/*************************** MAG Instrument **********************************/ /* MODIFICATIONS /* 920813 -- EFRIED /* Inserted values for INSTOPTICS, INSTRUMENT_MODE_DESC, REFERENCE_DESC, /* and AUTHOR_FULL_NAME /* 920916 -- EFRIED /* last changes made /* Template: Spacecraft Instrument Template - Rev: 19890121 /* Note: The following templates form part of a standard /* set for the submission of a spacecraft instrument /* to the PDS. /* /* Hierarchy: SCINSTRUMENT /* INSTINFO /* INSTDETECT /* INSTELEC /* INSTFILTER /* INSTOPTICS /* SCINSTOFFSET /* INSTSECTION /* INSTSECTINFO /* INSTSECTFOVS /* INSTSECTPARM /* INSTSECTDET /* INSTSECTELEC /* INSTSECTFILT /* INSTSECTOPTC /* INSTMODEINFO /* INSTMODESECT /* INSTREFINFO /* REFERENCE /* REFAUTHORS /* OBJECT = SCINSTRUMENT SPACECRAFT_ID = "VG2" INSTRUMENT_ID = "MAG" OBJECT = INSTINFO INSTRUMENT_NAME = "TRIAXIAL FLUXGATE MAGNETOMETER" INSTRUMENT_TYPE = "MAGNETOMETER" PI_PDS_USER_ID = "NNESS" NAIF_DATA_SET_ID = "N/A" BUILD_DATE = 1977-08-20 INSTRUMENT_MASS = 5.600000 INSTRUMENT_HEIGHT = "UNK" INSTRUMENT_LENGTH = 13.000000 INSTRUMENT_WIDTH = "UNK" INSTRUMENT_MANUFACTURER_NAME = "UNK" INSTRUMENT_SERIAL_NUMBER = "UNK" INSTRUMENT_DESC = " The magnetic field experiment carried out on the Voyager 2 mission consists of dual low field (LFM) and high field magnetometer (HFM) systems. The dual systems provide greater reliability and, in the case of the LFM's, permit the separation of the spacecraft magnetic fields from the ambient fields. Additional reliability is achieved through electronics redundancy. The wide dynamic ranges of +/- 0.002 G for the LFM's and +/- 20G for the HFM's, low quantization uncertainty (+/- 12.4, 488 nanotesla respectively), low sensor RMS noise level (0.006 nanotesla), and the use of data compaction schemes to optimize the experiment information rate all combine to permit the study of a broad spectrum of phenomena during the mission." SCIENTIFIC_OBJECTIVES_SUMMARY = " The investigations of the magnetic fields and magnetospheres of the major planetary systems in the outer Solar System and their interactions with the solar wind are primary objectives of the space exploration program to be conducted during the Voyager 2 mission. In addition, the investigation of the interplanetary magnetic field phenomena during the flights is of fundamental importance both to the understanding of the magnetospheric observations and to a number of outstanding questions in basic plasma physics and in the general dynamics of the solar wind. If the Heliospheric boundary is penetrated, accurate measurement of the interstellar magnetic field is also an important objective." INSTRUMENT_CALIBRATION_DESC = " The 13 meter Astromast booms have proved in extensive pre-flight testing to be highly rigid with respect to bending motions but soft to torsional or twisting motion. Deployment repeatability tests have shown as much as +/- 7 degrees uncertainty in the knowledge of the boom twist angle (about the boom axis) at the magnetometer sensor positions, compared with +/- 0.5 uncertainty in bend angles (rotation about axes orthogonal to the boom axis). In order to minimize sensor alignment uncertainties, a method to estimate an angular correction matrix was developed that eliminates most of the twist uncertainty and some of the bend uncertainty. A special calibration coil has been wound around the periphery of the spacecrafts high gain antenna to generate, upon command, a known magnetic field at both LFM magnetometer sensors. The difference between measurements taken when the coil is turned on and off is the coil field, independent of all external fields. Using a 20 turn coil of 1/2 amp yields nominal field intensities 0f 33.4 and 6.1 nanotesla at the inboard and outboard sensors, respectively. All magnetometer data are calibrated. Three types of in-flight calibrations are performed: 1) sensitivity calibrations, 2) zero-level calibrations, based on rolls of the spacecraft, and 3) boom-alignment calibrations based on the activation of on-board coils and resulting data (especially important when dual magnetometers are used and in strong fields for any magnetometer). Sensitivity calibrations (for 8 ranges) are done