This file contains numerical moments computed from measurements of the Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., Rev. Sci. Inst., in press 1993]. The moments are presented in s/c coordinates: the z-axis is aligned with the spin axis, which points radially toward the center of the Earth; the x-axis is in the plane containing the spacecraft spin axis and the spin axis of the Earth, with +X generally northward; and the y-axis points generally eastward. Polar angles are measured relative to the spin axis (+Z), and azimuthal angles are measured around the z-axis, with zero along the +X direction. The moments are computed for three 'species': lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 21.5 secs after the ion measurements. Epoch is the measurement time appropriate for the ions. The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined. Tperp and Tpara are obtained from diagonalization of the 3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by non-zero 'SCALEMIN' values in this file. A quality flag value of 1 indicates that the values are suspect because of unreliable location info.
Created SEP 1992 Modified JAN 1993 Electron time tags removed Mag Latitude added Local time added Post Gap flag added Ratio variables changed Modified SEP 1994 Changes noted in mail message from M.Kessel New Dict keys added sep95 Added new global attr. and variables from M.Kessel Oct 98
This is a virtual variable generated by read_myCDF w/ useof the data in the sc_pos_geo variable and a conversion routinespecified in the function attribute, namely conv_pos
This is a virtual variable generated by read_myCDF w/ useof the data in the sc_pos_geo variable and a conversion routinespecified in the function attribute, namely conv_pos
This file contains numerical moments computed from measurements of the Los Alamos Magnetospheric Plasma Analyzer (MPA) [Bame et al., Rev. Sci. Inst., in press 1993]. The moments are presented in s/c coordinates: the z-axis is aligned with the spin axis, which points radially toward the center of the Earth; the x-axis is in the plane containing the spacecraft spin axis and the spin axis of the Earth, with +X generally northward; and the y-axis points generally eastward. Polar angles are measured relative to the spin axis (+Z), and azimuthal angles are measured around the z-axis, with zero along the +X direction. The moments are computed for three 'species': lop (low-ener. ions, ~1eV/e-~130eV/e); hip (hi-ener. ions, ~130eV/e-~45keV/e); alle (electrons, ~30eV - ~45keV ). The electron measurements are obtained 21.5 secs after the ion measurements. Epoch is the measurement time appropriate for the ions. The moments are computed after the fluxes are corrected for background and s/c potential. Algorithms for these corrections are relatively unsophisticated, so the moments are suspect during times of high background and/or high spacecraft potential. Because the determined spacecraft potential is not very precise, the magnitude of the low-energy ion flow velocity is probably not accurate, but the flow direction is well determined. Tperp and Tpara are obtained from diagonalization of the 3-dimensional temperature matrix, with the parallel direction assigned to the eigenvalue which is most different from the other two. The corresponding eigenvector is the symmetry axis of the distribution and should be equivalent to the magnetic field direction. The eigenvalue ratio Tperp/Tmid, which is provided for each species, is a measure of the symmetry of the distribution and should be ~1.0 for a good determination. Several of the parameters have a fairly high daily dynamic range and for survey purposes are best displayed logarithmically. These parameters are indicated by non-zero 'SCALEMIN' values in this file. A quality flag value of 1 indicates that the values are suspect because of unreliable location info.
Created SEP 1992 Modified JAN 1993 Electron time tags removed Mag Latitude added Local time added Post Gap flag added Ratio variables changed Modified SEP 1994 Changes noted in mail message from M.Kessel New Dict keys added sep95 Added new global attr. and variables from M.Kessel Oct 98
This is a virtual variable generated by read_myCDF w/ useof the data in the sc_pos_geo variable and a conversion routinespecified in the function attribute, namely conv_pos
This is a virtual variable generated by read_myCDF w/ useof the data in the sc_pos_geo variable and a conversion routinespecified in the function attribute, namely conv_pos
MAG - ACE Magnetic Field Experiment References: http://www.srl.caltech.edu/ACE/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 9/7/01 12/04/02: Fixed description of Epoch time variable.
Data Quality Flag: 0 = good; 1 = S/C Maneuver & subsequent high-nutation period (~4 hr) 2 = Bad data/missing data
SWEPAM - Solar Wind Electron Proton Alpha Monitor References: http://www.srl.caltech.edu/ACE/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 02/23/00. 12/04/02: Fixed alpha/proton ratio precision bug. 12/04/02: Fixed description of Epoch time variable.
