HDPWS

Data Access

EMN observation network 3sec resolution geomagnetic field data at Sao Luis, Brazil

ResourceID
spase://IUGONET/NumericalData/ICSWSE/EMN/SLZ/fluxgate/PT3S_ICSWSE_storage

Description
Geomagnetic field data observed at EMN Sao Luis station, Brazil. The time resolution is 3 second. The data consist of 3 components (H, D, Z).

View XML | Edit

Details

Version:2.5.0

NumericalData

ResourceID
spase://IUGONET/NumericalData/ICSWSE/EMN/SLZ/fluxgate/PT3S_ICSWSE_storage
ResourceHeader
ResourceName
EMN observation network 3sec resolution geomagnetic field data at Sao Luis, Brazil
ReleaseDate
2014-01-03 00:00:00
ExpirationDate
2199-12-31 00:00:00
Description
Geomagnetic field data observed at EMN Sao Luis station, Brazil. The time resolution is 3 second. The data consist of 3 components (H, D, Z).
Contacts
Role Person StartDate StopDate Note
1. PrincipalInvestigator spase://IUGONET/Person/Akimasa.Yoshikawa
2. MetadataContact spase://IUGONET/Person/Shuji.Abe

AccessInformation
RepositoryID
Availability
Online
AccessRights
Restricted
AccessURL
Format
Binary
Acknowledgement
Scientists who want to engage in collaboration with ICSWSE should contact the project leader of MAGDAS/CPMN observations, Dr. A. Yoshikawa, Kyushu Univ., who will organize such collaborations. There is a possibility that the PI of MAGDAS will arrange offers so that there is less overlapping of themes between MAGDAS research groups. Before you use MAGDAS/CPMN data for your papers, you must agree to the following points; 1. Before you submit your paper, you must contact the PI and discuss authorship. 2. When you submit your paper after doing the above item 1, you must mention the source of the data in the acknowledgment section of your paper. 3. In general, you must use the following references: (i). Yumoto, K., and the 210MM Magnetic Observation Group, The STEP 210 magnetic meridian network project, J. Geomag. Geoelectr., 48, 1297-1310., 1996. (ii). Yumoto, K. and the CPMN Group, Characteristics of Pi 2 magnetic pulsations observed at the CPMN stations: A review of the STEP results, Earth Planets Space, 53, 981-992, 2001. (iii). Yumoto K. and the MAGDAS Group, MAGDAS project and its application for space weather, Solar Influence on the Heliosphere and Earth's Environment: Recent Progress and Prospects, Edited by N. Gopalswamy and A. Bhattacharyya, ISBN-81-87099-40-2, pp. 309-405, 2006. (iv). Yumoto K. and the MAGDAS Group, Space weather activities at SERC for IHY: MAGDAS, Bull. Astr. Soc. India, 35, pp. 511-522, 2007. 4. In all circumstances, if anything is published you must send a hardcopy to the following address: Dr. Akimasa Yoshikawa, PI of MAGDAS/CPMN Project, International Center for Space Weather Science and Education, Kyushu University 53, 6-10-1 Hakozaki, Higashi-ku Fukuoka 812-8581, JAPAN, TEL/FAX:+81-92-642-4403, e-mail: yoshi@geo.kyushu-u.ac.jp
ProcessingLevel
Calibrated
InstrumentIDs
MeasurementType
Magnetogram
TemporalDescription
TimeSpan
StartDate
1990-06-22 00:00:00
StopDate
1993-08-18 23:59:59
Cadence
PT3S
ObservedRegion
Earth.Magnetosphere
SpatialCoverage
CoordinateSystem
CoordinateRepresentation
Spherical
CoordinateSystemName
GEO
NorthernmostLatitude
-2.60
SouthernmostLatitude
-2.60
EasternmostLongitude
-44.20
WesternmostLongitude
-44.20
Keywords
ground observation magnetometer geomagnetic field
Parameter #1
Name
hdz_3sec
Description
3 components and total geomagnetic field value in unit of nano tesla. H is horizontal component (northward positive). D is declination component (northward positive). Z is vertical component (downward positive). Our observation system can keep time accuracy within 0.1 second. However it depends on the receiving condition of radio wave at observatory. Pay attention to use of our data, especially in a study affected by time accuracy. Our recording system cannot record quick variation more than about 2nT/3sec (corresponds to 40nT/min). There is not a problem for use of data in usual variation, but attention is necessary for use of data at SC.
Units
nT
Field
Qualifier
Vector
FieldQuantity
Magnetic