This page summarizes information about the selected resource and its origin based on SPASE metadata.
SPASE version 1.3.0
H+, O+, He+ and He++ upflowing fluxes and statistical uncertainties processed by the TIMAS science team.These data were used in preparing several papers, see Information URLs.
Includes also non-TIMAS Data: UT, altitude, invariant latitude, L shell, magnetic local time, geomagnetic latitude (signed - n/s hemisphere), average magnetic field vector in GSM coordinates at Polar (uses KH's co-ord conversion code), spacecraft potential from EFI data base, solar zenith angles at each end of the field line, time delayed solar wind parameters from WIND (Using KH's database) interpolated across data gaps of less than 10 minutes, IMF in GSM, solar wind dynamic pressure (nPa), solar wind density (/cc), solar wind velocity (km/sec).
This is a summary data base.It does not contain detailed energy step and pitch angle information for each data point. Extends over all altitudes, invariant latitudes and MLT. Below altitude of 4.0 Re 2 spin resolution (12s), above altitude of 4.0 Re 4 spin resolution (24s).
Reference:E.G. Shelley et al., The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the Polar Mission, Sp. Sci. Rev, Vol 71, pp 497-530, 1995.
Role | Person | |
---|---|---|
1. | Principal investigator | Dr. W. K. Peterson |
Several compromises were made in assembling the data base. In particular background subtraction, short averaging intervals and the normally low count rates for minor ions (O+, He+, and He++) lead to many data intervals where the data values reported are not statistically significant. The data files therefore contain many diagnostic parameters and data quality flags.
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 AD of variable accumulation intervals for H+
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 AD of variable accumulation intervals for O+
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 AD of variable accumulation intervals for He+
NSSDC standard-reference time value at the center of the accumulation interval.
Center epoch (milliseconds since 0 AD of variable accumulation intervals for He++
H+ Fluence (upward directed flux) at the altitude measured (R) with loss cone correction.
For statistical studies normalize to a standard altitude! Negative flux values correspond to downflowing fluxes.
O+ Fluence (upward directed flux) at the altitude measured (R) with loss cone correction.
For statistical studies normalize to a standard altitude! Negative flux values correspond to downflowing fluxes.
He+ Fluence (upward directed flux) at the altitude measured (R) with loss cone correction.
For statistical studies normalize to a standard altitude! Negative flux values correspond to downflowing fluxes.
He++ Fluence (upward directed flux) at the altitude measured (R) with loss cone correction.
For statistical studies normalize to a standard altitude! Negative flux values correspond to downflowing fluxes.
One standard deviation (sigma) of H+ fluence at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of O+ fluence at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of O+ fluence at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of He++ fluence at the altitude measured (R)
For statistical studies normalize to a standard altitude!
Net H+ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
Net O+ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
Net He+ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
Net He++ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of H+ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of O+ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of He+ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
One standard deviation (sigma) of He++ energy flux at the altitude measured (R)
For statistical studies normalize to a standard altitude!
Number of spins accumulated for H+
Number of spins of data accumulated for H+ .
Number of spins accumulated for O+
Number of spins of data accumulated for O+ .
Number of spins accumulated for He+
Number of spins of data accumulated for He+ .
Number of spins accumulated for He++
Number of spins of data accumulated for He++ .
Solar Zenith angle at the magnetic foot point
Check the SZA_status flag
Solar Zenith angle at the Conjugate magnetic foot point
Check the Conjugate_SZA_status flag
Quality of the solar zenith angle (SZA) values: 0=good, 99=invalid
Quality of the conjugate solar zenith angle (SZA) values: 0=good, 99=invalid
A quality flag in the range 0-99 with the following values/meanings:
0 OK. 1 Some data missing. 2 more than 5% data missing 3 not used. 4 not used. 5 Warning flags set. 6 not used. 9 Invalid pitch angles 99 No valid data.
A quality flag in the range 0-99 with the following values/meanings:
0 OK. 1 Some data missing. 2 more than 5% data missing 3 not used. 4 not used. 5 Warning flags set. 6 not used. 9 Invalid pitch angles 99 No valid data.
A quality flag in the range 0-99 with the following values/meanings:
0 OK. 1 Some data missing. 2 more than 5% data missing 3 not used. 4 not used. 5 Warning flags set. 6 not used. 9 Invalid pitch angles 99 No valid data.
A quality flag in the range 0-99 with the following values/meanings:
0 OK. 1 Some data missing. 2 more than 5% data missing 3 not used. 4 not used. 5 Warning flags set. 6 not used. 9 Invalid pitch angles 99 No valid data.
Geocentric Distance
MacIlwain L Parameter
Magnetic Local Time
Local Time
Magnetic Latitude
Invariant Latitude
Average magnetic field vector in GSM coordinates at Polar (Uses KH's co-ord conversion code).
3 components are GSM -X, -Y, and -Z
Index | Name | Component | Valid min | Valid max | Fill value |
---|---|---|---|---|---|
1 | -Bx | X | -100000.0 | 100000.0 | -1.0E31 |
2 | -By | Y | -100000.0 | 100000.0 | -1.0E31 |
3 | -Bz | Z | -100000.0 | 100000.0 | -1.0E31 |
Space craft potential from EFI
This Variable has not been extensively validated ... use with caution.