ACE s/c position, 3 comp. in GSE coord.
ACE s/c position, 3 comp. in GSM coord.
Label for ACE Position (GSE)
Vp is the solar wind proton speed, or more generally just the solar wind (bulk) speed. It is obtained by integrating the ion (proton) distribution function.
Np is the proton number density in units of cm-3, as calculated by integrating the ion distribution function.
Solar Wind Velocity in GSE coord., 3 components
Solar Wind Velocity in GSM coord., 3 comp.
Solar Wind Velocity in RTN coord., 3 components
Alpha ratio (Na/Np) - is the ratio of the number density of helium++ ions to the number density of protons.
The radial component of the proton temperature is the (1,1) component of the temperature tensor, along the radial direction. It is obtained by integration of the ion (proton) distribution function.
The Electron, Proton, and Alpha Monitor (EPAM) is composed of five telescope apertures of three different types. Two Low Energy Foil Spectrometers (LEFS) measure the flux and direction of electrons above 30 keV (geometry factor = 0.397 cm2*sr), two Low Energy Magnetic Spectrometers (LEMS) measure the flux and direction of ions greater than 50 keV (geometry factor = 0.48 cm2*sr), and the Composition Aperture (CA) measures the elemental composition of the ions (geometry factor = 0.24 cm2*sr). The telescopes use the spin of the spacecraft to sweep the full sky. Solid-state detectors are used to measure the energy and composition of the incoming particles. For more information about the EPAM instrument, visit the EPAM Home Page at JHU/APL: http://sd-www.jhuapl.edu/ACE/EPAM/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Public Release 01/28/03 (Version 3) 11/11/04: Improved metadata (Version 4)
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MAG - ACE Magnetic Field Experiment References: http://www.srl.caltech.edu/ACE/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 9/6/01 12/04/02: Fixed description of Epoch time variable.
Data Quality Flag: 0 = good; 1 = S/C Maneuver & subsequent high-nutation period (~4 hr) 2 = Bad data/missing data
The Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer(ACE) spacecraft is intended to be a major step in ascertaining the isotopic composition of the Galactic Cosmic Rays(GCRs) and hence a major step in determining their origin. The GCRs consist, by number, primarily of hydrogen nuclei(~92%) and helium nuclei (~7%). The energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to ~100 MeV/nucleon. During large solar events, when particle fluxes can increase over quiet-time values by factors of up to 10000, CRIS measures the isotopic composition of the solar corona, while during solar quiet times CRIS measures the isotopes of low-energy Galactic cosmic rays and the composition of the anomalous cosmic rays which are thought to originate in the nearby interstellar medium. The solar energetic particle measurements are useful to further our understanding of the Sun, while also providing a baseline for comparison with the Galactic cosmic ray measurements carried out by CRIS. CRIS has a geometry factor of ~40 cm2--sr, which is significantly larger than previous satellite solar particle isotope spectrometers. It is also designed to provide excellent mass resolution during the extremely high particle flux conditions which occur during large solar particle events.
Initial Release 02/08/05
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The Electron, Proton, and Alpha Monitor (EPAM) is composed of five telescope apertures of three different types. Two Low Energy Foil Spectrometers (LEFS) measure the flux and direction of electrons above 30 keV (geometry factor = 0.397 cm2*sr), two Low Energy Magnetic Spectrometers (LEMS) measure the flux and direction of ions greater than 50 keV (geometry factor = 0.48 cm2*sr), and the Composition Aperture (CA) measures the elemental composition of the ions (geometry factor = 0.24 cm2*sr). The telescopes use the spin of the spacecraft to sweep the full sky. Solid-state detectors are used to measure the energy and composition of the incoming particles. For more information about the EPAM instrument, visit the EPAM Home Page at JHU/APL: http://sd-www.jhuapl.edu/ACE/EPAM/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Public Release 01/28/03 (Version 3) 11/11/04: Improved metadata (Version 4)
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MAG - ACE Magnetic Field Experiment References: http://www.srl.caltech.edu/ACE/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 9/6/01 12/04/02: Fixed description of Epoch time variable.