approximately once every two months (early in the mission they were done more frequently). The magnetometer team generally use one or two axis rolls (cruise maneuvers, CRSMR's) of the spacecraft for zero level calibrations as often as they are provided which is variable this is about three times per year for the so-called mini-CRSMR's, which are two axis rolls. Full CRSMR's and z-axis (only) roll-maneuvers have not occurred within the last few years (full CRSMR's and mini's differ only in the number of rolls in each). The magnetometer team usually succeeds in arguing for a series of rolls near each planetary encounter. Boom-alignment calibrations were done once after launch and around the time of the Jupiter encounter. Others have been executed, but it has been determined that the inter-sensor misalignment is small and constant. For more information, consult Behannon et al, Space Science Reviews, 1977 volume 21 pages 235-257." OPERATIONAL_CONSID_DESC = " There are no special operational considerations for the magnetometer described in Behannon et al, Space Science Reviews, 21 (1977). All magnetometer data are calibrated. Three types of in-flight calibrations are performed: 1) sensitivity calibrations, 2) zero-level calibrations, based on rolls of the spacecraft, and 3) boom-alignment calibrations based on the activation of on-board coils and resulting data (especially important when dual magnetometers are used and in strong fields for any magnetometer). Sensitivity calibrations (for 8 ranges) are done approximately once every two months (early in the mission they were done more frequently). The magnetometer team generally use one or two axis rolls (cruise maneuvers, CRSMR's) of the spacecraft for zero level calibrations as often as they are provided which is variable this is about three times per year for the so-called mini-CRSMR's, which are two axis rolls. Full CRSMR's and z-axis (only) roll-maneuvers have not occurred within the last few years (full CRSMR's and mini's differ only in the number of rolls in each). The magnetometer team usually succeeds in arguing for a series of rolls near each planetary encounter. Boom-alignment calibrations were done once after launch and around the time of the Jupiter encounter. Others have been executed, but it has been determined that the inter-sensor misalignment is small and constant." END_OBJECT = INSTINFO OBJECT = INSTDETECT DETECTOR_ID = "HFM1" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The HFM1 detector is designated as the detector which measures the i component of the vector (i, j, k)." SENSITIVITY_DESC ="N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "HFM2" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The HFM2 detector is designated as the detector which measures the j component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "HFM3" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The HFM3 detector is designated as the detector which measures the k component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "LFM1" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The LFM1 detector is designated as the detector which measures the i component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "LFM2" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The LFM2 detector is designated as the detector which measures the j component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTDETECT DETECTOR_ID = "LFM3" DETECTOR_TYPE = "RING CORE" DETECTOR_ASPECT_RATIO = 0.000000 MINIMUM_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" NOMINAL_OPERATING_TEMPERATURE = 273.000000 DETECTOR_DESC = " Both high and low field magnetometer sensors utilize a ring core geometry and thus have lower drive power requirements and better zero level stability than other types of fluxgates and are smaller in size (Acuna, 1974). The cores consist of an advanced molybdenum alloy, especially developed in cooperation with the Naval Surface Weapons Center, White Oak, Maryland, which exhibits extremely low noise and high stability characteristics. The use of this alloy and the ring core sensor geometry thus allows the realization of compact, low power, ultrastable fluxgate sensors with a