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105 results for “pitch”
Wind Solar Wind Experiment (SWE) Electron Pitch-Angle Distributions (6-12s rate) (VEIS-era Mode)
Wind SWE electron pitch angle product providing electron fluxes at 30 directional bins relative to the instantaneous magnetic field direction at 16 different energy levels from the old mode (VEIS-era) of the electron instrument. The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Pitch-angle distrubutions, organized by energy, are computed from 3s measurements which are spaced either 6s or 12s in time. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 16 energy channels ranging from about 10 eV to as much as 3 keV. The exact energies at which observations are made is time-varying, and this data set reports the energy each channel observes (along with the observations themselves) at any time. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12, f_pitch_E13, f_pitch_E14, f_pitch_E15 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 16 spin-averaged energy bins). For reference, the electron speeds ( V , in cm/s) corresponding to the energy channels used, are reported in this data set.
ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM) Suprathermal Electron Pitch Angle 128-Second Level 3 Data
Suprathermal Electron Pitch Angle data from ACE/SWEPAM. Level 3 data, 128-second averages. These pitch angle distributions are calculated automatically by a computer code, and have not been validated by a person. It is therefore likely that they include some artifacts and erroneous values. These data files contain suprathermal electron pitch angle distribution functions (s^3 cm^-6) at 272 eV from the ACE/SWEPAM-E instrument. The energy channel is ~12% wide, centered at 272 eV. Pitch angle bins are 9 degrees wide, and run from 0 to 180 degrees (so 0-9, 9-18, 18-27 degrees, etc.). The break between the core and suprathermal electrons is generally around 70 eV at 1 AU, but varies around this value, at times exceeding 100 eV. Electrons at 272 eV are generally well within the suprathermal range, and the distribution at this energy typically shows very little contribution from the core population. The measured count rates at 272 eV energy provide excellent statistical significance. In addition, because of the high count rates, very few artifacts (for example due to sunlight contamination) are seen in the data at this energy. The data are in the solar wind frame, and have been corrected for the spacecraft potential. The spacecraft potential determination requires measurement of the lower energy electrons, and so the potentials calcuated at these times have been interpolated to the times of the suprathermal electron measurements. Transformation to the solar wind frame requires interpolation of the measurements (each at a different energy in the solar wind frame) to the desired energy (272 eV). Also note that the detector gains on the SWEPAM-E instrument change over time, including both slowly decreasing gains and abrupt increases when the instrument voltages are increased. The use of these data for long-term studies of the distribution function amplitudes is therefore strongly discouraged.
Wind Solar Wind Experiment (SWE) Averaged Electron Pitch Angle Distribution (12-15s rate)
Averaged Wind SWE electron pitch angle data (12-15 seconds rate) from a later mode (post-VEIS-era) of the electron instrument. The electron pitch-angle distribution averages included in this data set are derived from integrating the electron pitch-angle distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995). Averages of phase-space density (f) over key regions of the unit sphere (the set of all possible electron velocity directions) are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the averages reported in this data set. We begin this analysis with a measure of f for each pitch-angle bin, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). The f values for pitch-angles from 0-90 degrees (parallel streaming) are integrated (with angluar weighting and assumptions of gyrotropy) over this half-sphere, then averaged by dividing out the 2-pi solid angle of the half-sphere; the result being referred to as the 'f_para' average. Similarly, the 'f_perp' (flux nearly perpendicular to B) average is the result of integrating f for pitch-angles from 60-120 degrees (a region also 2-pi in solid angle). Next, the 'f_anti' (flux nearly anti-parallel to B) average covers the half-sphere of "backward" streaming electrons; having pitch-angles from 90-180 degrees. Finally, the 'f_omni' (omni-directional) average provides the integral of f over the full sphere, divided by the full 4-pi solid angle; providing a measure of total electron flux into the region of observation. The above analysis is carried out for each of 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV. For reference, the electron speeds ( V , in cm/s) corresponding to these energies are reported in this data set. Hence the data set reported here contains: f_para, f_perp, f_anti, f_omni (for each of 13 values of E), and the 13 values of V (constant, included for reference).
Wind Solar Wind Experiment (SWE) Electron Pitch-Angle Distributions (12-15s rate) (New Mode)
Wind SWE electron pitch angle product providing electron fluxes at 30 directional bins relative to the instantaneous magnetic field direction at 13 different energy levels from a later mode (post-VEIS-era) of the electron instrument. The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995). Pitch-angle distrubutions, organized by energy, are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 13 spin-averaged energy bins). For reference, the electron speeds ( V , in cm/s) corresponding to the energy channels used, are reported in this data set.
Wind 3DP EESA-LOW Electron Pitch-Angle Distributions
Wind 3DP electron pitch angle product providing electron fluxes in 8 directional bins relative to the local magnetic field direction at 15 different energy levels. Time resolution is mode- dependent, with 96s being used for the past several years and with higher resolution (e.g., 24s) used for some earlier intervals. For any given cadence, electron observations made over the full cadence interval and in all look directions in and out of the spacecraft spin plane, are folded together with the magnetic field vector as averaged over the cadence interval, to produce the pitch angle distributions. The data are calibrated science quality data.
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