HDPWS

SDO/HMI line-of-sight Magnetogram

(2011). SDO/HMI line-of-sight Magnetogram. [Data set]. Joint Science Operations Center (JSOC), Stanford University.

ResourceID
spase://NASA/NumericalData/SDO/HMI/LOS_Magnetogram/PT45S

Description
Magnetograms are maps of the observed solar magnetic field in the photosphere. The line-of-sight component of the field can be accurately measured as it evolves in time over the full visible disk of the Sun. The HMI instrument exploits the Zeeman effect, which allows the strength of the line-of-sight component of the magnetic field to be determined by measurements of the spectral line in circularly polarized light. HMI makes two independent measurements of the line-of-sight component of the photospheric magnetic field. One is collected every 45 seconds with the HMI Doppler camera. The other is computed every 720 seconds using filtergrams recorded by the Vector Field camera. The spatial resolution is 1 arc second (half arc-second pixels) and the full disk images are collected on a 4096**2 detector. The noise level is nominally between 5 and 10 Gauss. HMI really measures flux density in Mx/cm2 in each pixel.

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Details

Version:2.6.1

NumericalData

ResourceID
spase://NASA/NumericalData/SDO/HMI/LOS_Magnetogram/PT45S
ResourceHeader
ResourceName
SDO/HMI line-of-sight Magnetogram
ReleaseDate
2024-10-11 00:08:46
RevisionHistory
RevisionEvent
ReleaseDate
2024-10-11 00:08:46
Note
Metadata created by SY
Description
Magnetograms are maps of the observed solar magnetic field in the photosphere. The line-of-sight component of the field can be accurately measured as it evolves in time over the full visible disk of the Sun. The HMI instrument exploits the Zeeman effect, which allows the strength of the line-of-sight component of the magnetic field to be determined by measurements of the spectral line in circularly polarized light. HMI makes two independent measurements of the line-of-sight component of the photospheric magnetic field. One is collected every 45 seconds with the HMI Doppler camera. The other is computed every 720 seconds using filtergrams recorded by the Vector Field camera. The spatial resolution is 1 arc second (half arc-second pixels) and the full disk images are collected on a 4096**2 detector. The noise level is nominally between 5 and 10 Gauss. HMI really measures flux density in Mx/cm2 in each pixel.
PublicationInfo
Authors
The HMI Consortium: Stanford University (USA); NASA Goddard Space Flight Center (USA); Lockheed Martin Solar and Astrophysics Laboratory (USA); National Center for Atmospheric Research (USA);
PublicationDate
2011-01-21 00:00:00
PublishedBy
Joint Science Operations Center (JSOC), Stanford University
Contacts
Role Person StartDate StopDate Note
1. PrincipalInvestigator spase://SMWG/Person/Philip.H.Scherrer
2. GeneralContact spase://SMWG/Person/Rick.Bogart

InformationURL
Name
The HMI website at Stanford
URL
InformationURL
Name
The SDO/HMI Instrument paper
URL
AccessInformation
RepositoryID
Availability
Online
AccessRights
Open
AccessURL
Name
JSOC Data Center
URL
Style
Search
Description
Change the date and the time to find the HMI data.
AccessURL
Name
SDO/HMI Data Search via Virtual Solar Observatory
URL
Description
VSO path to JSOC-resident SDO HMI data files
Format
FITS
InstrumentIDs
MeasurementType
Magnetogram
TemporalDescription
TimeSpan
StartDate
2010-03-29 07:49:47
RelativeStopDate
-P3D
Cadence
PT45S
ObservedRegion
Sun
ObservedRegion
Sun.Photosphere
Parameter #1
Name
FITS Data Array
Description
Line-of-sight magnetic field strength
Cadence
PT45S
Units
gauss
CoordinateSystem
CoordinateRepresentation
Cartesian
CoordinateSystemName
HPC
Wave
WaveType
Photon
WaveQuantity
Polarization
WavelengthRange
Low
6173
High
6173
Units
angstrom
SpatialCoverage
CoordinateSystem
CoordinateRepresentation
Cartesian
CoordinateSystemName
HPC
Description
Array size: 4096x4096 Pixel Resolution: 0.504 arcsec