Data Quality Flag: 0 = good; 1 = S/C Maneuver & subsequent high-nutation period (~4 hr) 2 = Bad data/missing data
The SEPICA Instrument on ACE The Solar Energetic Particle Ionic Charge Analyzer is the sensor on ACE, which is used to determine the charge state distribution of energetic particle distributions. SEPICA is designed to measure the ionic charge state, Q, the kinetic energy, E, and the nuclear charge, Z, of energetic ions above 0.2 MeV/Nuc. This includes ions accelerated in solar flares as well as in interplanetary space during energetic storm particle (ESP) and co-rotating interaction region (CIR) events. For low mass numbers SEPICA also separates isotopes -- for example, 3He and 4He. For more information about the SEPICA instrument, visit the SEPICA Home Page at University of New Hampshire: http://www.ssg.sr.unh.edu/tof/Missions/Ace/index.html?sepicamain.html The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 07/27/07
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The Solar Isotope Spectrometer (SIS) is designed to provide high resolution measurements of the isotopic composition of energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to ~100 MeV/nucleon. During large solar events, when particle fluxes can increase over quiet-time values by factors of up to 10000, SIS measures the isotopic composition of the solar corona, while during solar quiet times SIS measures the isotopes of low-energy Galactic cosmic rays and the composition of the anomalous cosmic rays which are thought to originate in the nearby interstellar medium. The solar energetic particle measurements are useful to further our understanding of the Sun, while also providing a baseline for comparison with the Galactic cosmic ray measurements carried out by CRIS. SIS has a geometry factor of ~40 cm2--sr, which is significantly larger than previous satellite solar particle isotope spectrometers. It is also designed to provide excellent mass resolution during the extremely high particle flux conditions which occur during large solar particle events.
Initial Release 02/08/05
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SWEPAM - Solar Wind Electron Proton Alpha Monitor References: http://www.srl.caltech.edu/ACE/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 04/04/02. 12/04/02: Fixed alpha/proton ratio precision bug. 12/04/02: Fixed description of Epoch time variable. 12/04/02: -9999.9 fill-data values changed to -1.0e+31.
ACE s/c position, 3 comp. in GSE coord.
ACE s/c position, 3 comp. in GSM coord.
Label for ACE Position (GSE)
Vp is the solar wind proton speed, or more generally just the solar wind (bulk) speed. It is obtained by integrating the ion (proton) distribution function.
Np is the proton number density in units of cm-3, as calculated by integrating the ion distribution function.
Solar Wind Velocity in GSE coord., 3 components
Solar Wind Velocity in GSM coord., 3 comp.
Solar Wind Velocity in RTN coord., 3 components
Alpha ratio (Na/Np) - is the ratio of the number density of helium++ ions to the number density of protons.
The radial component of the proton temperature is the (1,1) component of the temperature tensor, along the radial direction. It is obtained by integration of the ion (proton) distribution function.
SWICS - The Solar Wind Ion Composition Spectrometer - determines uniquely the chemical and ionic-charge composition of the solar wind, the temperatures and mean speeds of major solar wind ions, at all speeds above 300 km/s (protons) and 170 km/s (Fe+16), and resolves H and He isotopes of solar and interstellar sources. SWICS measures the distribution functions of the interstellar cloud and dust cloud pickup ions up to energies of 100 keV/e. For more information about the SWICS instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace. The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 11/08/05
C6to5 is the C+6/C+5 Solar Wind charge_state Ratio
avqC is the Carbon Solar Wind average charge state
FetoO is the Fe/O Solar Wind elemental abundance ratio
avqFe is the Iron Solar Wind average charge state
O7to6 is the O+7/O+6 Solar Wind charge_state Ratio
avqO is the Oxygen Solar Wind average charge state
FetoO_qual is the quality flag for the Fe/O ratio. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
C6toC5_qual is the quality flag for the C+6/C+5 ratio. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
avqC_qual is the quality flag for the avqC average charge state. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
avqFe_qual is the quality flag for the avqFe average charge state. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
O7toO6_qual is the quality flag for the O+7/O+6 ratio. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
avqO_qual is the quality flag for the avqO average charge state. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
C5_qual is the quality flag for the C+5 speed and thermal speed data. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
Fe10_qual is the quality flag for the Fe+10 speed and thermal speed data. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
O6_qual is the quality flag for the O+6 speed and thermal speed data. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
He_qual is the quality flag for the helium speed and density data. 0: good quality. 1: low statistics. 2: very low stats.4: non-thermal dist. 5: 1 + 4. 6: 2 + 4. 8: Insufficient data to construct dist function.
vthC5 is the thermal speed of Carbon+5 in the solar wind, in km/s.
vC5 is the mean Carbon+5 ion speed in the solar wind, in km/s.
nHe2 is the number density of He++ ions in the solar wind, in #/cm^3
vthHe2 is the thermal speed of He++ in the solar wind, in km/s.
vHe2 is the mean Helium++ ion speed in the solar wind, in km/s.
vthFe10 is the thermal speed of Fe+10 in the solar wind, in km/s.
vFe10 is the mean Fe+10 ion speed in the solar wind, in km/s.
vthO6 is the thermal speed of Oxygen+6 in the solar wind, in km/s.
vO6 is the mean Oxygen+6 ion speed in the solar wind, in km/s.
