Data Description

This page summarizes information about the selected resource and its origin based on SPASE metadata.

Table of Contents

  1. Product
  2. Repository
  3. Instrument
  4. Observatory
  5. Persons

SPASE version 2.2.2

Numerical Data Product: SOHO COSTEP Key Parameter Data

Resource ID
spase://VEPO/NumericalData/SOHO/COSTEP/KP/PT5M Get XML
Name
SOHO COSTEP Key Parameter Data
Description

Data include 5-min differential fluxes of protons at seven energies between 0.54 and 47 MeV, of electrons at four energies between 0.5 and 7.4 MeV and of alpha particles at four energies between 6.1 and 47 MeV/n. They are key parameter data accessible from CDAWeb.

Additional information
CDAWeb Skeleton Table
Acknowledgement

Please acknowledge the P.I., Horst W. Kunow of Universitat Kiel

Contact
Role Person
1. Principal investigator Dr. Horst W. Kunow Get XML
Release date
2010-08-12 00:00:00
Repository
Name
SPDF Get XML
Availability
Online
Access rights
Open
URL
CDAWeb

With subset, plot and ASCII list functions from CDAWeb

FTP access to files at SPDF
HTTP access to files at SPDF

In CDF via HTTP from SPDF

Format
CDF
File size
76 kB per 1 day
Acknowledgement

Please acknowledge the P.I., Horst W. Kunow of Universitat Kiel, and CDAWeb at GSFC/SPDF

Instrument
Comprehensive Suprathermal and Energetic Particle Instrument (COSTEP) Get XML
Measurement type
Energetic particles
Temporal description
Start date
1995-12-07 00:00:00
Stop date
2002-01-31 00:00:00
Cadence
5 minutes
Observed regions
Heliosphere.NearEarth

Parameters

Parameter #1

Name
Electron fluxes
Parameter key
Electron
Description

Electron differential fluxes at 4 energies at 5 minute resolution

Cadence
5 minutes
Units
1/(cm**2 s sr MeV)
Structure
Size
4
Description

Set of four electron fluxes

Fill value
-1.0e+31
Particle type
Electron
Quantity
Number flux

Parameter #2

Name
Proton fluxes
Parameter key
Proton
Description

Proton differential fluxes at 7 energies at 5 minute resolution

Cadence
5 minutes
Units
1/(cm**2 s sr MeV)
Structure
Size
7
Description

Set of seven proton fluxes

Fill value
-1.0e+31
Particle type
Proton
Quantity
Number flux

Parameter #3

Name
Helium fluxes
Parameter key
Helium
Description

Helium differential fluxes at 4 energies at 5 minute resolution

Cadence
5 minutes
Units
1/(cm**2 s sr MeV/n)
Structure
Size
4
Description

Set of four helium nuclei fluxes

Fill value
-1.0e+31
Particle type
AlphaParticle
Quantity
Number flux

SPASE version 2.0.0

Instrument: Comprehensive Suprathermal and Energetic Particle Instrument (COSTEP)

Instrument ID
spase://SMWG/Instrument/SOHO/COSTEP Get XML
Name
Comprehensive Suprathermal and Energetic Particle Instrument (COSTEP)
Alternate name
COSTEP
Description

