Data on charged particles in space as measured by instruments
of TASPD SINP MSU are presented under this root directory.
TASPD SINP MSU stands for Theoretical and Applied Space Physics Division,
Skobeltsyn Institute of Nuclear Physics, Moscow State University.
The data sets co-reside on server TASPD.NPI.MSU.SU at MSU, Moscow, Russia
and on server at NSSDC/GSFC, NASA, USA.
The data of this collection have been restored from papers and old tapes.
This work has been supported, in its significant part, by NASA, grant NAG5-4656.
Data sets are given as ASCII tables and placed to the spacecraft-specific
subdirectories. Each subdirectory contains a data file, a descriptor on
data/instrument/mission and a GIF-file with overview-plots. Long data sets
(from the spacecraft GRANAT and COSMOS-900) use one-year and one-day file
formats respectively.
Each data file is organized as a table with blank-space separators. Two
heading lines provide information identifying the spacecraft/instrument
and the data columns. A line "The end." terminates each data file.
The column-legends from the 2nd header line are used in a file-descriptor
id_descr.txt for addressing the explanations to a particular column.
Each data line presents a record of measured parameters with leading time-tag.
Everywhere time is universal time (UT) and everywhere a time value corresponds
to the end of interval of measurement given in the record. Time format is
YYMMDDHHmmSS (YY - year, MM - month, ...). If time resolution is worse
than seconds, the respectively truncated form may be used instead.
Every data column is given in the exponential format E10.3.
Everywhere NODATA-filler is -9.999E+99.
Almost all measured data are given in count rates (1/s). Ultra-violet
sensor on COSMOS-900 is the only exception. Geometric factors are presented
for every data channel in the correspondent id_descr.txt files. They may
be used for converting the count rate to intensity.
Spacecraft trajectory information is also given if available. Coordinates of
a spacecraft are appended to each data record. For far missions, trajectory
is given in the Heliographic Inertial Coordinate System (HGI). For the Earth's
satellites GRANAT and COSMOS-900, trajectory is presented in a geocentric
coordinate system. File sc_coordinates.txt describes the used coordinates.
A definition of HGI system is given in the file rah_to_hgi.txt.
Trajectory information is not available for the following spacecraft:
- four lunar spacecraft (Moon's coordinates may be used instead);
- ZOND-1 (no source; Earth's coordinates may be used instead);
- MARS-2 for the part when it is in the Mars orbit (Mars' coordinates may used);
- VEGA-2 (no source; a very similar trajectory of VEGA-1 may be used);
- PHOBOS-2 (no source).
Trajectories for old missions were restored from old in-paper plots of
low quality, hence accuracy is as low as 5-10% or so. Therefore, these data
may be used only as a reference, not for precise analysis of the data from
spacecraft situated nearby each other. The trajectory data have been
converted to HGI system from another system, see notes on the method of
this conversion in the file rah_to_hgi.txt. Where available, a file of
spacecraft coordinates in both original and HGI form is provided in addition.
Below is a reference table on all data sets included in the collection.
In 'Columns', the contents of each data set is presented as an information
derived from the dataset's column legends. Notations are as follows.
A leading letters: 'p' - proton, 'e' - electron, 'a' - alpha-particle,
'n' - nucleon, 'uv' - ultra-violet. Following digits denote energy
range/threshold in MeV (except 'uv' channel on COSMOS-900). Trailing letter
denotes direction of where particles come from: '+' - from sunward Sun,
'-' - from antiSun, '*' - omni (from all directions), 'n' - perpendicular
to sunward direction, 'm','c' - 45 degrees to sunward direction,
'z' - perpendicular to lunar surface, 'a' - field-aligned,
'p' - field-perpendicular, 'e' - from center-of-Earth direction. Legends
present only main fraction of the measured fluxes for a particular channel
if the measurement is not pure; see notes on this issue in the file sensors.txt.
More details are given in the spacecraft specific files id_descr.txt placed in
the spacecraft relevant subdirectories.
