Data Description

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

Table of Contents

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  2. Repository
  3. Instrument
  4. ObservatoryObservatories
  5. Persons

SPASE version 2.2.2

Numerical Data Product: STEREO-B IMPACT/SEPT 1-min Level 1 Electron and Proton Spectra

Resource ID
spase://VEPO/NumericalData/STEREO-B/IMPACT/SEPT/L1/PT1M Get XML
Name
STEREO-B IMPACT/SEPT 1-min Level 1 Electron and Proton Spectra
Description

The IMPACT Solar Electron Proton Telescope (SEPT) Level 1 data consist of electron and proton fluxes from each of 32 energy bands that span ~20 keV to 2000(electrons) or 7000(protons) keV. These spectra are determined each minute, in each of 4 directions with 60 deg fields of view (parallel and anti-parallel to the Parker magnetic field direction, and northward and southward from the ecliptic plane.

Additional information
SEPT site at U. Kiel
CDAWeb Skeleton Table
Acknowledgement

Please acknowledge the IMPACT P.I., Janet Luhmann of UCB

Contact
Role Person
1. Principal investigator Dr. Janet G. Luhmann 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
3275 kB per 1 day
Acknowledgement

Please acknowledge the P.I., Janet Luhmann of UCB, and CDAWeb at GSFC/SPDF

Instrument
STEREO-B IMPACT SEPT Get XML
Measurement type
Energetic particles
Temporal description
Start date
2006-11-13 00:00:00
Relative stop date
5 months ago
Cadence
1 minute
Observed regions
Heliosphere.Remote1AU

Parameters

Parameter #1

Name
Electron spectrum viewing northward from ecliptic plane
Parameter key
Spec_0_NS
Description

Electron flux in each of 32 energy bands between 20 keV and 4000 keV, from the SEPT sensor pointed northward from the ecliptic plane

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 electron fluxes

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

Parameter #2

Name
Electron spectrum viewing southward from ecliptic plane
Parameter key
Spec_2_NS
Description

Electron flux in each of 32 energy bands between 20 keV and 4000 keV, from the SEPT sensor pointed southward from the ecliptic plane

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 electron fluxes

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

Parameter #3

Name
Proton spectrum viewing northward from ecliptic plane
Parameter key
Spec_3_NS
Description

Proton flux in each of 32 energy bands between 20 keV and 7000 keV, from the SEPT sensor pointed northward from the ecliptic plane

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 proton fluxes

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

Parameter #4

Name
Proton spectrum viewing southward from ecliptic plane
Parameter key
Spec_1_NS
Description

Proton flux in each of 32 energy bands between 20 keV and 7000 keV, from the SEPT sensor pointed southward from the ecliptic plane

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 proton fluxes

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

Parameter #5

Name
Electron spectrum viewing sunward along the Parker IMF angle
Parameter key
Spec_2_E
Description

Electron flux in each of 32 energy bands between 20 keV and 4000 keV, from the SEPT sensor pointed sunward along the Parker IMF spiral angle

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 electron fluxes

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

Parameter #6

Name
Electron spectrum viewing antisunward along the Parker IMF angle
Parameter key
Spec_0_E
Description

Electron flux in each of 32 energy bands between 20 keV and 4000 keV, from the SEPT sensor pointed antisunward along the Parker IMF spiral angle

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 electron fluxes

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

Parameter #7

Name
Proton spectrum viewing sunward along the Parker IMF angle
Parameter key
Spec_1_E
Description

Proton flux in each of 32 energy bands between 20 keV and 7000 keV, from the SEPT sensor pointed sunward along the Parker IMF spiral angle

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 proton fluxes

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

Parameter #8

Name
Proton spectrum viewing antisunward along the Parker IMF angle
Parameter key
Spec_3_E
Description

Proton flux in each of 32 energy bands between 20 keV and 7000 keV, from the SEPT sensor pointed antisunward along the Parker IMF spiral angle

Cadence
1 minute
Units
1/(sec sr cm^2 MeV)
Structure
Size
32
Description

Set of 32 proton fluxes

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

SPASE version 2.0.3

Instrument: STEREO-B IMPACT SEPT

Instrument ID
spase://SMWG/Instrument/STEREO-B/IMPACT/SEPT Get XML
Name
STEREO-B IMPACT SEPT
Alternate name
STEREO-B IMPACT Solar Electron Proton Telescope
Description

The Solar Electron Proton Telescope (SEPT) consists of two dual, double-ended magnet/foil solid state detector particle telescopes that separate and measure electrons in the energy range of 20-400 keV and protons from 20-7000 keV, while providing anisotropy information through use of several fields of view. Each Silicon Strip Detector (SSD) in SEPT is 300 microns thick and 0.53 cm2 in area. A rare-earth permanent magnet is used to sweep away electrons for ion detection, while a parylene foil transmits electrons but stops protons.

