Periodic tilting of Saturn s plasma sheet
|
|
- Roland Francis
- 5 years ago
- Views:
Transcription
1 GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L24101, doi: /2008gl036339, 2008 Periodic tilting of Saturn s plasma sheet J. F. Carbary, 1 D. G. Mitchell, 1 P. Brandt, 1 E. C. Roelof, 1 and S. M. Krimigis 1 Received 14 October 2008; accepted 14 November 2008; published 16 December [1] From the vantage of the dawn sector, the INCA instrument on Cassini imaged neutral hydrogen atoms (20 50 kev) emitted from the center of the Saturn s plasma sheet for five days during late Points along the center of the plasma sheet were found from contoured images projected onto the noon-midnight plane; points within 20 R S of Saturn were fitted to straight lines, and the slopes of these lines were examined as a function of time at one hour resolution. The slopes vary between 17 and 24 with a period of hours, the same as that of Saturn kilometric radiation (SKR). This periodic tilting of the plasma sheet is in phase with SKR radiation in the sense that the maximum tilt angle occurs when the maximum in the SKR power occurs, and the tilt angle periodicity has a phase angle of 47 in SLS-3 longitude. Citation: Carbary, J. F., D. G. Mitchell, P. Brandt, E. C. Roelof, and S. M. Krimigis (2008), Periodic tilting of Saturn s plasma sheet, Geophys. Res. Lett., 35, L24101, doi: /2008gl Introduction [2] The magnetosphere of Saturn exhibits a multitude of periodicities. A period near hours appears in energetic charged particles, both ions and electrons [Carbary and Krimigis, 1982; Carbary et al., 2007a], in low energy plasma [Gurnett et al., 2007], in the energetic neutral atoms [Paranicas et al., 2005; Carbary et al., 2008], and in magnetic field perturbations [Espinosa and Dougherty, 2000; Giampieri et al., 2006]. Saturn s kilometric radiation ( khz) shows an especially pronounced periodicity [Desch and Kaiser, 1981; Gurnett et al., 2005] upon which longitude systems may be based [Davies et al., 1996; Kurth et al., 2008]. However, the radio period does not remain constant and small variations of 1% have been detected over long times of several months [Galopeau and Lecacheux, 2000; Gurnett et al., 2005; Kurth et al., 2008]. [3] The source of these periodicities remains obscure. Saturn s magnetic axis is aligned within 1 of its rotation axis [Davis and Smith, 1990; Dougherty et al., 2005; Nichols et al., 2008], so periodicities at Saturn cannot arise from a significant magnetic tilt such as they do at Jupiter. Originally proposed to explain periodicities at Jupiter [e.g., Dessler and Hill, 1975], a rotating anomaly is often invoked to address Saturn s periodicities. The anomaly may result from some centrifugally-driven convective instability, which results in outflow at a particular longitude [Gurnett et al., 2007; Goldreich and Farmer, 2007], or it may be caused by a longitudinally asymmetric arrangement of 1 Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA. Copyright 2008 by the American Geophysical Union /08/2008GL field-aligned currents [Southwood and Kivelson, 2007]. Once the anomaly is established, it may cause a corotating or partially corotating bulge in Saturn s inner magnetosphere that propagates radially outward in the form of a spiral wave [Espinosa et al., 2003; Carbary et al., 2007c]. A wavy magnetotail can be generated by the sliding effects of the anomaly as its bulge rotates non-concentrically about Saturn [Carbary et al., 2007b]. Alternately, magnetospheric waves could be produced by solar wind pressure that alternately lifts the light side of the anomaly and drops the heavy side [Khurana et al., 2008]. The asymmetric slide model predicts that Saturn s plasma sheet would remain at a fixed angle relative to the solar wind flow, while the asymmetric lift model predicts that the plasma sheet angle would vary with the rotation period of the anomaly. [4] The Ion-Neutral CAmera (INCA) onboard the Cassini spacecraft affords a unique perspective with which to observe the plasma sheet. INCA observes energetic neutral atoms (ENA) generated by the collision of energetic ions (>10 kev) in Saturn s magnetosphere with cold neutral atoms in the neutral cloud surrounding the planet, and can provide images of the energetic plasma coming from the plasma sheet. During December 2004, Cassini moved outward along the dawn flank of Saturn s magnetosphere and afforded INCA several days of observing the plasma sheet from along the dawn side. This unique dataset has been used to measure periodicities in the ENA emissions and characterize the shape of the plasma sheet [e.g., Paranicas et al., 2005]. Here, the same data can be used to show time variations in the motion of the plasma sheet. 2. Instrument and Data Set [5] The Magnetospheric IMaging Instrument on the Cassini spacecraft consists of the Low Energy Magnetospheric Measurement System (LEMMS), the CHarge Energy Mass Spectrometer (CHEMS), and the Ion Neutral CAmera (INCA). The complete instrument is described by Krimigis et al. [2004]. [6] This paper relies on data from the INCA sensor. INCA measures energetic neutral atoms (ENA) from 7 kev to 3 MeV/nucleon with time resolution of 85 seconds to 6 minutes. The sensor uses a time-of-flight method that can separate energetic neutrals in energy and species by use of a thin-foil and fan technique. With a field of view of , INCA provides images with 64 64, 32 32, or pixels. The lower resolution images contain information on ENA energies at the cost of low spatial resolution, while the higher resolution images contain information on ENA spatial distribution at the cost of energy information. This investigation uses pixel images from the kev hydrogen channel, which represents a compromise between energy and spatial resolution. L of5
