Ulysses URAP Browse Description Ulysses URAP - Unified Radio and Plasma Wave Experiment Bundle PDS3 DATA_SET_ID = ULY-J-URAP-4-SUMM-PFR-AVG-E-10MIN-V1.0 ULY-J-URAP-4-SUMM-PFR-PEAK-E-10MIN-V1 ULY-J-URAP-4-SUMM-RAR-AVG-E-10MIN-V1.0 ULY-J-URAP-4-SUMM-RAR-AVG-E-144S-V1.0 ULY-J-URAP-4-SUMM-RAR-PEAK-E-10MIN-V1.0 ULY-J-URAP-4-SUMM-WFA-AVG-B-10MIN-V1.0 ULY-J-URAP-4-SUMM-WFA-AVG-E-10MIN-V1.0 ULY-J-URAP-4-SUMM-WFA-PEAK-B-10MIN-V1.0 ULY-J-URAP-4-SUMM-WFA-PEAK-E-10MIN-V1.0 START_TIME = 1991-11-26T00:00:00.000 STOP_TIME = 1992-06-07T23:50:00.000 PDS3 DATA_SET_RELEASE_DATE = 1998-05-01 PRODUCER_FULL_NAME = ROGER HESS SUMMARY PLOTS ============= URAP SUMMARY PLOT DESCRIPTION A URAP Summary Plot is a plot of one day of Ulysses Unified Radio and Plasma (URAP) experiment data. The URAP experiment consists of five instruments: Radio Astronomy Receiver (RAR), Plasma Frequency Receiver (PFR), Wave Form Analyzer (WFA), Fast Envelope Sampler (FES), and Sounder (SND). The Summary Plot consists of six plot panels. Data are plotted in the form of dynamic spectra (3 dimensional plots of wave intensity versus frequency and time, with the degree of darkness proportional to the wave intensity. Frequency is plotted along the vertical axis, and time along the horizontal axis. Most of the data are stretched (assigned a grey shade) between minimum and maximum data values, the maximum being the minimum plus dynamic range designated for a receiver. The specified dynamic ranges are shown at the right side of the plot, under the heading 'Dyn. Range'. A linear interpolation is done between minimum and maximum values to determine the degree of darkness of the plotted data point. Data at or below the minimum are plotted as white, and data at or above the maximum value are shown as black. The pixel-font uses a 4x4 dot pattern to represent 16 shades of gray. The plot consists of six panels, the first four of which are plotted with time along the horizontal axis. For these plots the time increment is 128 seconds, which means that 675 time steps are represented along the horizontal axis, corresponding to 24 hours of data. For data with a higher time resolution than this, the maximum data value occurring during a 128 second interval is plotted. Frequency is plotted along the vertical axis. Frequency labels such as 100K refer to 100 KHz; otherwise the labels refer to Hz. Dynamic ranges shown at the right of the panels are in telemetry units, except for the WFA ranges, which are in logarithm of floating point DPU-FFT output. The panels are described in order from top to bottom. Panel 1 This is a dynamic spectrum of RAR X antenna electric field data. The full set of 12 high receiver frequencies and 64 low receiver frequencies is plotted, with interpolation done for any missing frequencies (extrapolation is not done). The high receiver frequencies have a logarithmic spacing between approximately 50 KHz and 1 MHz. The low receiver frequencies are spaced linearly in frequency between 1.25 and 48.5 KHz. Panel 2 This panel is a dynamic spectrum of electric field data from RAR, PFR and WFA instruments. The 12 frequencies of the RAR high receiver Z antenna data are plotted. A gap separates RAR and PFR data. The PFR data is the peak data from the X antenna. Thirty-two PFR frequencies are plotted, ranging from 0.5 to 35 KHz. When the PFR is in fixed tune mode, there are 32 times as many PFR samples at a single frequency. They are spread across the 32 frequencies, to permit a better representation of the single frequency data. Twenty-four WFA frequencies from the X electric field antenna are plotted at the bottom of the panel. The low receiver frequencies range between about 0.1 to 5 Hz; the high receiver frequencies range from 9 to 448 Hz. The frequencies are approximately logarithmically spaced. The data plotted are average data from the WFA instrument. Panel 3 WFA magnetic field data are plotted here. The high receiver data (upper 12 frequencies) are always from the Y search coil. The low receiver (lower 12 frequencies) will be either Y or Z search