Spectrometer (INMS) observations have shown that the density structure in Titan's thermosphere responds strongly and quickly to the changing plasma environment, exhibiting hotter temperatures when Titan is within the plasma sheet than when it is in the lobe regions (Westlake et al. [2011] and Bell et al. [2011]). In this study we present an analysis of the plasma data from the Magnetospheric Imaging Instrument (MIMI) and CAPS electron and ion sensors prior to and during several Titan flybys in order to determine the drivers of the observed thermospheric heating.
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    ABSTRACT: Reviewed are CAPS positive ion measurements during the Cassini Enceladus encounters E3 (March 12, 2008), E5 (Oct 9, 2008) and E7 (Nov 2, 2009). If possible new CAPS data from E14 (Oct 1, 2011) will also be included. In these encounters plasma flow stagnation from momentum loading within the dense plume region and new water group and water cluster ion production are observed. Thermal ion density, flow velocity and temperature are estimated along the Cassini trajectory with the results similar for all three encounters even though charged dust is not detected during E7. These observations are compared with predictions from hybrid simulations including charged dust (Omidi et al., this meeting).
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    ABSTRACT: The formation of Titan’s induced magnetosphere is a unique and important example in the solar system of a plasma-moon interaction where the moon has a substantial atmosphere. The field and particle conditions upstream of Titan are important in controlling the interaction and also play a strong role in modulating the chemistry of the ionosphere. In this paper we review Titan’s plasma interaction to identify important upstream parameters and review the physics of Saturn’s magnetosphere near Titan’s orbit to highlight how these upstream parameters may vary. We discuss the conditions upstream of Saturn in the solar wind and the conditions found in Saturn’s magnetosheath. Statistical work on Titan’s upstream magnetospheric fields and particles are discussed. Finally, various classification schemes are presented and combined into a single list of Cassini Titan encounter classes which is also used to highlight differences between these classification schemes.
    Space Science Reviews 12/2011; 162(1-4). DOI:10.1007/s11214-011-9849-x · 5.87 Impact Factor
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    ABSTRACT: The interaction between the flow of solar wind plasma from the Sun and a magnetized planet produces a cavity in the flow known as a magnetosphere. Magnetic reconnection is a fundamental process that disrupts this shielding of the planet by allowing solar wind into the magnetosphere and releasing magnetic energy. Evidence for dayside reconnection at Saturn is very limited compared to Earth and other planets, representing one of the major open issues in Saturnian magnetospheric science. By combining theory, observations, and simulations we show that this is due to the pressure conditions in the vicinity of Saturn's magnetopause, which largely suppress reconnection. Our results demonstrate that solar wind-magnetosphere coupling via reconnection can vary between planets, and we cannot assume that the nature of this coupling is always Earth-like.

Publication Stats

3k Citations
574.54 Total Impact Points

Institutions

  • 1996–2014
    • University of Colorado at Boulder
      • • Department of Astrophysical and Planetary Sciences
      • • Laboratory for Atmospheric and Space Physics (LASP)
      Boulder, Colorado, United States
  • 2007–2012
    • Southwest Research Institute
      • Space Science and Engineering Division
      San Antonio, Texas, United States
  • 2009
    • University of Kansas
      • Department of Physics and Astronomy
      Lawrence, KS, United States
    • Utah State University
      • Department of Electrical and Computer Engineering
      Logan, Ohio, United States
  • 2008
    • University of Cologne
      • Institute of Geophysics and Meteorology
      Köln, North Rhine-Westphalia, Germany
    • University of California, Los Angeles
      • Institute of Geophysics and Planetary Physics
      Los Ángeles, California, United States
  • 2001–2008
    • University of Michigan
      • Department of Atmospheric, Oceanic and Space Sciences
      Ann Arbor, MI, United States
  • 2001–2007
    • Imperial College London
      • Department of Physics
      London, ENG, United Kingdom
  • 2005
    • University of Oulu
      Uleoborg, Oulu, Finland
  • 1998
    • California Institute of Technology
      Pasadena, California, United States