2 [7] INCA images from day 352 (December 17) through 356 (December 21) 2004 were used for this study. INCA made unique observations during this time for three reasons. First, the spacecraft was moving outbound along the dawn flank, near the equatorial plane at radial distances greater than 20 R S, and remained in a constant orientation with INCA looking toward Saturn. Second, INCA made nearly continuous observations throughout the period. The unique combination of viewing geometry and continuous measurement allowed INCA to monitor the entire Saturnian magnetosphere from one side. Third, at this time, the equatorial plane of Saturn (at noon) was inclined 23 relative to the Saturn-Sun-Orbit plane [Acton, 1996; Arridge et al., 2008]; the planet had just passed its southern hemisphere solstice. Therefore, Cassini had the opportunity to observe the plasma sheet from an edge-on perspective when the sheet was tilted at an extreme angle to the solar wind flow. The exceptional INCA images from this time have been used previously to examine ENA periodicity and plasma sheet warping [Paranicas et al., 2005]. 3. Analysis Technique [8] To improve the statistics, INCA images were first averaged into one-hour time periods for the five days in the observing interval. Because the INCA orientation and range to Saturn were essentially constant for each hour interval, the images suffered no degradation from motion of the spacecraft. After 5 5 pixel smoothing, the images were then projected onto the noon-midnight plane of the Saturn- Sun-Orbit (SSO) coordinate system and the intensities were corrected for slant viewing. Figure 1 shows a sample projected image. The +X SSO axis points toward the Sun and the X SSO axis toward the magnetotail. The spin axis of Saturn is tilted about 23 from the vertical, and the bright central region defines the plasma sheet. [9] The center of the plasma sheet can be determined by simple image processing. For each projected image, 32 contours were constructed using the CONTOUR procedure in the Interactive Data Language (IDL) software. Each contour line consists of a set of positions {X SSO,Z SSO } in SSO coordinates. The centroids of each set define the center of the contour (X C = SX SSO /N, Y C = SY SSO /N, where N = number of points in each contour set), and the range points (R = [(X SSO X C ) 2 +(Y SSO Y C ) 2 ] 1/2 ) define the distances of each point from the center. The two maxima for each set of R points determines the center of the of the plasma sheet for a particular contour. The red triangles in Figure 1 indicate the maxima from the contours. The locus of these points defines the central plasma sheet in profile as viewed from the edge-on geometry. [10] In profile, the plasma sheet center appears as a roughly straight line between approximately 20 R S and +20 R S.In Figure 1, a thick red line shows this linear fit. The tilt angle of the plasma sheet is the slope of this straight line, which is 22.9 in the example. The tilt angle is found for each hour by fitting straight lines to the contour maxima from each image between 20 R S and +20 R S. The tilt angles are then displayed as a function of time to determine possible variations in the plasma sheet orientation. [11] A JPEG animation (Animation 1) has been generated to show the temporal variation of the plasma sheet and its tilt. 1 Each frame of Animation 1 represents an hour average of the projected ENA images from kev hydrogen in the same format as Figure 1 except the contours arenot plotted. The straight white lines indicate fits to the contour maxima. Two regular variations appear in Animation 1. The first is a rotational motion of a bright spot (or blob ), which moves left to right along the central plasma sheet (see Carbary et al. [2008] for a discussion of blob motion), and the second is the tilting motion of the central plasma sheet. This paper concerns the variations in the latter. 4. Periodic Behavior and Relation to SKR [12] The top plot of Figure 2 presents the tilt angle as a function of time for days 352 to 356. The angle s signal exhibits a regular modulation with a period very close to the period of SKR radiation during this time [Kurth et al., 2008]. A tick scale in the top plot of Figure 2 emphasizes this. The angle varies from 17 to 24, with a mean uncertainty of 0.5 in the angle. The amplitude of the variation is irregular, although it may be decreasing with time as suggested by the dashed line envelope in Figure 2. [13] The period of this modulation can be confirmed by a Lomb periodogram, as shown in the bottom plot of Figure 3. The periodogram was limited to period between 5 and 15 hours, which is the region of interest for SKR periodicity. In that range, the tilt signal has only one very strong peak at 10.8 hours. The signal-to-noise ratio of the peak is 11.3 (i.e., peak value to mean value of secondary peaks). [14] A precise relationship between the plasma sheet tilt and the SKR radiation can be demonstrated. A cross correlation analysis was performed between the tilt angle and the logarithm of SKR power ( khz) summed into 1-hour time bins without correction. The correlation coefficient between the angle and the SKR power was computed for hourly time shifts between 10 hours and +10 hours. The top frame of Figure 3 indicates the results. Although the peak correlation coefficient is only r = 0.4, the probability p ffiffiffiffiffiffiffiffi that the two signals are not correlated is only p = erfc(r N=2 )= [e.g., Press et al., 1992]. The SKR power reaches a maximum at the same time that the angle reaches a maximum. That is, when the plasma sheet tilts highest on the dayside (and lowest on the nightside), SKR power is maximized. [15] Finally, the phase of the tilt angle can be examined as a function of SLS-3 longitude, as defined by Kurth et al. [2008]. The SKR longitude was computed for the noon meridian at 20 R S, where the tilt angle is measured. The bottom of Figure 3 indicates the resulting phase relation between the tilt angle and SLS-3. If the tilt angle q is fit to the function cos(8 8 o ), where 8 is the SLS longitude and 8 o is the phase, the phase is found to be 46. If the tilt is caused by a weighting of the plasma sheet, then the sheet would be lightest at this longitude and heaviest at = 226 in SLS-3 longitude. 5. Discussion [16] This analysis tacitly assumes that the intense region of ENA emission in the equatorial plane represents the 1 Animations are available in the HTML. 2of5