noise performance that is improved almost an order of magnitude over the best previously flown fluxgate sensors. The HFM's use specially processed miniature ring cores (1cm diameter) which minimize the power required to measure large fields. This description is taken directly from Behannon et al, Space Science Reviews (1977). The LFM3 detector is designated as the detector which measures the k component of the vector (i,j,k)." SENSITIVITY_DESC = "N/A" END_OBJECT = INSTDETECT OBJECT = INSTELEC ELECTRONICS_ID = "P" ELECTRONICS_DESC = " P - primary system. The experiment electronics instrumentation consists of the flux-gate magnetometer electronics and associated controls, and the calibration and data processing electronics. Complete redundancy is provided for the analog to digital converters, data and status readout buffers, command decoders and power converters. Thus not only can the two magnetometers of a system be interchanged, but considerable cross-strapping within the electronics permits interchange of critical internal functions as well. This significantly reduces the impact of single-component failure on the ability of the experiment to continue successful operation during the mission duration of > 4 years. This description is directly transposed from Behannon et al, Space Science Reviews, 21 (1977) page 249." END_OBJECT = INSTELEC OBJECT = INSTELEC ELECTRONICS_ID = "S" ELECTRONICS_DESC = " S - secondary system. The experiment electronics instrumentation consists of the flux-gate magnetometer electronics and associated controls, and the calibration and data processing electronics. Complete redundancy is provided for the analog to digital converters, data and status readout buffers, command decoders and power converters. Thus not only can the two magnetometers of a system be interchanged, but considerable cross-strapping within the electronics permits interchange of critical internal functions as well. This significantly reduces the impact of single-component failure on the ability of the experiment to continue successful operation during the mission duration of > 4 years. This description is directly transposed from Behannon et al, Space Science Reviews, 21 (1977) page 249." END_OBJECT = INSTELEC OBJECT = INSTFILTER FILTER_NUMBER = "N/A" FILTER_NAME = "N/A" FILTER_TYPE = "N/A" MINIMUM_WAVELENGTH = "N/A" CENTER_FILTER_WAVELENGTH = "N/A" MAXIMUM_WAVELENGTH = "N/A" MEASUREMENT_WAVE_CALBRT_DESC = "N/A" END_OBJECT = INSTFILTER OBJECT = INSTOPTICS TELESCOPE_ID = "N/A" TELESCOPE_FOCAL_LENGTH = "N/A" TELESCOPE_DIAMETER = "N/A" TELESCOPE_F_NUMBER = "N/A" TELESCOPE_RESOLUTION = "N/A" TELESCOPE_TRANSMITTANCE = "N/A" TELESCOPE_T_NUMBER = "N/A" TELESCOPE_T_NUMBER_ERROR = "N/A" TELESCOPE_SERIAL_NUMBER = "N/A" OPTICS_DESC = "N/A" END_OBJECT = INSTOPTICS OBJECT = SCINSTOFFSET PLATFORM_OR_MOUNTING_NAME = "MAGNETOMETER BOOM" CONE_OFFSET_ANGLE = "N/A" CROSS_CONE_OFFSET_ANGLE = "N/A" TWIST_OFFSET_ANGLE = "N/A" INSTRUMENT_MOUNTING_DESC = " The LFM is located near the tip of the boom and the HFM is located near the spacecraft body. See Behannon et al, 1977 for a picture of the actual magnetometer mounting positions and a complete description." END_OBJECT = SCINSTOFFSET OBJECT = INSTSECTION SECTION_ID = "HFM" OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = "UNK" SAMPLE_BITS = 12 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = "N/A" VERTICAL_FOV = "N/A" FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "MAGNETIC FIELD COMPONENT" MINIMUM_INSTRUMENT_PARAMETER = -2000000.000000 MAXIMUM_INSTRUMENT_PARAMETER = 2000000.000000 NOISE_LEVEL = 0.006000 INSTRUMENT_PARAMETER_UNIT = "NANOTESLA" SAMPLING_PARAMETER_NAME = "TIME" MINIMUM_SAMPLING_PARAMETER = 0.600000 MAXIMUM_SAMPLING_PARAMETER = 0.600000 SAMPLING_PARAMETER_INTERVAL = 0.600000 SAMPLING_PARAMETER_RESOLUTION = 0.600000 SAMPLING_PARAMETER_UNIT = "SECOND" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "HFM1" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "HFM2" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "HFM3" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = "P" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTELEC ELECTRONICS_ID = "S" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "HFM1" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTSECTION SECTION_ID = "LFM" OBJECT = INSTSECTINFO SCAN_MODE_ID = "N/A" DATA_RATE = "UNK" SAMPLE_BITS = 12 TOTAL_FOVS = 1 OBJECT = INSTSECTFOVS FOV_SHAPE_NAME = "N/A" HORIZONTAL_PIXEL_FOV = "N/A" VERTICAL_PIXEL_FOV = "N/A" HORIZONTAL_FOV = "N/A" VERTICAL_FOV = "N/A" FOVS = 1 END_OBJECT = INSTSECTFOVS END_OBJECT = INSTSECTINFO OBJECT = INSTSECTPARM INSTRUMENT_PARAMETER_NAME = "MAGNETIC FIELD COMPONENT" MINIMUM_INSTRUMENT_PARAMETER = -50000.000000 MAXIMUM_INSTRUMENT_PARAMETER = 50000.000000 NOISE_LEVEL = 0.006000 INSTRUMENT_PARAMETER_UNIT = "NANOTESLA" SAMPLING_PARAMETER_NAME = "TIME" MINIMUM_SAMPLING_PARAMETER = 0.060000 MAXIMUM_SAMPLING_PARAMETER = 0.060000 SAMPLING_PARAMETER_INTERVAL = 0.060000 SAMPLING_PARAMETER_RESOLUTION = 0.060000 SAMPLING_PARAMETER_UNIT = "SECOND" END_OBJECT = INSTSECTPARM OBJECT = INSTSECTDET DETECTOR_ID = "LFM1" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "LFM2" END_OBJECT = INSTSECTDET OBJECT = INSTSECTDET DETECTOR_ID = "LFM3" END_OBJECT = INSTSECTDET OBJECT = INSTSECTELEC ELECTRONICS_ID = "P" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTELEC ELECTRONICS_ID = "S" END_OBJECT = INSTSECTELEC OBJECT = INSTSECTFILT FILTER_NUMBER = "LFM1" END_OBJECT = INSTSECTFILT OBJECT = INSTSECTOPTC TELESCOPE_ID = "N/A" END_OBJECT = INSTSECTOPTC END_OBJECT = INSTSECTION OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "CRUISE" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "REALTIME" INSTRUMENT_POWER_CONSUMPTION = 2.200000 INSTRUMENT_MODE_DESC = " In the CRUISE mode, only the LFM subsystem is operating. The basic sample rate in this mode is 50/3 vectors/second." OBJECT = INSTMODESECT SECTION_ID = "LFM" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTMODEINFO INSTRUMENT_MODE_ID = "ENCOUNTER" GAIN_MODE_ID = "N/A" DATA_PATH_TYPE = "REALTIME" INSTRUMENT_POWER_CONSUMPTION = 2.200000 INSTRUMENT_MODE_DESC = " In the ENCOUNTER mode, both LFM and HFM subsystems are operating. The basic sample rate in this mode is 50/3 vectors/second for the LFM system and 5/3 vectors/second for the HFM system." OBJECT = INSTMODESECT SECTION_ID = "HFM" END_OBJECT = INSTMODESECT OBJECT = INSTMODESECT SECTION_ID = "LFM" END_OBJECT = INSTMODESECT END_OBJECT = INSTMODEINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "ACUNAETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "Z3 ZONAL HARMONIC MODEL SATURN'S MAGNETIC FIELD ANALYSIS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Acuna, M. H., J. E. P. Connerney, and N. F. Ness, The Z3 Zonal Harmonic Model of Saturn's Magnetic Field: Analysis and Implications, J. Geophys. Res., 88, 8771, 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1977" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD EXPERIMENT FOR VOYAGER 1 AND 2" JOURNAL_NAME = "SPACE SCIENCE REVIEWS" PUBLICATION_DATE = 1977 REFERENCE_DESC = " Behannon K. W., M. H. Acuna, L. F. Burlaga, R. P. Lepping, N. F. Ness, and F. M. Neubauer, Magnetic Field Experiment for Voyagers 1 and 2, Space Science Reviews, 21, 235, 1977." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "F.M. NEUBAUER" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "JOVIAN MAGNETOTAIL AND CURRENT SHEET" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Behannon, K. W., L. F. Burlaga, and N. F. Ness, The Jovian Magnetotail and its Current Sheet, J. Geophys. Res., 86, 8385, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "STRUCTURE DYNAMICS SATURN'S OUTER MAGNETOSPHERE BOUNDARY" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Behannon, K. W., R. P. Lepping, and N. F. Ness, Structure and Dynamics of Saturn's Outer Magnetosphere and Boundary Regions, J. Geophys. Res., 88, 8791, 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "BEHANNONETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETOTAIL URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Behannon, K. W., et al, The Magnetotail of Uranus, J. Geophys. Res., 92, 366, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MODELING JOVIAN CURRENT SHEET AND INNER MAGNETOSPHERE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Connerney, J. E. P., M. H. Acuna, and N. F. Ness, Modeling of the