coil data, depending on which search coil was being sampled (indicated in panel 4). Frequencies and units are as for the WFA Ex data. Panel 4 This panel indicates various instrument statuses. A dark line indicates an 'on' condition, and a light line indicates 'off'. Six status flags are shown. These are: a) RAR SUM: The flag indicates whether the RAR is in summation (X+Z) mode. A dark line indicates summation is on. There are a pair of lines for this flag. The top line of the pair indicates RAR high receiver summation, and the second line indicates low RAR receiver summation. b) RAR POLAR: This flag indicates RAR polarization mode on or off. Again, the first of the two polarization lines is for the high receiver and the next is for the low receiver. c) PFR Fast: a dark line indicates that the PFR is in fast-scan mode; a light line indicates that the mode is slow-scan; no line indicates fixed-tune (single-frequency) mode. The fixed tune frequency is shown during the fixed tune interval. Note that the PFR causes a mode (and bit rate) dependent interference in the WFA data. d) Greater than 10 Hz Ez: This flag indicates that the WFA high receiver data is from the Ez antenna (dark) or, alternatively, from the WFA Bz antenna (light). Note that neither of these types of data is plotted on the Summary Plot. (Only Ex data is plotted for the high band EWFA; only By data is plotted for the high band BWFA.) e) Less than 10 Hz By: This indicates whether the magnetic data in the low receiver is from the By (dark) or Bz (light) antenna. This flag does correspond to the data plotted for the B lo receiver. f) 1024 bps: A dark line indicates 1024 bps data. A light line indicates 512 bps. A blank corresponds to a bit rate lower than 512 bps or a data gap. Panels 5,6 The bottom two side-by-side panels (to the right of the plot label) show data for each observed FES event for high band and low band detectors. For each event, shown by a straight horizontal line, 1024 data points are taken. On the plot, however, only the maximum value of 4 contiguous points is displayed. Up to 56 individual events may be plotted. The events are plotted from bottom to top of panel in order of their occurrence. The vertical scale is time of event in hours of the day. Each event shown represents the most intense FES event observed during 49 formats (a format is 32 sec at 1024 bps). These panels are in the form of dynamic spectra; therefore the degree of darkness is proportional to the intensity of data observed during event. The FES low and hi band plots show two vertical lines at the beginning of each plot. These indicate the instrument antenna and filter status. For the FES high band the Ex antenna is flagged by a black point, and the Ez antenna by a light point. The 6-60 kHz filter is shown by black, the 2-20 kHz filter is designated by a light point and all filters with an upper limit of 6 kHz or lower are designated by a blank. For the low receiver antenna, a black point indicates Ex, a light point, Ez, and no point, the B search coils. For the low band filter, a black point indicates 2-10 Khz, a light point .6-6 kHz, and no point indicates the upper frequency limit is lower than 2 kHz. When the FES receiver is attached to the B antenna, the band is always 0.01-1 kHz. The option exists for plotting electron plasma frequency fpe, ion plasma frequency fpi and electron gyrofrequency fce as lines on the dynamic spectra. The fpe data is plotted on the PFR plot, fpi is plotted on the EWFA panel, and fce is shown on the BWFA panel. These data are obtained from Ulysses files of plasma (SWOOPS) and magnetometer (MAG) data, provided by the respective instrument teams. Various plot labels are printed in the lower left-hand corner of the Summary Plot. The first 3 lines give date of the plotted data, version number of the Summary Plot program, and date the plot was generated. The next 2 lines designate the RAR high and low receiver modes at the beginning and end of the plotted time interval. The modes are M (measure mode), L (linear