3 Figure 1. Sample linear fit determining the tilt of the plasma sheet. Hour averages of INCA images of neutral hydrogen (20 50 kev) were projected onto the noonmidnight plane in Saturn-Sun-Orbit coordinates (SSO). Contours of the image are shown as white lines; the range maxima of these contours appear as red triangles. The triangles within ±20 R S (dotted red lines) generally lie in a straight line and are subject to a linear fit, shown as the heavy red line. In this case, N = 36 points were used for the fit, which had a standard deviation of 0.5 R S ; the fitted line had a tilt angle of Figure 3. Comparison of the tilt angle signal with SKR signal (sum of radio power within khz band). (top) Correlation coefficient vs. offset time between tilt angle and SKR signal. (bottom) Tilt angle as function of SLS-3 longitude. The solid line represents a cosine fit to the tilt angle in SLS-3 longitude system. The dashed vertical line indicates the phase of this fit is Figure 2. (top) The slopes of linear fits are shown as a function of time for five days in The tick marks appear at intervals to show SKR period; the dashed lines indicate an envelope within which the oscillations occur. (bottom) Lomb periodogram of the tilt angle signal. The dashed vertical line shows the SKR period. plasma sheet [e.g., Mitchell et al., 2003]. This assumption is reasonable because energetic neutral atoms originate from collisions between cold neutrals and energetic ions, both of which should be found in the equatorial plane. Another assumption is that the intensity contours of a projected ENA image can capture the plasma sheet emissions. Inherent in this assumption are sufficiently adequate statistics of the ENA and a benign geometry. Hour averaging and an optimal side view at near 90 help mitigate concerns about the second assumption. Finally, the analysis has examined only a few days in 2004 when Saturn was near solstice. Not examined here, solar wind conditions may have favored the expression of tilt periodicity at this time, so that such periodicity may not always be taking place at Saturn. Nevertheless, the results show that Saturn s plasma sheet can exhibit periodicity in its tilting at least some times. [17] Although Saturn s magnetic axis is aligned to within 1 of its spin axis, the planet can apparently generate latitudinal motion of its plasma sheet in a manner similar to that of Jupiter. In the case of Jupiter, whose magnetic axis is tilted, this motion has a constant amplitude of 10. At Saturn, the peak-to-peak amplitude varies from 6 to 4 and changes throughout the observing interval. The tilting of Saturn s plasma sheet was observed for several days in late 2004 when the planet was near its southern solstice. More 3of5
4 observations are required to confirm that this motion is a regular dynamical feature of Saturn s magnetosphere, or whether it appears only under certain conditions. The extended Cassini mission may offer opportunities for these observations. [18] The periodic tilting motion of Saturn s plasma sheet reflects periodic variations observed throughout the magnetosphere including those of the magnetic fields, charged particles, both ions and electrons, and the kilometric radiation. The periodic tilting does not reflect tilting of the neutral cloud itself, which must be confined by non-electromagnetic forces to the equatorial plane of Saturn [e.g., Richardson, 1998]. [19] The tilting motion of the plasma sheet suggests that the asymmetric sliding model of magnetospheric periodicity [Carbary et al., 2007b] is inappropriate for Saturn, at least at the time the observations shown here were made. In contrast, two other models can produce a periodic tilting of the plasma sheet. A system of rotating non-axisymmetric currents could produce an apparently oscillating dipole with a tilt amplitude of [Southwood and Kivelson, 2007], while the asymmetric lift model predicts a periodic tilting of the plasma sheet with an amplitude of 8 10 [Khurana et al., 2008]. In the latter model, solar wind pressure alternately raises and lowers the plasma sheet because of a longitudinal mass asymmetry. From the bottom plot of Figure 3, the light sector should occur near SLS-3 longitude of 47 and the heavy sector should occur near 227. The asymmetric lift model further suggests that the plasma sheet tilting should be affected by the solar wind ram pressure and the seasons at Saturn. As Saturn approaches its equinox, the model predicts that the modulations should be greatly reduced. [20] On the other hand, the observations do suggest disparities with the asymmetric lift model as presently configured. Most importantly, the model indicates that the light sector should become parallel to the solar wind flow on the nightside, and the observations presented here do not indicate this. Also, the amplitude of plasma sheet oscillation is only 2 3 whereas the model suggests a larger amplitude of 8 or more. 6. Conclusions [21] Imaged by the Cassini INCA detector during late 2004, neutral hydrogen atoms (20 50 kev) trace the center of the Saturn s plasma sheet, the center of which was determined by linear fits to contour maxima. When examined as a function of time, these slopes vary between 17 and 24 with a well-defined period of hours, the same period as that of Saturn kilometric radiation (SKR). The maximum tilt angle occurs when the maximum in the SKR variation occurs. The periodic tilting of the plasma sheet agrees qualitatively with predictions of the asymmetric-lift model of Saturn s magnetosphere and offers evidence of a mechanism that could generate some of the periodicities known in Saturn s magnetosphere. [22] Acknowledgments. This research was supported partly by the NASA Office of Space Science under task order 003 of contract NAS between NASA Goddard Space Flight Center and the Johns Hopkins University and partly by NASA grant NNX07AJ69G under the Cassini Data Analysis Program. References Acton, C. H. (1996), Ancillary data services of NASA s navigation and ancillary information facility, Planet. Space Sci., 44, Arridge, C. S., K. K. Khurana, C. T. Russell, D. J. Southwood, N. Achilleos, M. K. Dougherty, A. J. Coates, and H. K. Leinweber (2008), Warping of Saturn s magnetospheric and magnetotail current sheets, J. Geophys. Res., 113, A08217, doi: /2007ja Carbary, J. F., and S. M. Krimigis (1982), Charged particle periodicity in the Saturnian magnetosphere, Geophys. Res. Lett., 9, Carbary, J. F., D. G. Mitchell, S. M. Krimigis, D. C. Hamilton, and N. Krupp (2007a), Charged particle periodicities in Saturn s outer magnetosphere, J. Geophys. Res., 112, A06246, doi: /2007ja Carbary, J. F., D. G. Mitchell, S. M. Krimigis, D. C. Hamilton, and N. Krupp (2007b), Spin-period effects in magnetospheres with no axial tilt, Geophys. Res. Lett., 34, L18107, doi: /2007gl Carbary, J. F., D. G. Mitchell, S. M. Krimigis, and