Time delayed Wind IFM Magnetic Field from WIND spacecraft in GSM Coordinates
Index | Name | Component | Valid min | Valid max | Fill value |
---|---|---|---|---|---|
1 | IMF Bx | X | -100000.0 | 1000.0 | -1.0E31 |
2 | IMF By | Y | -100000.0 | 1000.0 | -1.0E31 |
3 | IMF Bz | Z | -100000.0 | 1000.0 | -1.0E31 |
Time lagged solar wind dynamic pressure from WIND observations
Time lagged solar wind density from WIND observations
Time lagged Solar wind velocity from WIND in GSM Coordinates
Index | Name | Component | Valid min | Valid max | Fill value |
---|---|---|---|---|---|
1 | Vx | X | -700.0 | 700.0 | -1.0E31 |
2 | Vy | Y | -700.0 | 700.0 | -1.0E31 |
3 | Vz | Z | -700.0 | 700.0 | -1.0E31 |
Average counts per spin in the fast event counter
The TIMAS detector has a non linear response at high count rates that is, to some extent corrected for in the software that generated the data here. The correction, however introduces some uncertainty. The FEC count rate is carried as an indication of the corrections applied to the raw data.
Average background counts per spin
TIMAS is operated in one of 3 energy ranges. Energy_Range ID indicates which of the 3 instrumental energy ranges is currently active. Energy Range Identification: 0: Full energy range; 1: Reduced energy range; 2: Low energy range
# of intervals in the po_H0_tim data file included in the average reported here. These values should be compared with X_spins where = H, O He1 and He2
Quality of the SC potential value obtained from EFI: 0=good 99=invalid
Quality of the IMF_status values: 0=good 99=invalid
Quality of the SW data: 0=good 99=invalid
Quality of the Polar magnetometer data: 0=good 99=invalid
Quality of the Polar ephemeris data: 0=good 99=invalid
SPASE version 1.3.0
This investigation onboard POLAR spacecraft utilizes a toroidal ion mass spectrograph (TIMS) to fulfill its objectives, which are to study (1) the properties, location, and morphology of the principal source region for the entry of solar wind plasma into the magnetosphere, i.e., the polar cusp; (2) the properties, location, and morphology of the principal source region for hot ionospheric plasma in the magnetosphere, i.e., the auroral acceleration region; (3) the details of the processes by which the source plasmas are injected into trapped orbits, with special emphasis on the mass dependence of these processes; (4) details of the processes by which relatively cool source plasmas are energized into hot plasma, with special emphasis on the mass dependence of these processes; and (5) the details of the processes by which the hot magnetospheric plasma are lost, for example through wave-particle scattering and charge exchange, with special emphasis on the mass dependence of these processes.
The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) instrument measures the full three-dimensional velocity distribution functions of all major magnetospheric ion species with one-half spin period time resolution. The TIMAS is a first order double focusing (angle and energy), imaging spectrograph that simultaneously measures all mass per charge components from 1 AMU/e to greater than 32 AMU/e over a nearly 360 degrees by 10 degree instantaneous field-of-view in 20 milliseconds. Mass per charge is dispersed radially on an anular microchannel plate detector and the azimuthal position on the detector is a map of the instantaneous 360 degrees field of view. With the rotation of the spacecraft, the TIMAS sweeps out a 4pi solid angle image in a half spin period. The energy per charge range from 15eV/e to 32 keV/e is covered in 28 non-contiguous steps spaced approximately logarithmically with adjacent steps separated by about 30%. In order to handle the large volume of data within the telemetry limitations the distributions are compressed to varying degrees in angle and energy, log-count compressed and then further compressed by a lossless technique. This data processing task is supported by two SA3300 microprocessors. The voltages (up to + 5 kV) for the tandem toroidal electrostatic analyzers are supplied from common high voltage supplies using optically controlled series-shunt regulators.
Role | Person | |
---|---|---|
1. | Principal investigator | Dr. W. K. Peterson |
SPASE version 1.3.0
POLAR is one of four spacecraft in the Global Geospace Science (GGS) program. These are among the six spacecraft in the International Solar Terrestrial Physics (ISTP) program. POLAR provides multi-wavelength imaging of the aurora, measuring plasma entry into the polar magnetosphere and geomagnetic tail, the flow of plasmas to and from the ionosphere, and the deposition of particle energy in the ionosphere and upper atmosphere. POLAR has on-board propulsion systems and a design lifetime of three to five years, with redundant subsystems. POLAR is cylindrical, approximately 2.8 m in diameter by 1.25 m high (plus 1.25 m for its two despun platforms), with body-mounted solar cells, weighs 1250 kg and uses 333 W of power. The spin rate is 10 rpm around an axis approximately normal to the orbital plane. It has long wire spin-plane antennas, inertial booms, and spin-plane appendages to support sensors. POLAR has two despun gimbaled instrument platforms, and booms are deployed along both Z axes. Data are stored using on-board tape recorders and are relayed to the Deep Space Network at 600 kbps maximum (250 kbps nominal) although the average real-time data rate for POLAR is 41.6 kbps. POLAR has a 22.6-h polar orbit (90 deg inclination), with perigee and apogee of 11,500 and 57,000 km. Polar was launched to observe the polar magnetosphere and, as its orbit has precessed with time, has observed the equatorial inner magnetosphere and is now carrying out an extended period of southern hemisphere coverage. Details on the POLAR mission and instrumentation are provided in Space Science Reviews (Vol. 71, Nos. 1-4, 1995) and reprinted in The Global Geospace Mission, edited by C. T. Russell (Kluwer, 1995).
Role | Person | |
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1. | Project scientist | Dr. John B. Sigwarth |
SPASE version 1.3.0
SPASE version 1.3.0
SPASE version 1.3.0
The TIMAS Science Team's data base of TIMAS H2 data
Role | Person | |
---|---|---|
1. | Principal investigator | Dr. W. K. Peterson |