Spacecraft Instrument Id TimeRes DataStart DataEnd Columns:
---------- ---------- -- ------- --------- ------- --------
ZOND-1 KS-OLD Z1 1d 64/04/02-64/05/16 UT p>30+
ZOND-3 KS-18 Z3 4h 65/07/19-66/01/21 UT p>30+ p1-5n
LUNA-17/lk1 RV-2N LG 1d 70/11/10-71/09/14 UT p>30z p1-5z a4-8z
LUNA-19 RV-2N-LS LI >1d 71/09/29-72/08/23 UT p>30+ p1-5+ p5-12+ p12-40+
LUNA-21/lk2 RV-2N LK 1d 73/02/14-73/04/20 UT p>30z p1-5z a4-8z
LUNA-22 RV-2N-1 LL 4h 74/05/29-75/08/23 UT p1-5+ p5-15+ a5-10+
LUNA-22 RV-2N-1 LS 1d 74/05/29-75/08/26 UT p>30+
MARS-2/crs KS-18-4M M2 4h 71/05/21-71/11/26 UT p>30+ p1-5v+ p1-5+ p5-12+ p1-5v- p1-5- p5-12- p>500*
MARS-2/orb KS-18-4M/ga MA 4h 71/11/26-72/06/01 UT p>30+ p1-5+ p5-12+ p1-5- p5-12- e>.3-
MARS-2/orb KS-18-4M/gb MB 4h 71/11/26-72/06/01 UT p1-5v+ p1-5v- p>500* e>.3+ e>.05-
MARS-4 KS-18-5M M4 4h 73/07/23-73/10/30 UT p>30+ p1-5+ p4-12+ p4-12- p>500*
MARS-5 KS-18-5M M5 4h 73/07/26-74/02/08 UT p>30+ p1-5+ p1-5- p4-12+
MARS-7 KS-18-5M M7 4h 73/08/17-74/03/25 UT p>30+ p1-5+ p1-5- p4-12+ p>500*
VENERA-2 KS-18M V2 4h 65/11/15-66/01/25 UT p>30+ p1-5n
VENERA-3 KS-18M V3 4h 65/11/16-65/12/10 UT p>30+ p1-5n e>.05n
VENERA-4 KS-2M V4 4h 67/06/12-67/10/16 UT p>30+ p1-5+ p1-5- e>.05-
VENERA-5 KS-3M V5 4h 69/01/05-69/03/09 UT p>30+ p1-4+ p1-4- p1-4n e>.05n
VENERA-6 KS-3M V6 4h 69/01/10-69/05/15 UT p>30+ p1-4+ p1-4- p1-4n e>.05n
VENERA-7 KS-4M V7 4h 70/08/17-70/12/15 UT p>30+ p1-5+ p1-5- p4-12+ p4-12-
VENERA-8 KS-18-4M V8 4h 72/03/27-72/07/22 UT p>30+ p1-5- p5-10+ p>0.3- e>.05+ e>.05-
VENERA-9 KS-18-5M V9 4h 75/06/09-76/01/11 UT p>30+ p>800* p4-12-
VENERA-10 KS-18-5M VA 4h 75/08/19-76/04/01 UT p>30+ p>500* p4-12-
VENERA-11 ASP-8 VB 20m 78/09/11-79/10/04 UT p>30+ p3-5+ p3-5-
VENERA-13 ASP-8M VD 20m 81/10/31-83/04/12 UT p>30+ p1-3+ p1-3-
VENERA-14 ASP-8M VE 20m 81/11/06-83/03/16 UT p>30+ p1-3+ p1-3-
VENERA-13 ASP-8M WD 80m 81/10/31-83/04/12 UT p2-3+ p3-5+ p5-8+ p2-3- p3-5- p5-8-
VENERA-14 ASP-8M WE 80m 81/11/06-83/03/16 UT p1-2+ p2-4+ p4-8+ p1-2- p2-4- p4-8-
VENERA-16 KS-18-6V VG 4h 83/06/08-85/05/28 UT p>30+ p>60+ p1-65+ p1-11+ p5-8+ a7-24+ p1-70- p1-9- p5-10- a7-22-
VEGA-1 VFS-VK A1 20m 84/12/22-86/07/08 UT p>30m p>30c
VEGA-2 VFS-VK A2 20m 84/12/28-85/05/03 UT p>30m p>30c
PHOBOS-2 VFS-F F2 1h 88/07/13-89/03/23 UT p>30n
GRANAT KS-18-M/gr1 G1 20m 89/12/02-95/12/16 UT p>20+ p>6+ p1-20+ p>20- p>6- p1-20-
GRANAT KS-18-M/gr2 G2 2m 89/12/01-95/12/16 UT p2-7+ p5-20+ p2-7- p5-20-
GRANAT KS-18-M/gr3 G3 20m 89/12/02-94/07/11 UT a12-18+ a12-18-
GRANAT KS-18-M/gr4 G4 2m 89/12/01-95/12/16 UT p1-2+ p1-2-
GRANAT KS-18-M/gr5 G5 20m 89/12/02-95/11/30 UT p1-2+ p2-3+ p5-6+ p6-30+ p30-100+ a7-12+ n>20+ p1-2- p2-3- p5-6- p6-30- p30-100- a7-12- n>20-
GRANAT KS-18-M/gr6 G6 20m 89/12/02-95/12/16 UT p>20+ p>2.4+ p1-6+ a7-28+ a20-90+ p>20- p>2.4- p1-6- a6-40- a20-90-
COSMOS-900 DPS-MES-NS-UF C9 5s 77/04/01-79/09/10 UT p.050-.080p p.080-.128p p.128-.206p p.206-.314p p.211-.326a p1-3p e.030-.050a e.030-.050p e.050-.080p e.080-.130p e.130-.210p uv3900e
All listed spacecraft except GRANAT and COSMOS-900 are non-geocentric.
The two latter are satellites: GRANAT has a high-altitude orbit with its
initial apogee ~200000 km and COSMOS-900 has a circular orbit with h=~500 km
and i=83 degrees. Since GRANAT spent most of time out of geomagnetosphere,
its data sets are split to the subdirectories /heliospheric_data and
/magnitospheric_data.
Time resolution listed above may be understood differently for different
spacecraft. For old non-geocentric spacecraft it may vary from one record
to another; the almost smallest value is given in the table. For newer
spacecraft, given time resolution is the best that the instruments have
provided. The given values are almost constant ones but they may not be
exactly equal to 4 hours or 20 minutes, - some small shifting of time grid
may be observed. On GRANAT, 2 minute mode has been used only for several
channels and mostly in the periods of high intensity of measured fluxes.
Please feel free to direct any questions or comments on the data collection
to Nick Pavlov: nnpavlov@taspd.npi.msu.su