N. Krupp (2007c), Evidence for spiral pattern in Saturn s magnetosphere using the new SKR longitudes, Geophys. Res. Lett., 34, L13105, doi: / 2007GL Carbary, J. F., D. G. Mitchell, P. Brandt, E. C. Roelof, and S. M. Krimigis (2008), Track analysis of energetic neutral atom blobs at Saturn, J. Geophys. Res., 113, A01209, doi: /2007ja Davies, M. E., et al. (1996), Report for the IAU/IAG/COSPAR working group on cartographic coordinates and rotational elements of the planets and satellites: 1994, Celestial Mech. Dyn. Astron., 63, Davis, L., and E. J. Smith (1990), A model of Saturn s magnetic field based on all available data, J. Geophys. Res., 95, 15,257 15,261. Desch, M. D., and M. L. Kaiser (1981), Voyager measurements of the rotation period of Saturn s magnetic field, Geophys. Res. Lett., 8, Dessler, A. J., and T. W. Hill (1975), High order magnetic monopoles as a source of gross asymmetry in the distant Jovian magnetotail, Geophys. Res. Lett., 2, Dougherty, M. K., et al. (2005), Cassini magnetometer observations during Saturn orbit insertion, Science, 307, , doi: / science Espinosa, S. A., and M. K. Dougherty (2000), Periodic perturbations in Saturn s magnetic field, Geophys. Res. Lett., 27, Espinosa, S. A., D. J. Southwood, and M. K. Dougherty (2003), How can Saturn impose its rotation period in a noncorotating magnetosphere?, J. Geophys. Res., 108(A2), 1086, doi: /2001ja Galopeau, P. H. M., and A. Lecacheux (2000), Variations of Saturn s radio period measured at kilometer wavelengths, J. Geophys. Res., 105, 13,089 13,101. Giampieri, G., M. K. Dougherty, E. J. Smith, and C. T. Russell (2006), A regular period for Saturn s magnetic field that may track its internal rotation, Nature, 441, 62 64, doi: /nature Goldreich, P., and A. J. Farmer (2007), Spontaneous axisymmetry breaking of the external magnetic field at Saturn, J. Geophys. Res., 112, A05225, doi: /2006ja Gurnett, D. A., et al. (2005), Radio and plasma wave observations at Saturn from Cassini s approach and first orbit, Science, 307, , doi: /science Gurnett, D. A., A. M. Persoon, W. S. Kurth, J. B. Groene, T. F. Averkamp, M. K. Dougherty, and D. J. Southwood (2007), The variable rotation period of the inner region of Saturn s plasma disk, Science, 316, , doi: /science Khurana, K. K., D. G. Mitchell, C. S. Arridge, M. K. Dougherty, C. T. Russell, C. Paranicas, N. Krupp, and A. J. Coates (2008), Sources of rotational signals in Saturn s magnetosphere, J. Geophys. Res., doi: /2008ja013312, in press. Krimigis, S. M., et al. (2004), Magnetospheric imaging instrument (MIMI) on the Cassini mission to Saturn/Titan, Space Sci. Rev., 114, Kurth, W. S., T. F. Averkamp, D. A. Gurnett, J. B. Groene, and A. Lecacheux (2008), An update to a Saturnian longitude system based on kilometric radio emissions, J. Geophys. Res., 113, A05222, doi: / 2007JA Mitchell, D. G., P. C. Brandt, E. C. Roelof, D. C. Hamilton, C. Retterer, and S. Mende (2003), Global imaging of O + from IMAGE/HENA, Space Sci. Rev., 109, Nichols, J. D., J. T. Clarke, S. W. H. Cowley, J. Duval, A. J. Farmer, J.-C. Gérard, D. Grodent, and S. Wannawichian (2008), Oscillation of Saturn s southern auroral oval, J. Geophys. Res., 113, A11205, doi: / 2008JA Paranicas, C., D. G. Mitchell, E. C. Roelof, P. C. Brandt, D. J. Williams, S. M. Krimigis, and B. H. Mauk (2005), Periodic intensity variations in global ENA images of Saturn, Geophys. Res. Lett., 32, L21101, doi: /2005gl of5
5 Press, W. H., S. A. Teukelosky, W. T. Vetterling, and B. P. Flannery (1992), Numerical Recipes: The Art of Scientific Computing, 2nd ed., Cambridge Univ. Press, 631 pp., Cambridge, U. K. Richardson, J. D. (1998), Thermal plasma and neutral gas in Saturn s magnetosphere, Rev. Geophys., 36(4), Southwood, D. J., and M. G. Kivelson (2007), Saturnian magnetospheric dynamics: Elucidation of a camshaft model, J. Geophys. Res., 112, A12222, doi: /2007ja P. Brandt, J. F. Carbary, S. M. Krimigis, D. G. Mitchell, and E. C. Roelof, Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. (james.carbary@jhuapl.edu) 5of5
ENA periodicities at Saturn
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L07102, doi:10.1029/2008gl033230, 2008 ENA periodicities at Saturn J. F. Carbary, 1 D. G. Mitchell, 1 P. Brandt, 1 C. Paranicas, 1 and
More informationDirect observation of warping in the plasma sheet of Saturn
GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L24201, doi:10.1029/2008gl035970, 2008 Direct observation of warping in the plasma sheet of Saturn J. F. Carbary, 1 D. G. Mitchell, 1 C. Paranicas, 1 E. C. Roelof,
More informationPeriodicity in Saturn s magnetosphere: Plasma cam
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L14203, doi:10.1029/2009gl039043, 2009 Periodicity in Saturn s magnetosphere: Plasma cam J. L. Burch, 1 A. D. DeJong, 1 J. Goldstein,
More informationDawn dusk oscillation of Saturn s conjugate auroral ovals
GEOPHYSICAL RESEARCH LETTERS, VOL. 37,, doi:10.1029/2010gl045818, 2010 Dawn dusk oscillation of Saturn s conjugate auroral ovals J. D. Nichols, 1 S. W. H. Cowley, 1 and L. Lamy 2 Received 11 October 2010;
More informationStatistical analysis of injection/dispersion events in Saturn s inner magnetosphere
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2008ja013166, 2008 Statistical analysis of injection/dispersion events in Saturn s inner magnetosphere Y. Chen 1 and T. W. Hill 1 Received 18 March
More informationPUBLICATIONS. Journal of Geophysical Research: Space Physics. Local time dependences of oxygen ENA periodicities at Saturn
PUBLICATIONS RESEARCH ARTICLE Key Points: Periodicities of energetic oxygen atoms depend on local time Dual periods near midnight but mono periods near noon or midnight Periodicities may disappear entirely
More informationA plasmapause like density boundary at high latitudes in Saturn s magnetosphere
GEOPHYSICAL RESEARCH LETTERS, VOL. 37,, doi:10.1029/2010gl044466, 2010 A plasmapause like density boundary at high latitudes in Saturn s magnetosphere D. A. Gurnett, 1 A. M. Persoon, 1 A. J. Kopf, 1 W.
More informationPlasma convection in Saturn s outer magnetosphere determined from ions detected by the Cassini INCA experiment
GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L04102, doi:10.1029/2007gl032342, 2008 Plasma convection in Saturn s outer magnetosphere determined from ions detected by the Cassini INCA experiment M. Kane, 1 D.
