Overview of Objectives and Requirements of the Helioseismic and
Magnetic Imager Investigation
The
primary scientific objectives of the Helioseismic and Magnetic Imager (HMI)
investigation are to improve understanding of the interior sources and
mechanisms of solar variability and the relationship of these internal physical
processes to surface magnetic field structure and activity. The HMI
investigation is based on inferences to be made from measurements obtained by
the HMI instrument as part of the Solar Dynamics Observatory (SDO) mission. The
HMI instrument will make measurements of the dynamic motion of the solar
photosphere on global and local solar scales to study solar surface
oscillations and will make similarly scaled measurements of the polarization in
a spectral line to study all three components of the photospheric magnetic
field. HMI observations are crucial for establishing the relationships between
the internal solar dynamics and related magnetic activity, leading to an
understanding of the limits of and possible development of techniques for
reliable predictive capability.
Specific
scientific objectives of the HMI investigation are to measure and study:
To
enable accomplishment of the science objectives of the investigation, the HMI
instrument will produce measurements in the form of filtergrams in a set of
polarizations and spectral line positions at a regular cadence for the duration
of the mission that meet these basic requirements:
The HMI data completeness and continuity requirement is to
capture 99.99% of the HMI data 95% of the time.
In
addition, the HMI investigation will provide sufficient computing capability to
convert these raw filtergram measurements into a set of observables and derived
data products required for the HMI science objectives. The primary observables
(Dopplergrams, longitudinal and vector magnetograms, and continuum intensity
images) will be constructed from the raw filtergrams and will be made available
at full resolution and cadence. Other
derived products such as subsurface flow maps, far-side activity maps, and coronal and
solar wind models that require longer sequences of observations shall be
produced and made available. All HMI data products will be made available to
all interested investigators.