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1) Hawkeye Multi-Instrument Summary Plots maxmize
Resource ID:spase://VWO/DisplayData/Hawkeye/VLF/Multi.Instrument.PT51H
Start:1974-06-06 03:00:00 Observatory:Hawkeye Cadence:
Stop:1978-04-28 17:00:00 Instrument:Hawkeye VLF Resource:DisplayData
To help the user in searching through the Hawkeye data set, summary plots of the entire Hawkeye archive have been generated. Each summary plot consists of an entire orbit's worth of data from all of the instruments, along with the spacecraft position. Solar wind plasma pressure and IMF data have been added to the plots to help the user in data selection. HAWKEYE SUMMARY PLOT LAYOUT Title The orbit number is the orbit number at start of the plot time interval. Day 1 = January 1. First (top) panel Solar Wind pressure (red curve and red dots). Solar Wind IMF Bz component (in GSM) (blue dots). IMP-8 spacecraft Bz (in GSM) component (black curve). Second Panel The two numbers above the second panel are the positions of IMP-8 in degrees ( sign(y_gsm) * atan(sqrt(y_gsm^2+z_gsm^2)/x_gsm) ), at the start of and at the end of the plot time interval. Usually, if IMP-8 lies between -110 and +110 degrees it is in the solar wind. Solar Wind IMF magnetic field magnitude |B| (blue dots). IMP-8 magnetic Field magnitude |B| (black curve). Hawkeye magnetic Field magnitude |B| (red curve). Third Panel The two numbers above the third panel are: (left corner) The angle between the sun vector and spacecraft spin plane. Because the Hawkeye particle instrument's (LEPEDEA) field view is +/- 15 degrees out the the spin plane, this angle has to be less than 15 degrees in order to detect the solar wind when the spacecraft is located in the solar wind. (right corner)The spin period of the spacecraft in seconds. The electron energy-time spectrogram averaged over the solid angle sampled by LEPEDEA is plotted. Fourth Panel The ion energy-time spectrogram averaged over the solid angle sampled by LEPEDEA Fifth Panel The frequency-time spectrogram of the magnetic field as measured by the loop antenna The electron cyclotron frequency (white curve) as determined by the on-board magnetometer Sixth (bottom) Panel The electric field frequency-time spectrogram as measured by the dipole antenna The electron cyclotron frequency (white curve) as determined by the on-board magnetometer Time Axis Labels The universal time (hr:mm). The spacecraft position in Earth radii (RE) in units of RE. The spacecraft position in magnetic latitude (MLAT) in units of degrees. The spacecraft position in magnetic local time (MLT) in units of degrees. The spacecraft position in X-GSM in units of RE.

2) Hawkeye Electric and Magnetic Field Radio Frequency Spectrum Analyzer High Time Resolution maxmize
Resource ID:spase://VWO/NumericalData/Hawkeye/VLF/PT22S
Start:1974-06-08 06:45:10 Observatory:Hawkeye Cadence:22 seconds
Stop:1978-04-26 15:59:05 Instrument:Hawkeye VLF Resource:NumericalData
The CDF file contains approximately 22 second time resolution Electric and Magnetic field data, average magnetic field magnitude, and orbital position data from Hawkeye 1. The VLF experiment measured electric and magnetic fields using a 42.45-m electric dipole (tip-to-tip) which extended perpendicular to the spin axis and a search coil antenna deployed 1.58 m from the spacecraft. The electric field spectrum measurements were made in 16 logarithmically spaced frequency channels extending from 1.78 Hz to 178 kHz, and dc electric fields were also measured. The bandwidth of these channels varied from 7.5% to 30% depending on center frequency. Channel sensitivity and dynamic range were 1E-6 V/m and 100 dB, respectively. A wideband receiver was also used, with two selectable bandwidth ranges: 0.15 to 10 kHz or 1 to 45 kHz. The magnetic field spectrum was measured in eight discrete, logarithmically spaced channels from 1.78 Hz to 5.62 kHz. The bandwidth of these channels varied from 7.5% to 30% depending on frequency. The dynamic range was 100 dB, and the sensitivity ranged from 0.1 nT at 1.78 Hz to 3.4E-4 nT at 5.62 kHz. The wideband receiver described above could be used with the magnetic antenna. Each discrete channel was sampled once every 11.52 s.

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