More informationThe chiming of Saturn s magnetosphere at planetary periods
The chiming of Saturn's magnetosphere at planetary periods. Gabby Provan with help from David Andrews and Stan Cowley The chiming of Saturn s magnetosphere at planetary periods G. Provan, D. J. Andrews
More informationInfluence of hot plasma pressure on the global structure of Saturn s magnetodisk
GEOPHYSICAL RESEARCH LETTERS, VOL. 37,, doi:10.1029/2010gl045159, 2010 Influence of hot plasma pressure on the global structure of Saturn s magnetodisk N. Achilleos, 1,2 P. Guio, 1,2 C. S. Arridge, 2,3
More informationROTATIONAL MODULATION OF SATURN KILOMETRIC RADIATION, NARROWBAND EMISSION AND AURORAL HISS
1 2 3 ROTATIONAL MODULATION OF SATURN KILOMETRIC RADIATION, NARROWBAND EMISSION AND AURORAL HISS 4 S. Y. Ye,G.Fischer, W. S. Kurth,J.D.Menietti,andD.A.Gurnett 5 6 7 8 9 10 11 12 13 14 15 16 17 18 Abstract
More informationUpdate on Periodicities in Saturn s Magnetosphere
Update on Periodicities in Saturn s Magnetosphere J.F. Carbary & the Cassini/MIMI Team Johns Hopkins University Applied Physics Laboratory Laurel, MD 20723 Presented at Saturn Periodicities Workshop 2
More informationJOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, A04212, doi: /2009ja014729, 2010
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja014729, 2010 Magnetic field oscillations near the planetary period in Saturn s equatorial magnetosphere: Variation
More informationRotational modulation and local time dependence of Saturn s infrared H 3 + auroral intensity
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117,, doi:10.1029/2012ja017990, 2012 Rotational modulation and local time dependence of Saturn s infrared H 3 + auroral intensity S. V. Badman, 1 D. J. Andrews, 2
More informationPERIODICITIES IN SATURN S MAGNETOSPHERE
PERIODICITIES IN SATURN S MAGNETOSPHERE J. F. Carbary 1 and D. G. Mitchell 1 Received 31 August 2012; revised 2 February 2013; accepted 5 February 2013; published 27 March 2013. [1] Although the exact
More informationVARIABILITY OF SOUTHERN AND NORTHERN SKR PERIODICITIES
VARIABILITY OF SOUTHERN AND NORTHERN SKR PERIODICITIES L. Lamy Abstract Among the persistent questions raised by the existence of a rotational modulation of the Saturn Kilometric Radiation (SKR), the origin
More informationReanalysis of Saturn s magnetospheric field data view of spin-periodic perturbations
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. A2, 1085, doi:10.1029/2001ja005083, 2003 Reanalysis of Saturn s magnetospheric field data view of spin-periodic perturbations Stéphane A. Espinosa 1 Max-Planck-Institut
More informationThe plasma density distribution in the inner region of Saturn s magnetosphere
JOURNAL OF GEOPHYSICAL RESEARCH: SPACE PHYSICS, VOL. 118, 970 974, doi:10.100/jgra.5018, 013 The plasma density distribution in the inner region of Saturn s magnetosphere A. M. Persoon, 1 D. A. Gurnett,
More informationStatistical morphology of ENA emissions at Saturn
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2007ja012873, 2008 Statistical morphology of ENA emissions at Saturn J. F. Carbary, 1 D. G. Mitchell, 1 P. Brandt, 1
More informationAn update to a Saturnian longitude system based on kilometric radio emissions
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2007ja012861, 2008 An update to a Saturnian longitude system based on kilometric radio emissions W. S. Kurth, 1 T. F. Averkamp, 1 D. A. Gurnett,
More informationARTICLE IN PRESS. Planetary and Space Science
Planetary and Space Science 57 (2009) 1732 1742 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Recurrent energization of plasma in the
More informationA SLS4 LONGITUDE SYSTEM BASED ON A TRACKING FILTER ANALYSIS OF THE ROTATIONAL MODULATION OF SATURN KILOMETRIC RADIATION
A SLS4 LONGITUDE SYSTEM BASED ON A TRACKING FILTER ANALYSIS OF THE ROTATIONAL MODULATION OF SATURN KILOMETRIC RADIATION D.A. Gurnett, J.B. Groene,T.F.Averkamp, W.S. Kurth, S.-Y. Ye, and G. Fischer Abstract
More informationSaturn s equinoctial auroras
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L24102, doi:10.1029/2009gl041491, 2009 Saturn s equinoctial auroras J. D. Nichols, 1 S. V. Badman, 1 E. J. Bunce, 1 J. T. Clarke, 2 S.
More informationDynamics of the Jovian magnetosphere for northward interplanetary magnetic field (IMF)
GEOPHYSICAL RESEARCH LETTERS, VOL. 32, L03202, doi:10.1029/2004gl021392, 2005 Dynamics of the Jovian magnetosphere for northward interplanetary magnetic field (IMF) Keiichiro Fukazawa and Tatsuki Ogino
More informationObservations of plasma sheet structure and dynamics
Observations of plasma sheet structure and dynamics Chris Arridge 1,2 1. Mullard Space Science Laboratory, UCL. 2. The Centre for Planetary Sciences at UCL/Birkbeck. Email: csa@mssl.ucl.ac.uk Twitter:
More informationModeling of Saturn s magnetosphere during Voyager 1 and Voyager 2 encounters
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja015124, 2010 Modeling of Saturn s magnetosphere during Voyager 1 and Voyager 2 encounters M. Chou 1 and C. Z. Cheng 1,2 Received 20 November
More informationCold ionospheric plasma in Titan s magnetotail
GEOPHYSICAL RESEARCH LETTERS, VOL. 34, L24S06, doi:10.1029/2007gl030701, 2007 Cold ionospheric plasma in Titan s magnetotail H. Y. Wei, 1 C. T. Russell, 1 J.-E. Wahlund, 2 M. K. Dougherty, 2 C. Bertucci,
More informationPossible eigenmode trapping in density enhancements in Saturn s inner magnetosphere
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 34, L04103, doi:10.1029/2006gl028647, 2007 Possible eigenmode trapping in density enhancements in Saturn s inner magnetosphere J. D. Menietti,
More informationSaturn s Erratic Clocks: Searching for the Rotation Rate of a Planet
Saturn s Erratic Clocks: Searching for the Rotation Rate of a Planet J.F. Carbary 1, M.M. Hedman 2, T.W. Hill 3, X. Jia 4, W.S. Kurth 5, L. Lamy 6, and G. Provan 7 1 Johns Hopkins University Applied Physics
More informationOrigins of Saturn s Auroral Emissions and Their Relationship to Large-Scale Magnetosphere Dynamics
Origins of Saturn s Auroral Emissions and Their Relationship to Large-Scale Magnetosphere Dynamics Emma J. Bunce Department of Physics and Astronomy, University of Leicester, Leicester, UK In this review
More informationFirst whistler observed in the magnetosphere of Saturn
GEOPHYSICAL RESEARCH LETTERS, VOL. 33, L20107, doi:10.1029/2006gl027019, 2006 First whistler observed in the magnetosphere of Saturn F. Akalin, 1 D. A. Gurnett, 1 T. F. Averkamp, 1 A. M. Persoon, 1 O.
More informationParticle pressure, inertial force and ring current density profiles. in the magnetosphere of Saturn, based on Cassini measurements.