Jovian Current Sheet and Inner Magnetosphere, J. Geophys Res., 86, 8370, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "CURRENTS IN SATURN'S MAGNETOSPHERE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Connerney, J. E. P., M. H. Acuna, and N. F. Ness, Currents in Saturn's Magnetosphere, J. Geophys. Res., 88, 8779, 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "CONNERNEYETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Connerney, J. E. P., M. H. Acuna, and N. F. Ness, The Magnetic Field of Uranus, J. Geophys. Res., 92, 336, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "J.E.P. CONNERNEY" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.H. ACUNA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "DESCH&KAISER1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "VOYAGER MEASUREMENT ROTATION PERIOD SATURN MAGNETIC FIELD" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH LETTERS" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Desch, M.D., and M.L. Kaiser, Voyager Measurement of the Rotation Period of Saturn's Magnetic Field, J. Geophys. Res. Letters, 8, 253, 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.D. DESCH" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "M.L. KAISER" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "DESSLER1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "PHYSICS OF JOVIAN MAGNETOSPHERE COORDINATE SYSTEMS" JOURNAL_NAME = "PHYSICS OF THE JOVIAN MAGNETOSPHERE" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Dessler, A. J. ed., Physics of the Jovian Magnetosphere, Cambridge University Press, London, Appendix B - Coordinate Systems, Dessler, A. J., 1983." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "A.J. DESSLER" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1981" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD AND PLASMA FLOW IN JUPITER MAGNETOSHEATH" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1981 REFERENCE_DESC = " Lepping R. P., et al, Observations of the Magnetic Field and Plasma Flow in the Jupiter Magnetosheath, J. Geophys. Res., 86, 8145 1981." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "LEPPINGETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "SURFACE WAVES URANUS MAGNETOPAUSE" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Lepping, R. P., L. F. Burlaga, and L. W. Klein, Surface Waves on Uranus' Magnetopause, J. Geophys, Res., 92, 353, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.F. BURLAGA" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "L.W. KLIEN" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "R.P. LEPPING" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "NESSETAL1979A" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES AT JUPITER BY VOYAGER 2" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1979 REFERENCE_DESC = " Ness, N. F., et al, Magnetic Field Studies at Jupiter by Voyager 2: Preliminary Results, Science, 206, 966, 1979." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "NESSETAL1983" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES VOYAGER 2 SATURN PRELIMINARY" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1983 REFERENCE_DESC = " Ness, N. F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "NESSETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD STUDIES URANUS" JOURNAL_NAME = "SCIENCE" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Ness, N. F., et al, Magnetic Fields at Uranus, Science, 233, 85, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO OBJECT = INSTREFINFO REFERENCE_KEY_ID = "VOIGTETAL1986" OBJECT = REFERENCE DOCUMENT_TOPIC_TYPE = "MAGNETIC FIELD CURRENT STRUCTURES MAGNETOSPHERE URANUS" JOURNAL_NAME = "JOURNAL OF GEOPHYSICAL RESEARCH" PUBLICATION_DATE = 1986 REFERENCE_DESC = " Voigt, G. H., K. W. Behannon, and N. F. Ness, Magnetic Field and Current Structures in the Magnetosphere of Uranus, J. Geophys. Res., 92, 346, 1986." OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "G.H. VOIGT" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "K.W. BEHANNON" END_OBJECT = REFAUTHORS OBJECT = REFAUTHORS AUTHOR_FULL_NAME = "N.F. NESS" END_OBJECT = REFAUTHORS END_OBJECT = REFERENCE END_OBJECT = INSTREFINFO END_OBJECT = SCINSTRUMENT