Design and Ground Calibration of the Helioseismic and Magnetic Imager (HMI) Instrument on the Solar Dynamics Observatory (SDO)

By J. Schou, P. Scherrer, R. Bush, R. Wachter, S. Couvidat, M. Rabello-Soares, R. Bogart, J. Todd Hoeksema, Yang Liu, T. Duvall and 11 more. 2012

1,760 citations recorded by the source corpus.

The Helioseismic and Magnetic Imager (HMI) investigation (Solar Phys. doi:10.1007/s11207-011-9834-2, 2011) will study the solar interior using helioseismic techniques as well as the magnetic field near the solar surface. The HMI instrument is part of the Solar Dynamics Observatory (SDO) that was launched on 11 February 2010. The instrument is designed to measure the Doppler shift, intensity, and vector magnetic field at the solar photosphere using the 6173 Å Fe i absorption line. The instrument consists of a front-window filter, a telescope, a set of waveplates for polarimetry, an image-stabilization system, a blocking filter, a five-stage Lyot filter with one tunable element, two wide-field tunable Michelson interferometers, a pair of 40962 pixel cameras with independent shutters, and associated electronics. Each camera takes a full-disk image roughly every 3.75 seconds giving an overall cadence of 45 seconds for the Doppler, intensity, and line-of-sight magnetic-field measurements and a slower cadence for the full vector magnetic field. This article describes the design of the HMI instrument and provides an overview of the pre-launch calibration efforts. Overviews of the investigation, details of the calibrations, data handling, and the science analysis are provided in accompanying articles.

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/a46efa70a663a2d21fed12e18d983316e74b957e

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Citations in the corpus

DETECTION OF EQUATORWARD MERIDIONAL FLOW AND EVIDENCE OF DOUBLE-CELL MERIDIONAL CIRCULATION INSIDE THE SUN (2013, background): “The continuous Doppler observations by the Helioseismic and Magnetic Imager (HMI; Scherrer et al. 2012; Schou et al. 2012) onboard the recently launchedSolar Dynamics Observatory mission (SDO; Pesnell et al. 2012) allow us to measure and detect the long-s u ht equatorward flow.”
The Polarimetric and Helioseismic Imager on Solar Orbiter (2019, methodology): “Co-ordinated observations at the correct phase of its orbit by SO/PHI and by an instrument in the Sun-Earth line observing at the same wavelength (e.g. SDO/HMI) will give direct measurements of photospheric height differences.”
The magnetic field in the solar atmosphere (2014, methodology): “AR(s) Active Region(s) CH(s) Coronal Hole(s) CME(s) Coronal Mass Ejection(s) ECH(s) Equatorial Coronal Hole(s) EUV Extreme Ultraviolet) FOV Field-Of-View FASR Frequency Agile Solar Radiotelescope (Gary and Keller, 2005) GOES Geostationary Operational Environmental Satellite (http://www.goes.noaa.gov”
SOLAR FLARE PREDICTION USING SDO/HMI VECTOR MAGNETIC FIELD DATA WITH A MACHINE-LEARNING ALGORITHM (2014, background): “Active region features: the SHARP parameters The HMI data repository, located at the Joint Science Operations Center1, contains the first continuous measurement of the full-disk photospheric vector magnetic field taken from space (Schou et al., 2012).”
Predicting Solar Flares Using SDO/HMI Vector Magnetic Data Products and the Random Forest Algorithm (2017, background): “It is notable that since 2010 May, the Helioseismic and Magnetic Imager (HMI; Schou et al. 2012) on board the Solar Dynamics Observatory (SDO; Pesnell et al. 2012) has been producing unprecedented photospheric vector magnetograms with continuous high-cadence (normally 12 minutes), full-disk…”
Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, methodology): “…the 1 m New Vacuum Solar Telescope (NVST; Liu et al. 2014a) at the Fux- ian Solar Observatory, China, the 1.5 m GREGOR telescope (Schmidt et al. 2012; Schou et al. 2012) at the Teide Observatory, Tenerife, and the 1.6 m New Solar Telescope (NST; Cao et al. 2010) at the Big Bear Solar Observatory…”
MAGNETIC PROPERTIES OF SOLAR ACTIVE REGIONS THAT GOVERN LARGE SOLAR FLARES AND ERUPTIONS (2016, methodology): “In order to identify the physical parameters that may characterize the flare events, we used the observational data taken by the Helioseismic and Magnetic Imager (HMI; Scherrer et al. 2012; Schou et al. 2012) and the Atmospheric Imaging Assembly (AIA; Lemen et al. 2012) aboard SDO.”
The standard flare model in three dimensions - I. Strong-to-weak shear transition in post-flare loops (2012, methodology): “We identify the magnetic field of its source region by using line-of-sight magnetograms from the Helioseismic and Magnetic Imager (HMI: Schou et al. 2012) from SDO, recorded at the time of its passage through the central meridian (i.e. three weeks before and one week after the day of the event).”
Comparison of Line-of-Sight Magnetograms Taken by the Solar Dynamics Observatory/Helioseismic and Magnetic Imager and Solar and Heliospheric Observatory/Michelson Doppler Imager (2012, methodology): “The HMI instrument (Schou et al., 2012) is a filtergraph with full-disk coverage by 4096,×4096 pixels.”
Solar Orbiter (2012, background): “…and subsurface flow fields at low and middle latitudes has seen major advances, largely due to the availability of high-quality data from the SOHO’s Michelson Doppler Imager (MDI: Scherrer et al., 1995) instrument and, more recently, SDO’s Helioseismic and Magnetic Imager (HMI: Schou et al., 2012).”
WHY IS THE GREAT SOLAR ACTIVE REGION 12192 FLARE-RICH BUT CME-POOR? (2015, methodology): “Here, we utilize photospheric vector magnetic data from the Helioseismic and Magnetic Imager (HMI; Schou et al. 2012) on board the Solar Dynamics Observatory (SDO) to probe the cause and consequence of the largest confined flare (X3.”
Magnetic Flux Transport at the Solar Surface (2014, methodology): “One approach, adopted by Schrijver (2001) and Upton and Hathaw y (2014), is to include in the advection velocities and small-scale cellular flows or random motions corresponding to, e.g., supergranulation.”
CRISPRED: A data pipeline for the CRISP imaging spectropolarimeter (2014, methodology): “By use of a code developed by Norén (2013) we measured the image scale in the CRISP WB camera by comparison with approximately co-temporal 617 nm continuum images from SDO/HMI (Schou et al. 2012).”