1 2 Particle pressure, inertial force and ring current density profiles in the magnetosphere of Saturn, based on Cassini measurements. 3 4 5 6 N. Sergis 1, S.M. Krimigis 1,2, E.C. Roelof 2, C.S. Arridge
More informationGlobal configuration and seasonal variations of Saturn s magnetosphere
Global configuration and seasonal variations of Saturn s magnetosphere N. Krupp, A. Masters, M.F. Thomsen, D.G. Mitchell, P. Zarka, P. Kollmann, X. Jia Magnetosphere chapters in Saturn book 2009 Gombosi
More informationSaturn s magnetodisc current sheet
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2007ja012540, 2008 Saturn s magnetodisc current sheet C. S. Arridge, 1,2,4 C. T. Russell, 3 K. K. Khurana, 3 N. Achilleos,
More informationSaturn s ring current: Local time dependence and temporal variability
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 116,, doi:10.1029/2010ja016216, 2011 Saturn s ring current: Local time dependence and temporal variability S. Kellett, 1 C. S. Arridge, 2,3 E. J. Bunce, 1 A. J. Coates,
More informationExternal triggering of plasmoid development at Saturn
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117,, doi:10.1029/2012ja017625, 2012 External triggering of plasmoid development at Saturn A. Kidder, 1 C. S. Paty, 2 R. M. Winglee, 1 and E. M. Harnett 1 Received
More informationRelationship between solar wind corotating interaction regions and the phasing and intensity of Saturn kilometric radiation bursts
Ann. Geophys., 26, 3641 3651, 2008 European Geosciences Union 2008 Annales Geophysicae Relationship between solar wind corotating interaction regions and the phasing and intensity of Saturn kilometric
More informationOccurrence characteristics of Saturn s radio burst
Occurrence characteristics of Saturn s radio burst D. Maruno 1, Y. Kasaba 1, T. Kimura 2, A. Morioka 1, B. Cecconi 3 1 Department of Geophysics, Tohoku University 2 ISAS, JAXA 3 LESIA, Observatorire de
More informationLongitudinal plasma density variations at Saturn caused by hot electrons
GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L03107, doi:10.1029/2007gl031095, 2008 Longitudinal plasma density variations at caused by hot electrons P. A. Delamere 1 and F. Bagenal 1 Received 22 June 2007;
More informationJovian Radiation Environment Models at JPL
Copyright 2016 California Institute of Technology. Government sponsorship acknowledged. Jovian Radiation Environment Models at JPL By Insoo Jun and the JPL Natural Space Environments Group Jet Propulsion
More informationTest-particle simulation of electron pitch angle scattering due to H 2 O originating from Enceladus
Test-particle simulation of electron pitch angle scattering due to H 2 O originating from Enceladus Hiroyasu Tadokoro 1 and Yuto Katoh 2 1 Tokyo University of Technology E-mail: tadokorohr@stf.teu.ac.jp
More informationEnergetic electron microsignatures as tracers of radial flows and dynamics in Saturn s innermost magnetosphere
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja014808, 2010 Energetic electron microsignatures as tracers of radial flows and dynamics in Saturn s innermost magnetosphere
More informationTitle: Effects of radial motion on interchange injections at Saturn
Elsevier Editorial System(tm) for Icarus Manuscript Draft Manuscript Number: ICARUS-14182R2 Title: Effects of radial motion on interchange injections at Saturn Article Type: Regular Article Keywords: Saturn;
More informationSaturn s Gravitational Field, Internal Rotation, and Interior Structure
Saturn s Gravitational Field, Internal Rotation, and Interior Structure John D. Anderson 1 and Gerald Schubert 2 1 121 South Wilson Ave., Pasadena, CA 91106-3017, USA 2 Department of Earth and Space Sciences
More informationA Saturnian cam current system driven by asymmetric thermospheric heating
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 1 April 2010 (MN LATEX style file v2.2) A Saturnian cam current system driven by asymmetric thermospheric heating C. G. A. Smith The Brooksbank School,
More informationLocation of Saturn s northern infrared aurora determined from Cassini VIMS images
GEOPHYSICAL RESEARCH LETTERS, VOL. 38,, doi:10.1029/2010gl046193, 2011 Location of Saturn s northern infrared aurora determined from Cassini VIMS images S. V. Badman, 1 N. Achilleos, 2 K. H. Baines, 3
More informationEquatorward diffuse auroral emissions at Jupiter: Simultaneous HST and Galileo observations
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L07101, doi:10.1029/2009gl037857, 2009 Equatorward diffuse auroral emissions at Jupiter: Simultaneous HST and Galileo observations A.
More informationSheared magnetic field structure in Jupiter s dusk magnetosphere: Implications for return currents
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A7, 1116, 10.1029/2001JA000251, 2002 Sheared magnetic field structure in Jupiter s dusk magnetosphere: Implications for return currents Margaret G. Kivelson,
More informationTowards jointly-determined magnetospheric periods
Towards jointly-determined magnetospheric periods Dave Andrews ISSI, October 2015 david.andrews@irfu.se Outline Lots of independent work done on determining rotation periods of various magnetospheric phenomena
More informationObservation of similar radio signatures at Saturn and Jupiter: Implications for the magnetospheric dynamics.
Observation of similar radio signatures at Saturn and Jupiter: Implications for the magnetospheric dynamics. P. Louarn, W.S. Kurth, D.A. Gurnett, G.B. Hospodarsky, A.M. Persoon, B. Cecconi, A. Lecacheux,
More informationA new form of Saturn s magnetopause using a dynamic pressure balance model, based on in situ, multi instrument Cassini measurements
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja014262, 2010 A new form of Saturn s magnetopause using a dynamic pressure balance model, based on in situ, multi
More informationAURORA: GLOBAL FEATURES
AURORA: GLOBAL FEATURES Jean-Claude Gérard LPAP Université de Liège OUTLINE - collisional processes involved in the aurora - remote sensing of auroral electron energy - Jupiter - Saturn MOP meeting - 2011
More informationSUPPLEMENTARY INFORMATION
doi:.38/nature149 1 Observation information This study examines 2 hours of data obtained between :33:42 and 12:46:28 Universal Time (UT) on April 17 11 using the -metre Keck telescope. This dataset was
More informationPlanetary ENA imaging:! where we are, where to go! Stas Barabash Swedish Institute of Space Physics Kiruna, Sweden
Planetary ENA imaging:! where we are, where to go! Stas Barabash Swedish Institute of Space Physics Kiruna, Sweden 1 Planetary ENA imaging overview. Where we are now! Object ---------! Difficulties: from
More informationIDENTIFICATION OF SATURN S MAGNETOSPHERIC REGIONS AND ASSOCIATED PLASMA PROCESSES: SYNOPSIS OF CASSINI OBSERVATIONS DURING ORBIT INSERTION
IDENTIFICATION OF SATURN S MAGNETOSPHERIC REGIONS AND ASSOCIATED PLASMA PROCESSES: SYNOPSIS OF CASSINI OBSERVATIONS DURING ORBIT INSERTION N. André, 1,2,3 M. Blanc, 3 S. Maurice, 3 P. Schippers, 3 E. Pallier,