The COSTEP (COmprehensive SupraThermal and Energetic Particle) instrument with sensors LION and EPHIN is a subset of the CEPAC experiment measuring the solar particle emission over a wide range of species (electrons through iron) and energies (40 KeV/particle to 500 MeV/nucleon). LION (Low-energy Ion and electron instrument) has two sensor heads, each containing a double telescope and measuring spectra of ions and electrons in the range 40 KeV to 5 MeV for protons, 1.5--6 MeV/nucleon for Helium nuclei, and 40--300 KeV for electrons. The LION detector system consists of three ion implanted silicon detectors. One sensor head employs a broom magnet to sweep electrons of energies <300 KeV away from the detectors. The total field of view is 60 x 40 degrees. A total of 32 energy channels are accumulated with 15 s resolution. From these it is possible to derive good spectra during large solar events with about one minute resolution. The EPHIN sensor is a multi-element array of solid state detectors with anticoincidence to measure energy spectra of electrons in the range 150 KeV to >5MeV and hydrogen and helium isotopes in the range 4 MeV/nucleon to >53 MeV/nucleon with a maximum geometric factor of 5.1 cm**3 sr (self-adapting to particle fluxes). The field of view is a cone of 90 degrees full angle. The separation of particle species is provided by a set of five thresholds in the first detector. A small sample of particles is analyzed in pulse height. Four 128-bin histograms containing coarse spectral information are generated on-board separately for four detector ranges and transmitted each minute together with rates and pulse height words. The COSTEP data will be routinely searched for irregular 3He contributions in the EPHIN pulse height words, especially during special campaigns or if other information is available predicting higher contributions. If 3He is observed, the correlation with electron observations of various energies will be investigated to compare acceleration, release, and travel times as well as spectral features. This information is from the paper ``COSTEP - Comprehensive Suprathermal and Energetic Particle Analyser for SOHO - Scientific Goals and Data Description,'' by H. Kunow et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 43-46, November 1992).

Additional information
NSSDC's Master Catalog

Information about the Comprehensive Suprathermal and Energetic Particle Instrument (COSTEP) experiment on the SOHO mission.

Contact
Role Person
1. Principal investigator Dr. Horst W. Kunow Get XML
Release date
2009-05-20 21:10:10
Instrument type
Energetic Particle Instrument
Investigation name
Comprehensive Suprathermal and Energetic Particle Instrument (COSTEP) on SOHO
Observatory
SOHO Get XML

SPASE version 2.2.0

Observatory: SOHO

Observatory ID
spase://SMWG/Observatory/SOHO Get XML
Name
SOHO
Alternate name
1995-065A
Solar and Heliospheric Observatory
Description

The primary scientific aims of the Solar and Heliospheric Observatory mission (SOHO) were to investigate: (1) the physical processes that form and heat the Sun's corona, maintain it and give rise to the expanding solar wind; and, (2) the interior structure of the Sun. Imaging and collection of spectroscopic plasma diagnostics of the solar chromosphere, transition region and corona, as well as in situ solar-wind measurements are used to study the corona and solar wind. Solar interior structure is investigated by helioseismological means and by the observation of variations in solar irradiance. SOHO was part of the International Solar-Terrestrial Physics Program (ISTP).

The SOHO spacecraft was three-axis stabilized and pointed towards the Sun with an accuracy of +/- 10 arcsec per 15 min. It consisted of a Payload Module to accommodate the instruments and a Service Module carrying the spacecraft subsystems and solar arrays. SOHO occupied a halo orbit at the Earth-Sun L1 Lagrangian point to obtain uninterrupted sunlight. The design life was two years, but on-board consumables were sufficient for an extra four years of operations.

Twelve instruments comprised the payload, producing a continuous stream of data at 40 kbs, except whenever the solar oscillations imager Michelson Doppler Imager (MDI) was operated in high-bit-rate mode, producing 160 kbs. The high-bit-rate mode was used during scheduled daily eight-hour periods or during dedicated campaigns. Magnetic tape stored data between telemetry contacts with the Experiment Operations Facility, located at NASA-GSFC. For more information, see B. Fleck, V. Domingo, and A. I. Poland, eds., Solar Physics, V. 162, 1995.

SOHO was a joint mission of the European Space Agency and NASA. It was launched aboard an Atlas IIAS rocket from Cape Canaveral Air Station, FL, on Dec. 2, 1995, and mission operations were directed from NASA's Goddard Space Flight Center, Greenbelt, MD.