sweep), and F (freeze mode). For measure mode, the list number is given after the '#' sign. For freeze mode, the frequency number follows the '#' sign. For the low receiver in measure mode, 'F' designates full list, 'E' indicates first half of list, and 'O' implies the second half of the list is used. The next line indicates RAR background type and offset. Designation for the RAR background determination is as follows: Background type '0' indicates offset values (computed minus standard background values) and dynamic ranges may be specified for the RAR receiver. Background type '1' indicates that for each frequency a background is computed from the data for that day, and a histogram of data minus background for all frequencies is used to automatically set the offset and dynamic range for each RAR receiver. The offset and range depend on the percentage of white and black pixels chosen by the user. The offsets (either chosen or computed) are shown after the '/'. The 3 offsets shown correspond to offsets for the RAR X high, X low, and Z high, respectively. The next line shows the minimum and maximum data values in telemetry units for the RAR low X data for the day. In the next 3 lines, distances and angles are given as determined using various locations, namely, Ulysses (U), Sun (S), Jupiter (J), and Earth (E). The last 2 lines give the longitude and latitude of the spacecraft in either heliographic coordinates (_H) or ecliptic coordinates (_E), as determined from the SEDR database. Backgrounds may be computed from the data. This is done separately for each RAR receiver (RAR X high, RAR X low, RAR Z high) as well as for the non-RAR receivers (PFR, WFA high, WFA low, B WFA high and B WFA low). The goal is to achieve a full utilization of the gray scale. To accomplish this, a percentage of white and black pixels is specified, typically 4% white and 4% black. Histograms of the data values are computed for each panel. The background and range are defined by these histograms; i.e. they are calculated to provide the percentages of black and white pixels specified. References ========== Barrow, C.H., and A. Lecacheux, Radio Emission from Jupiter Observed by Ulysses Before and After Encounter, Astron. Astrophys, 271, 335-343, 1993. Canu, P., N. Cornilleau-Werhlin, C. de Villedary, P.J. Kellogg, C.C. Harvey, and R.J. MacDowall, Observation of Electron Plasma Waves Upstream of Jupiter's Bow Shock by the URAP Experiment on board the Ulysses Spacecraft, in Proc. of the 2nd European Workshop on Collisionless Shocks, Issy-les-Moulineaux, France, 30 Sept-2 Oct 1992. (https://doi:10.1016/0032-0633(93)90088-J) Canu, P., N. Cornilleau-Werhlin, C. de Villedary, P.J. Kellogg, C.C. Harvey, and R.J. MacDowall, Observations of Electron Plasma Waves Upstream of the Jovian Bow Shock, Plan. Space Sci., 41, 811-822, 1993. (https://doi:10.1016/0032-0633(93)90088-J) Desch, M.D., Jupiter Radio Bursts and Particle Acceleration, Ap. J. Supp., 90 541-546, 1994. (https://doi:10.1086/191872) Desch, M.D., W.M. Farrell, and M.L. Kaiser, Asymmetries in the Io plasma torus, J. Geophys. Res., 99, 17205-17210, 1994. (https://doi.org/10.1029/94JA01615) Farrell, W.M., R.J. MacDowall, M.D. Desch, M.L. Kaiser, R.G. Stone, P.J. Kellogg, N. Lin, N. Cornilleau-Wehrlin, P. Canu, S.J. Bame, and J.L. Phillips, Ulysses Observations of Auroral Hiss at High Jovian Latitudes, Geophys. Res. Let., 20, 2259-2262, 1993. (https://doi.org/10.1029/93GL01120) Farrell, W.M., R.J. MacDowall, R.A. Hess, M.L. Kaiser, M.D. Desch, and R.G. Stone, An Interpretation of the Broadband VLF Waves near the Io Torus as Observed by Ulysses, J. Geophys. Res., 98, 21177-21188, 1993. (https://doi.org/10.1029/93JA02591) Hoang, S., N. Meyer-Vernet, M. Moncuquet, A. Lecacheux, and B.M. Pedersen, Electron Density and Temperature in the Io Torus from Ulysses thermal plasma noise measurements, Plan. Space Sci. 41, 1011-1020, 1993. (https://doi:10.1016/0032-0633(93)90105-B) Kaiser, M.L., and M.D. Desch, in Planetary Radio Emissions III, Jovian Broadband Kilometric Radiation: New Observations from Ulysses, Proc. of the Third International Workshop, Graz, Austria, H.O Rucker, S.J. Bauer, and M.L. Kaiser, eds., pp. 35-43, 1992. Kaiser, M.L., M.D. Desch, W.M. Farrell, R.J. MacDowall, R.G. Stone, A. Lecacheux, B.