More informationPeak emission altitude of Saturn s H 3 + aurora
GEOPHYSICAL RESEARCH LETTERS, VOL. 39,, doi:10.1029/2012gl052806, 2012 Peak emission altitude of Saturn s H 3 + aurora Tom S. Stallard, 1 Henrik Melin, 1 Steve Miller, 2 Sarah V. Badman, 3 Robert H. Brown,
More informationPlasmas observed near local noon in Jupiter s magnetosphere with the Galileo spacecraft
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109,, doi:10.1029/2002ja009795, 2004 Plasmas observed near local noon in Jupiter s magnetosphere with the Galileo spacecraft L. A. Frank and W. R. Paterson Department
More informationCold plasma in the jovian system
Cold plasma in the jovian system Chris Arridge 1,2 and the JuMMP Consortium 1. Mullard Space Science Laboratory, Department of Space and Climate Physics, University College London, UK. 2. The Centre for
More informationPlanetary period oscillations in Saturn s magnetosphere: Evolution of magnetic oscillation properties from southern summer to post-equinox
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117,, doi:10.1029/2011ja017444, 2012 Planetary period oscillations in Saturn s magnetosphere: Evolution of magnetic oscillation properties from southern summer to
More informationSaturn s northern auroras as observed using the Hubble Space Telescope
Saturn s northern auroras as observed using the Hubble Space Telescope J. D. Nichols a,, S. V. Badman b, E. J Bunce a, J. T. Clarke c, S. W. H. Cowley a, G. J. Hunt a, G. Provan a a Department of Physics
More information12a. Jupiter. Jupiter Data (Table 12-1) Jupiter Data: Numbers
12a. Jupiter Jupiter & Saturn data Jupiter & Saturn seen from the Earth Jupiter & Saturn rotation & structure Jupiter & Saturn clouds Jupiter & Saturn atmospheric motions Jupiter & Saturn rocky cores Jupiter
More informationTest-particle simulation
Electron elastic collision by H 2 O originating from Enceladus: Test-particle simulation Hiroyasu Tadokoro 1 and Yuto Katoh 2 1 Tokyo University of Technology, Tokyo, Japan Now at Musashino University,
More informationarxiv: v1 [astro-ph.ep] 1 Jun 2015
Saturn s aurora observed by the Cassini camera at visible wavelengths. arxiv:1506.00664v1 [astro-ph.ep] 1 Jun 2015 Ulyana A. Dyudina a, Andrew P. Ingersoll a, Shawn P. Ewald a, Danika Wellington b a Division
More informationA diffusive equilibrium model for the plasma density in Saturn s magnetosphere
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114,, doi:10.1029/2008ja013912, 2009 A diffusive equilibrium model for the plasma density in Saturn s magnetosphere A. M. Persoon, 1 D. A. Gurnett, 1 O. Santolik,
More informationRE-VISITING SATURNIAN KILOMETRIC RADIATION WITH ULYSSES/URAP
RE-VISITING SATURNIAN KILOMETRIC RADIATION WITH ULYSSES/URAP A. Lecacheux, P. Galopeau, and M. Aubier Abstract Due to its excellent sensitivity, the URAP radio astronomy experiment aboard the interplanetary
More informationSmall scale structures in Saturn s ultraviolet aurora
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 116,, doi:10.1029/2011ja016818, 2011 Small scale structures in Saturn s ultraviolet aurora D. Grodent, 1 J. Gustin, 1 J. C. Gérard, 1 A. Radioti, 1 B. Bonfond, 1 and
More informationAuroral evidence of Io s control over the magnetosphere of Jupiter
GEOPHYSICAL RESEARCH LETTERS, VOL. 39,, doi:10.1029/2011gl050253, 2012 Auroral evidence of Io s control over the magnetosphere of Jupiter B. Bonfond, 1 D. Grodent, 1 J.-C. Gérard, 1 T. Stallard, 2 J. T.
More informationAzimuthal magnetic fields in Saturn s magnetosphere: effects associated with plasma sub-corotation and the magnetopause-tail current system
Annales Geophysicae (23) 21: 179 1722 c European Geosciences Union 23 Annales Geophysicae Azimuthal magnetic fields in Saturn s magnetosphere: effects associated with plasma sub-corotation and the magnetopause-tail
More informationCassini observations of the thermal plasma in the vicinity of Saturn s main rings and the F and G rings
GEOPHYSICAL RESEARCH LETTERS, VOL. 32, L14S04, doi:10.1029/2005gl022690, 2005 Cassini observations of the thermal plasma in the vicinity of Saturn s main rings and the F and G rings R. L. Tokar, 1 R. E.
More informationModel of a variable radio period for Saturn
JOURNAL OF GEOPHYSICAL RESEARCH, VOL.???, NO., PAGES 0, Model of a variable radio period for Saturn B. Cecconi,,2 and P. Zarka, 2 Abstract. We propose an explanation for the variations at the % level of
More informationSignificance of Dungey-cycle flows in Jupiter s and Saturn s magnetospheres, and their identification on closed equatorial field lines
Ann. Geophys., 25, 941 951, 2007 European Geosciences Union 2007 Annales Geophysicae Significance of Dungey-cycle flows in Jupiter s and Saturn s magnetospheres, and their identification on closed equatorial
More informationCorrelation between energetic ion enhancements and heliospheric current sheet crossings in the outer heliosphere
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 33, L21112, doi:10.1029/2006gl027578, 2006 Correlation between energetic ion enhancements and heliospheric current sheet crossings in the
More informationJuno Status and Earth Flyby Plans. C. J. Hansen
Juno Status and Earth Flyby Plans C. J. Hansen July 2013 Juno will improve our understanding of the history of the solar system by investigating the origin and evolution of Jupiter. To accomplish this
More informationEnergetic ion spectral characteristics in the Saturnian magnetosphere using Cassini/MIMI measurements
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114,, doi:10.1029/2008ja013761, 2009 Energetic ion spectral characteristics in the Saturnian magnetosphere using Cassini/MIMI measurements K. Dialynas, 1,2 S. M. Krimigis,
More informationarxiv: v1 [physics.space-ph] 27 Apr 2018
submitted to Planetary and Space Science Journal Logo arxiv:1804.10564v1 [physics.space-ph] 27 Apr 2018 Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral
More informationA multi-instrument view of tail reconnection at Saturn
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2008ja013592, 2008 A multi-instrument view of tail reconnection at Saturn C. M. Jackman, 1 C. S. Arridge, 2,3 N. Krupp,
More informationAuroral evidence of a localized magnetic anomaly in Jupiter s northern hemisphere
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2008ja013185, 2008 Auroral evidence of a localized magnetic anomaly in Jupiter s northern hemisphere Denis Grodent, 1
More informationIon heating during geomagnetic storms measured using energetic neutral atom imaging. Amy Keesee
Ion heating during geomagnetic storms measured using energetic neutral atom imaging Amy Keesee Outline Motivation Overview of ENA measurements Charge exchange MENA and TWINS ENA instruments Calculating
More informationChapter 9 Saturn s Magnetospheric Configuration
Chapter 9 Saturn s Magnetospheric Configuration Tamas I. Gombosi, Thomas P. Armstrong, Christopher S. Arridge, Krishan K. Khurana, Stamatios M. Krimigis, Norbert Krupp, Ann M. Persoon, and Michelle F.