In April 1998, SOHO successfully completed its nominal two-year mission to study the Sun's atmosphere, surface and interior. Major science highlights include the detection of rivers of plasma beneath the surface of the Sun; the discovery of a magnetic "carpet" on the solar surface that seems to account for a substantial part of the energy that is needed to cause the very high temperature of the corona, the Sun's outermost layer; the first detection of flare-induced solar quakes; the discovery of more than 50 sungrazing comets; the most detailed view to date of the solar atmosphere; and spectacular images and movies of coronal mass ejections, which were being used to improve the ability to forecast space weather.

Contact with SOHO was lost at 23:16 GMT on June 24, 1998 during maintenance operations. The spacecraft went into emergency sun reacquisition mode, which is activated when an anomaly occurs and the spacecraft loses its orientation toward the Sun. When this happened, the spacecraft automatically tried to point itself toward the Sun again by firing its attitude control thrusters under the guidance of an onboard Sun sensor. Efforts to re-establish contact with SOHO did not succeed and telemetry was lost, not to be reestablished for several weeks.

Attitude analysis led to the conclusion that SOHO went into a spin such that the solar panels were nearly edge-on towards the Sun, and thus did not generate any power. Because the spin axis is fixed in space, as the spacecraft progressed in its orbit the orientation of the panels with respect to the Sun gradually changed, resulting in increased solar illumination of the solar arrays as time progressed. On August 3, contact was re-established with SOHO following six weeks of silence. After a lengthy recovery process, on September 16 the spacecraft again locked onto the Sun, and experiment heaters were switched on. After recommissioning of various subsystems, and an orbit correction maneuver, SOHO was finally brought back to normal mode on 25 September at 19:52:58 GMT. Instrument switch-on started October 5, 1998, and by November 4 all instruments were back to normal.

Additional information
NSSDC's Master Catalog

Information about the SOHO mission

Contact
Role Person
1. Project scientist Dr. Arthur I. Poland Get XML
Release date
2010-08-05 18:19:18
Location
Region
Heliosphere.NearEarth

SPASE version 2.2.0

Person: Dr. Horst W. Kunow

Name
Dr. Horst W. Kunow
Organization
Universitat Kiel
Person ID
spase://SMWG/Person/Horst.W.Kunow Get XML

SPASE version 2.2.0

Person: Ms. Tamara J. Kovalick

Name
Ms. Tamara J. Kovalick
Organization
GSFC-Code 672
Email
Tamara.J.Kovalick@nasa.gov
Phone
+1-301-286-9422
Person ID
spase://SMWG/Person/Tamara.J.Kovalick Get XML
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

Person: Mr. Robert M. Candey

Name
Mr. Robert M. Candey
Organization
NASA Goddard Space Flight Center
Address
Code 672, Greenbelt, MD 20771, USA
Email
robert.m.candey@nasa.gov
Phone
1-301-286-6707
Person ID
spase://SMWG/Person/Robert.M.Candey Get XML
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

Person: Dr. Robert E. McGuire

Name
Dr. Robert E. McGuire
Organization
NASA Goddard Space Flight Center
Address
Code 672, Greenbelt, MD 20771, USA
Email
mcguire@mail630.gsfc.nasa.gov
Phone
+1 301 286 7794
Person ID
spase://SMWG/Person/Robert.E.McGuire Get XML
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

Person: Dr. Arthur I. Poland

Name
Dr. Arthur I. Poland
Organization
GSFC-Code 682
Email
poland@pal.gsfc.nasa.gov
Phone
+1-301-286-7076
Person ID
spase://SMWG/Person/Arthur.I.Poland Get XML
Release date
2010-08-05 17:35:45

SPASE version 1.3.0

Repository: SPDF

Repository ID
spase://SMWG/Repository/NASA/GSFC/SPDF Get XML
Name
SPDF
Description

Space Physics Data Facility

Additional information
SPDF

Space Physics Data Facility

Contact
Role Person
1. General contact Ms. Tamara J. Kovalick Get XML
2. Technical contact Mr. Robert M. Candey Get XML
3. Project scientist Dr. Robert E. McGuire Get XML
Release date
2008-08-26 21:02:30
Prior IDs
spase://vspo/repository/61
spase://SMWG/Repository/SPDF
Access URL