SW_type is a rough classification of solar wind type based on functions of O7+/O6+ vs proton speed (Zhou 2008). 0: Streamer Wind. 1: Coronal Hole Wind. 2: Coronal Mass Ejection.
The ULEIS Instrument on ACE The Ultra Low Energy Isotope Spectrometer measures ion fluxes over the charge range from H through Ni from about 20 keV/nucleon to 10 MeV/nucleon, thus covering both suprathermal and energetic particle energy ranges. Exploratory measurements of ultra-heavy species (mass range above Ni) will also be performed in a more limited energy range near 0.5 MeV/nucleon. ULEIS will be studying the elemental and isotopic composition of solar energetic particles, and the mechanisms by which these particles are energized in the solar corona. ULEIS will also investigate mechanisms by which supersonic interplanetary shock waves energize ions. For more information about the ULEIS instrument, visit the ULEIS Home Page at JHU/APL: http://sd-www.jhuapl.edu/ACE/ULEIS/ The quality of ACE level 2 data is such that it is suitable for serious scientific study. However, to avoid confusion and misunderstanding, it is recommended that users consult with the appropriate ACE team members before publishing work derived from the data. The ACE team has worked hard to ensure that the level 2 data are free from errors, but the team cannot accept responsibility for erroneous data, or for misunderstandings about how the data may be used. This is especially true if the appropriate ACE team members are not consulted before publication. At the very least, preprints should be forwarded to the ACE team before publication.
Initial Release 07/19/04
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The Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer(ACE) spacecraft is intended to be a major step in ascertaining the isotopic composition of the Galactic Cosmic Rays(GCRs) and hence a major step in determining their origin. The GCRs consist, by number, primarily of hydrogen nuclei(~92%) and helium nuclei (~7%). The energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to ~100 MeV/nucleon. During large solar events, when particle fluxes can increase over quiet-time values by factors of up to 10000, CRIS measures the isotopic composition of the solar corona, while during solar quiet times CRIS measures the isotopes of low-energy Galactic cosmic rays and the composition of the anomalous cosmic rays which are thought to originate in the nearby interstellar medium. The solar energetic particle measurements are useful to further our understanding of the Sun, while also providing a baseline for comparison with the Galactic cosmic ray measurements carried out by CRIS. CRIS has a geometry factor of ~40 cm2--sr, which is significantly larger than previous satellite solar particle isotope spectrometers. It is also designed to provide excellent mass resolution during the extremely high particle flux conditions which occur during large solar particle events.
Initial Release 02/08/05
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EPAM - ACE Electron, Proton, and Alpha Monitor References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. EPAM Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 04/30/99
175-315 keV Electron Flux (5 min)
38-53 keV Electron Flux (5 min)
1060-1910 keV Ion Flux (5 min)
112-187 keV Ion Flux (5 min)
310-580 keV Ion Flux (5 min)
47-65 keV Ion Flux (5 min)
0.48-0.97 MeV (5 min)
if 0 ignore data (5 min)
Pre-generated PWG plots
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MAG - ACE Magnetic Field Experiment References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. MAG Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 11/10/98
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SIS - ACE Solar Isotope Spectrometer References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SIS Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 04/10/99
Note that the energy intervals for the dominant elements C, N, and O all differ somewhat from the nominal values of 10 to 15 MeV/nuc, and that the relative abundance of the contributing elements depend on the source of the particles.
Note that the energy intervals for the most abundant elements C, N, and O all differ somewhat from the nominal values of 7 to 10 MeV/nuc.
Proton Flux E>10 MeV - During solar quiet times, these fluxes are contaminated by background from particles entering from the sides of the instrument.
Proton Flux E>30 MeV - During solar quiet times, these fluxes are contaminated by background from particles entering from the sides of the instrument.