More informationModeling the electron and proton radiation belts of Saturn
GEOPHYSICAL RESEARCH LETTERS, VOL. 30, NO. 20, 2059, doi:10.1029/2003gl017972, 2003 Modeling the electron and proton radiation belts of Saturn D. Santos-Costa, 1 M. Blanc, 1 S. Maurice, 2 and S. J. Bolton
More informationPlasma interaction at Io and Europa
Plasma interaction at Io and Europa Camilla D. K. Harris Tidal Heating: Lessons from Io and the Jovian System Thursday, Oct 18 2018 1. Jupiter s Magnetosphere 2. Moon-Magnetosphere Plasma Interaction 3.
More informationJupiter: A fundamentally different magnetospheric interaction with the solar wind
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 34, L20106, doi:10.1029/2007gl031078, 2007 Jupiter: A fundamentally different magnetospheric interaction with the solar wind D. J. McComas
More informationTen years of Hubble Space Telescope observations of the variation of the Jovian satellites auroral footprint brightness
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja014456, 2010 Ten years of Hubble Space Telescope observations of the variation of the Jovian satellites auroral
More informationProperties of the magnetic field in the Jovian magnetotail
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A8, 1196, 10.1029/2001JA000249, 2002 Properties of the magnetic field in the Jovian magnetotail Margaret G. Kivelson and Krishan K. Khurana Institute of Geophysics
More informationA statistical analysis of the location and width of Saturn s southern auroras
European Geosciences Union 2006 Annales Geophysicae A statistical analysis of the location and width of Saturn s southern auroras S. V. Badman 1, S. W. H. Cowley 1, J.-C. Gérard 2, and D. Grodent 2 1 Department
More informationPSWS meeting Multi-wavelength observations of Jupiter's aurora during Juno s cruise phase T. Kimura (RIKEN)
PSWS meeting 2017 Multi-wavelength observations of Jupiter's aurora during Juno s cruise phase T. Kimura (RIKEN) Background p a Bagenal+14 Planetary parameters p a Earth Jupiter Saturn Spin period (hr)
More informationDavid versus Goliath 1
David versus Goliath 1 or A Comparison of the Magnetospheres between Jupiter and Earth 1 David and Goliath is a story from the Bible that is about a normal man (David) who meets a giant (Goliath) Tomas
More informationIo s volcanism controls Jupiter s radio emissions
GEOPHYSICAL RESEARCH LETTERS, VOL. 4, 67 675, doi:.2/grl.595, 23 Io s volcanism controls Jupiter s radio emissions M. Yoneda, F. Tsuchiya, H. Misawa, B. Bonfond, 2 C. Tao, 3 M. Kagitani, and S. Okano Received
More informationJupiter and Saturn: Lords of the Planets
11/5/14 Jupiter and Saturn: Lords of the Planets Guiding Questions 1. Why is the best month to see Jupiter different from one year to the next? 2. Why are there important differences between the atmospheres
More informationOuter magnetospheric structure: Jupiter and Saturn compared
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 116,, doi:10.1029/2010ja016045, 2011 Outer magnetospheric structure: Jupiter and Saturn compared D. R. Went, 1 M. G. Kivelson, 2,3 N. Achilleos, 4,5 C. S. Arridge,
More informationSaturn s polar ionospheric flows and their relation to the main auroral oval
Annales Geophysicae (2003) 21: 1 16 European Geosciences Union 2003 Annales Geophysicae Saturn s polar ionospheric flows and their relation to the main auroral oval S. W. H. Cowley 1, E. J. Bunce 1, and
More informationINNER MAGNETOSPHERE PLASMA DENSITIES. Bodo W. Reinisch and Xueqin Huang
XA0303034 INNER MAGNETOSPHERE PLASMA DENSITIES Bodo W. Reinisch and Xueqin Huang Environmental, Earth, and Atmospheric Sciences Department, Centerfor Atmospheric Research, University of Massachusetts Lowell,
More informationDetection of negative ions in the deep ionosphere of Titan during the Cassini T70 flyby
GEOPHYSICAL RESEARCH LETTERS, VOL. 39,, doi:10.1029/2012gl051714, 2012 Detection of negative ions in the deep ionosphere of Titan during the Cassini T70 flyby K. Ågren, 1 N. J. T. Edberg, 1 and J.-E. Wahlund
More informationCassini Detection of Water Group Pick-up Ions in Saturn s Toroidal Atmosphere
Cassini Detection of Water Group Pick-up Ions in Saturn s Toroidal Atmosphere R.L.Tokar 1, R.J. Wilson 1, R.E. Johnson 2, M.G. Henderson 1, M.F.Thomsen 1, M.M. Cowee 1, E.C. Sittler, Jr. 3, D.T. Young
More informationA Survey of Spacecraft Charging Events on the DMSP Spacecraft in LEO
A Survey of Spacecraft Charging Events on the DMSP Spacecraft in LEO Phillip C. Anderson Space Science Applications Laboratory The Aerospace Corporation PO Box 92957 M2/260 Los Angeles, CA 90009-2957 ph:
More informationJOVIAN BURSTY HIGH-LATITUDE EMISSIONS REVISITED: THE ULYSSES-JUPITER DISTANT ENCOUNTER
JOVIAN BURSTY HIGH-LATITUDE EMISSIONS REVISITED: THE ULYSSES-JUPITER DISTANT ENCOUNTER M. J. Reiner, M. L. Kaiser, M. D. Desch, and R. J. MacDowall Abstract New observations of Jovian bursty high-latitude
More informationWhistler-mode auroral hiss emissions observed near Saturn s B ring
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111,, doi:10.1029/2005ja011432, 2006 Whistler-mode auroral hiss emissions observed near Saturn s B ring L. Xin, 1 D. A. Gurnett, 1 O. Santolík, 1,2 W. S. Kurth, 1
More informationObservations of thermal plasmas in Jupiter s magnetotail
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A1, 1003, 10.1029/2001JA000077, 2002 Observations of thermal plasmas in Jupiter s magnetotail L. A. Frank and W. R. Paterson Department of Physics and Astronomy,
More informationMagnetosphere Magnetic Field Wobble Effects on the Dynamics of the Jovian Magnetosphere
1 Magnetosphere Magnetic Field Wobble Effects on the Dynamics of the Jovian Magnetosphere R. M. Winglee 1 and E. M. Harnett 1 (1)Department of Earth and Space Sciences University of Washington Seattle,
More informationNumerical Simulation of Jovian and Kronian Magnetospheric Configuration
Feb. 16, 2015 Numerical Simulation of Jovian and Kronian Magnetospheric Configuration Keiichiro FUKAZAWA 1, 2 1.Academic Center for Computing and Media Studies, Kyoto University 2.CREST, JST Context Jovian
More information