SEPT is divided into two pieces for field-of-view reasons. The SEPT-E telescope is housed with the rest of the SEP Package on the body of the spacecraft. It looks in the ecliptic plane along the Parker Spiral magnetic field direction, both forward and backward. SEPT-N/S is housed separately at a different spacecraft location, and looks out of the ecliptic plane perpendicular to the nominal magnetic field, both north and south. The viewing cones for the SEPT telescopes are each ~60 degrees.

The electronics  were provided by ESA-ESTEC, SCI-A. The housing and the sensors were provided by the University of Kiel (Germany).

Additional information
STEREO/IMPACT Mission Site
NSSDC's Master Catalog

Information about the In-Situ Measurements of Particles and CME Transients (IMPACT) experiment on the STEREO B mission.

Acknowledgement

The STEREO IMPACT/SEPT team

Contact
Role Person
1. Principal investigator Dr. Janet G. Luhmann Get XML
2. CoInvestigator Dr. Horst W. Kunow Get XML
3. CoInvestigator Reinhold Müller-Mellin Get XML
4. CoInvestigator Stephan Boettcher Get XML
5. CoInvestigator Dr. Bernd Heber Get XML
6. CoInvestigator Dr. Trevor R. Sanderson Get XML
7. CoInvestigator Dr. Richard G. Marsden Get XML
Release date
2010-03-18 14:37:51
Instrument type
Particle Detector
Investigation name
In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Electron Proton Telescope on STEREO B
Observatory
STEREO B Get XML

SPASE version 2.2.0

Observatory: STEREO B

Observatory ID
spase://SMWG/Observatory/STEREO-B Get XML
Name
STEREO B
Alternate name
STEREO Behind
STEREO West
Solar Terrestrial Relations Observatory B
Description

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs). These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations.

Additional information
STEREO Project Page

Project home page

NSSDC's Master Catalog

Information about the STEREO B mission

Contact
Role Person
1. Project scientist Mr. Michael L. Kaiser Get XML
Release date
2010-09-25 03:09:48
Prior ID
spase://vspo/observatory/140
Observatory group
STEREO Mission Get XML
Location
Region
Heliosphere.Remote1AU

SPASE version 2.2.0

Observatory: STEREO Mission

Observatory ID
spase://SMWG/Observatory/STEREO Get XML
Name
STEREO Mission
Description

The Solar-Terrestrial Relations Observatory (STEREO) mission includes two spacecraft respectively lagging (STEREO A) and leading (STEREO B) the Earth in heliocentric orbit around the Sun for remote 3-D imaging and radio observations of coronal mass ejections (CMEs). These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations.

Additional information
STEREO Project Page

Project home page

Contact
Role Person
1. Project scientist Mr. Michael L. Kaiser Get XML
Release date
2009-05-20 20:00:12
Location
Region
Heliosphere.Remote1AU

SPASE version 2.2.0

Person: Dr. Janet G. Luhmann

Name
Dr. Janet G. Luhmann
Organization
University of California, Berkeley
Person ID
spase://SMWG/Person/Janet.G.Luhmann 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. 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: Reinhold Müller-Mellin

Name
Reinhold Müller-Mellin
Organization
University of Kiel
Email
mueller-mellin@kernphysik.uni-kiel.de
Person ID
spase://SMWG/Person/Reinhold.Mueller-Mellin Get XML
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

Person: Stephan Boettcher

Name
Stephan Boettcher
Organization
University of Kiel
Email
boettcher@physik.uni-kiel
Person ID
spase://SMWG/Person/Stephan.Boettcher Get XML
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

Person: Dr. Bernd Heber

Name
Dr. Bernd Heber
Organization
Universitat Osnabruck
Person ID
spase://SMWG/Person/Bernd.Heber Get XML

SPASE version 2.2.0

Person: Dr. Trevor R. Sanderson

Name
Dr. Trevor R. Sanderson
Organization
ESA-European Space Research Technology
Person ID
spase://SMWG/Person/Trevor.R.Sanderson Get XML

SPASE version 2.2.0

Person: Dr. Richard G. Marsden

Name
Dr. Richard G. Marsden
Organization
ESA-European Space Research Technology
Email
richard.marsden@esa.int
Phone
+1-31-1715653583
Person ID
spase://SMWG/Person/Richard.G.Marsden Get XML
Release date
2010-08-05 17:35:47

SPASE version 2.2.0

Person: Mr. Michael L. Kaiser

Name
Mr. Michael L. Kaiser
Organization
GSFC-Code 695
Person ID
spase://SMWG/Person/Michael.L.Kaiser Get XML

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