Note that the quoted energy interval of ~9 to 21 MeV/nuc is strictly valid only for Si. For Ne the corresponding interval is ~8 to ~17 MeV/nuc, while for Fe it is ~12 to ~26 MeV/nuc.
SWEPAM - Solar Wind Electron Proton Alpha Monitor References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SWEPAM Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 12/01/98
He_ratio is the ratio of the number density of helium++ ions to the number density of protons.
Vp is the solar wind proton speed, or more generally just the solar wind (bulk) speed. It is obtained by integrating the ion (proton) distribution function.
Np is the proton number density in units of cm-3, as calculated by integrating the ion distribution function.
He_ratio is the ratio of the number density of helium++ ions to the number density of protons.
Vp is the solar wind proton speed, or more generally just the solar wind (bulk) speed. It is obtained by integrating the ion (proton) distribution function.
Np is the proton number density in units of cm-3, as calculated by integrating the ion distribution function.
The radial component of the proton temperature is the (1,1) component of the temperature tensor, along the radial direction. It is obtained by integration of the ion (proton) distribution function.
The radial component of the proton temperature is the (1,1) component of the temperature tensor, along the radial direction. It is obtained by integration of the ion (proton) distribution function.
EPAM - ACE Electron, Proton, and Alpha Monitor References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. EPAM Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 08/26/99
175-315 keV Electron Flux (1 hr)
38-53 keV Electron Flux (1 hr)
1060-1910 keV Ion Flux (1 hr)
112-187 keV Ion Flux (1 hr)
310-580 keV Ion Flux (1 hr)
47-65 keV Ion Flux (1 hr)
0.48-0.97 MeV (1 hr)
if 0 ignore data (1 hr)
MAG - ACE Magnetic Field Experiment References: http:// www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. MAG Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 11/10/98
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SWEPAM - Solar Wind Electron Proton Alpha Monitor References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SWEPAM Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 12/01/98
He_ratio is the ratio of the number density of helium++ ions to the number density of protons.
Vp is the solar wind proton speed, or more generally just the solar wind (bulk) speed. It is obtained by integrating the ion (proton) distribution function.
Np is the proton number density in units of cm-3, as calculated by integrating the ion distribution function.
He_ratio is the ratio of the number density of helium++ ions to the number density of protons.
Vp is the solar wind proton speed, or more generally just the solar wind (bulk) speed. It is obtained by integrating the ion (proton) distribution function.
Np is the proton number density in units of cm-3, as calculated by integrating the ion distribution function.
The radial component of the proton temperature is the (1,1) component of the temperature tensor, along the radial direction. It is obtained by integration of the ion (proton) distribution function.
The radial component of the proton temperature is the (1,1) component of the temperature tensor, along the radial direction. It is obtained by integration of the ion (proton) distribution function.
MAG - ACE Magnetic Field Experiment References: http://www.srl.caltech.edu/ACE/ ACE browse data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. MAG Browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed studies.
Initial Release 11/10/98
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GROUP 1 Satellite Resolution Factor
ace 720 1
Coord/ Min/Max Range Filter Filter
Component Output Markers Minimum Maximum Mins/Maxes
GSE X YES - - - - - -
GSE Y YES - - - - - -
GSE Z YES - - - - - -
GSE Lat YES - - - - - -
GSE Lon YES - - - - - -
Addtnl Min/Max Range Filter Filter
Options Output Markers Minimum Maximum Mins/Maxes
dEarth YES - - - -
Formats and units:
Day/Time format: YYYY DDD HH:MM
Degrees/Hemisphere format: Decimal degrees with 2 place(s).
Longitude 0 to 360, latitude -90 to 90.
Distance format: Kilometers with 2 place(s).
Originated 03/14/96
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This ionogram was digitized from the original ALOUETTE 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at http://nssdc/space/isis/isis-status.html
created April 1998
This variable could be used as x-axis on amplitude spectrograms if fixed part is subtracted.
Virtual variable.
This variable could be used as x-axis on amplitude spectrograms if fixed part is subtracted.
time of frequency markers
seperates the fixed and swept portions
This ionogram was digitized from the original ALOUETTE 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at http://nssdc/space/isis/isis-status.html
created April 1998
Virtual variable.
This variable could be used as x-axis on amplitude spectrograms if fixed part is subtracted.
time of frequency markers
seperates the fixed and swept portions
This ionogram was digitized from the original ALOUETTE 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at http://nssdc/space/isis/isis-status.html
created April 1998
Virtual variable.