-M. Pedersen, and P. Zarka, Ulysses Observations of Escaping VLF Emissions from Jupiter, Geophys. Res. Let., 19, 649-652, 1992. (https://doi:10.1029/92GL00387) Kaiser, M.L., Time-variable Magnetospheric Radio Emissions from Jupiter, J. Geophys. Res., Vol. 98, pp. 18757-18765, 1993. (https://doi.org/10.1029/93JE01279) Kaiser, M.L., M.D. Desch, and W.M. Farrell, Clock-like Behavior of Jovian Continuum Radiation, Plan. Space Sci., 41, 1073-1077, 1993. (https://doi:10.1016/0032-0633(93)90110-N) Kaiser, M.L., M.D. Desch, W.M. Farrell, R.A. Hess, and R.J. MacDowall, Ordinary and Z-Mode Emissions from the Jovian Polar Region, Plan. Space Sci., 41, 977-985, 1993. (https://doi:10.1016/0032-0633(93)90102-8) Kellogg, P.J., K. Goetz, R.L. Howard, S.J. Monson, A. Balogh, and R.J. Forsyth, Measurement of Electric Fields and Plasma Flow Speeds in Jupiter's Magnetosphere, J. Geophys. Res., 98, 13307-13314, 1993. (https://doi.org/10.1029/92JA02982) Lecacheux, A., B.-M. Pedersen, P. Zarka, M.G. Aubier, M.L. Kaiser, M.D. Desch, W.M. Farrell, R.J. MacDowall, and R.G. Stone, In Ecliptic Observations of Jovian Radio Emissions by Ulysses: Comparison with Voyager Results, Geophys. Res. Let., 19, 1307-1310, 1992. (https://doi.org/10.1029/92GL01037) Lin, N., P.J. Kellogg, R.J. MacDowall, Y. Mei, N. Cornilleau- Wehrlin, P. Canu, C. de Villedary, L. Rezeau, A. Balogh, and R.J. Forsyth, ULF Waves in the Io Torus: Ulysses Observations, J. Geophys Res., 98, 21151-21162, 1993. (https://doi.org/10.1029/93JA02593) Lin, N., P.J. Kellogg, J.P. Thiessen, D. Lengyel-Frey, B.T. Tsurutani, and J.L. Phillips, Whistler Mode Waves in the Jovian Magnetosheath, J. Geophys. Res., 99, 23527, 1994. (https://doi.org/10.1029/94JA01998) MacDowall, R.J., M.L. Kaiser, M.D. Desch, W.M. Farrell, R.A. Hess, and R.G. Stone, Quasiperiodic Jovian Radio Bursts: Observations from the Ulysses Radio and Plasma Wave Experiment, Plan. Space Sci., 41, 1059-1072, 1993. (https://doi:10.1016/0032-0633(93)90109-F) Meyer-Vernet, N., S. Hoang, and M. Moncuquet, Bernstein Waves in the Io Torus: a Novel Kind of Electron Temperature Sensor, J. Geophys. Res., 98, 21163-21176, 1993. (https://doi.org/10.1029/93JA02587) Osherovich, V., R.F. Benson, J. Fainberg, R.G. Stone, and R.J. MacDowall, Sounder Stimulated Dn Resonances in Jupiter's Io Plasma Torus, J. Geophys. Res., 98, 18751-18756, 1993. (https://doi.org/10.1029/93JE01481) Reiner, M.J., J. Fainberg, R.G. Stone, R. Manning, M.L. Kaiser, M.D. Desch, B.-M. Pedersen, and P. Zarka, Source Characteristics of Jovian Narrow-Band Kilometric Radio Emissions, J. Geophys. Res., 98, 13163-13176, 1993. (https://doi.org/10.1029/93JE00536) Reiner, M.J., J. Fainberg, and R.G. Stone, Source Characteristics of Jovian Hectometric Emissions, J. Geophys. Res., 98, 18767-18777, 1993. (https://doi.org/10.1029/93JE01779) Reiner, M.J., J. Fainberg, and R.G. Stone, A New Component of Jovian Kilometric Radio Emission, J. Geophys. Res., 99, 6137-6144, 1994. (https://doi.org/10.1029/93JA03398) Stone, R.G., B.-M. Pedersen, C.C. Harvey, P. Canu, N. Cornilleau- Wehrlin, M.D. Desch, C. de Villedary, J. Fainberg, W.M. Farrell, K. Goetz, R.A. Hess, S. Hoang, M.L. Kaiser, P.J. Kellogg, A. Lecacheux, N. Lin, R.J. MacDowall, R. Manning, C.A. Meetre, N. Meyer-Vernet, M. Moncuquet, V. Osherovich, M.J. Reiner, A. Tekle, J. Thiessen, and P. Zarka, Ulysses Radio and Plasma Wave Observations in the Jupiter Environment, Science, 257, 1524-1531, 1992. (https://doi.org/10.1126/science.257.5076.1524) Thiessen, J.P., and P.J. Kellogg, Langmuir Wave Decay and Collapse in the Jovian Foreshock, Plan. Space Sci., 41, 823-832, 1993. (https://doi:10.1016/0032-0633(93)90089-K) Zarka P., B. P. Pedersen, R. Prange, P. Ferrando, S. Hoang, and P. Canu, Quelques resultats marquants de la rencontre Ulysses-Jupiter, Bulletin de la S.F.P., 90, 3-9, 1993.