This variable could be used as x-axis on amplitude spectrograms if fixed part is subtracted.
time of frequency markers
seperates the fixed and swept portions
This ionogram was digitized from the original ALOUETTE 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at http://nssdc/space/isis/isis-status.html
created April 1998
Virtual variable.
This variable could be used as x-axis on amplitude spectrograms if fixed part is subtracted.
time of frequency markers
seperates the fixed and swept portions
This ionogram was digitized from the original ALOUETTE 2 analog telemetry data on 7-track tape using the facilities of the Data Evaluation Laboratory at GSFC (Code 500). This data restoration project is headed by Dr. R.F. Benson (GSFC, Code 692). Ionograms were digitized at the rate of 40,000 16-bit samples/sec. This sample rate is higher than the Nyquist frequency of 30 kHz. The sample frequency of 40 kHz provides a measurement every 25 microseconds corresponding to an apparent range (c*t/2) interval of 3.747 km. Each ionogram consists of a fixed-frequency and and a swept-frequency portion. The time resolution is typically 24 seconds. More information can be found at http://nssdc/space/isis/isis-status.html
created April 1998
Virtual variable.
This variable could be used as x-axis on amplitude spectrograms if fixed part is subtracted.
time of frequency markers
seperates the fixed and swept portions
This is the hourly-averaged data from the Apollo 12 Solar Wind Spectrometer instrument, reformatted by NSSDC for easier access and use. During the lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation. Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at ftp://nssdcftp.gsfc.nasa.gov/miscellaneous/documents
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Points into proton flow; no correction for orbital velocity.Set 1: least restrictive quality selection.
Points into proton flow; no correction for orbital velocity. Set 2: RMS error on curve fitting < 20
Points into proton flow; no correction for orbital velocity. Set 3: fit RMS <20 & 1 angle measured.
Points into proton flow; no correction for orbital velocity.Set 4: fit RMS <20 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
This 28-s data set is the highest resolution data set available from the Apollo 12 Solar Wind Spectrometer instrument, and was reformatted by NSSDC for easier access and use. During the lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation. Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at ftp://nssdcftp.gsfc.nasa.gov/miscellaneous/documents
These FLAG Bits of no interest to user; kept as record of original.
If IA = 0, alpha is measured; = 1, alpha is assumed; = 2, alpha is limited; = 3, cup seeing protons is too far from sun direction to be plausible.
If IB = 0, beta is measured; = 1, beta is assumed; = 2, beta is limited; = 3, cup seeing protons is too far from sun direction to be plausible.
This is the hourly-averaged data from the Apollo 15 Solar Wind Spectrometer instrument, reformatted by NSSDC for easier access and use. During the lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation. Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at ftp://nssdcftp.gsfc.nasa.gov/miscellaneous/documents
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Points into proton flow; no correction for orbital velocity.Set 1: least restrictive quality selection.
Points into proton flow; no correction for orbital velocity. Set 2: RMS error on curve fitting < 20
Points into proton flow; no correction for orbital velocity. Set 3: fit RMS <20 & 1 angle measured.
Points into proton flow; no correction for orbital velocity.Set 4: fit RMS <20 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
Set 1: least restrictive quality selection.
Set 2: RMS error on curve fitting < 20
Set 3: fit RMS <20 & 1 angle measured.
Set 4: fit RMS <20 & 2 angles measured.
This 28-s data set is the highest resolution data set available from the Apollo 15 Solar Wind Spectrometer instrument, and was reformatted by NSSDC for easier access and use. During the local lunar night there is no solar wind signal so there are data gaps of about 15 days each lunation. Users should refer to the data set documentation paper entitled 'ALSEP solar wind spectrometer plasma data as observed at the Apollo 12 and 15 landing sites,' by Goldstein, Clay,Snyder, and Neugebauer, which is contained in the online Data Set Catalog at ftp://nssdcftp.gsfc.nasa.gov/miscellaneous/documents
These FLAG Bits of no interest to user; kept as record of original.
If IA = 0, alpha is measured; = 1, alpha is assumed; = 2, alpha is limited; = 3, cup seeing protons is too far from sun direction to be plausible.
If IB = 0, beta is measured; = 1, beta is assumed; = 2, beta is limited; = 3, cup seeing protons is too far from sun direction to be plausible.