The HMI AIA Joint Science Operations (JSOC-SDP) Science
HMI AIA Joint Science Operations (JSOC-SDP)
Science Data Processing for the Solar Dynamics Observatory
Helioseismic & Magnetic Imager on the Solar Dynamics Observatory
The HMI Team Stanford University, LMSAL, HAO, ++
HMI Recent Progress & Current HMI Activities
HMI Major Science Objectives
The primary goal of the Helioseismic and Magnetic Imager (HMI) investigation is to
study the origin of solar variability and to characterize and understand the Suns interior
and the various components of magnetic activity. The HMI investigation is based on
measurements obtained with the HMI instrument as part of the Solar Dynamics
Observatory (SDO) mission. HMI makes measurements of the motion of the solar
photosphere to study solar oscillations and measurements of the polarization in a spectral
line to study all three components of the photospheric magnetic field. HMI produces data
to determine the interior sources and mechanisms of solar variability and how the
physical processes inside the Sun are related to surface magnetic field and activity. It also
produces data to enable estimates of the coronal magnetic field for studies of variability
in the extended solar atmosphere. HMI observations will enable establishing the
relationships between the internal dynamics and magnetic activity in order to understand
solar variability and its effects, leading to reliable predictive capability, one of the key
elements of the Living With a Star (LWS) program.
The broad goals described above will be addressed in a coordinated investigation in a
number of parallel studies. These segments of the HMI investigation are to observe and
understand these interlinked processes:
The JSOC-SDP Team Stanford University
Convection-zone dynamics and the solar dynamo;
Origin and evolution of sunspots, active regions and complexes of activity;
Sources and drivers of solar activity and disturbances;
Links between the internal processes and dynamics of the corona & heliosphere;
Precursors of solar disturbances for space-weather forecasts.
These goals address long-standing problems that can be studied by a number of
immediate tasks. The approaches to study these processes reflect our current level of
understanding and will obviously evolve in the course of the investigation.
(as of May 2010)
SDO with HMI was launched on Feb 11, 2010.
The HMI aperture door was opened on March 24.
Limb Sensor Assembly
Filter Oven Assembly
ISS Pre-Amp Electronics
Lyot Filter Assembly
Oven Controller E-Box
Camera Electronics Box
ISS Mirror Assembly
Primary Lens Assembly
Hollow Core Motors
Front Window Assembly
Secondary Lens Assembly
Front Door Assembly
Effective Focal Length: 495 cm
Telescope Clear Aperture: 14 cm
Box: 0.84 0.55 0.16 m
Over All: 1.19 0.83 0.30 m
Mass: 44.0 kg
First Mode: 73 Hz
We expect stable data products to be regularly available starting mid
HMI level-1 science data will be available within a day or so after
Regular processing of higher level products will begin during the
next few months.
Access to HMI data is available via the HMI/AIA JSOC (see right half
of this poster) and VSO.
The HMI instrument design and observing strategy are based on the highly
successful MDI instrument, with several important improvements. HMI observes
the full solar disk in the Fe I absorption line at 6173 with a resolution of 1 arcsecond. HMI consists of a refracting telescope, a polarization selector, an image
stabilization system, a narrow band tunable filter and two 4096 pixel CCD
cameras with mechanical shutters and control electronics. The continuous data
rate is 55Mbits/s.
The polarization selector, a set of rotating waveplates, enables measurement of
Stokes I, Q, U and V with high polarimetric efficiency. The tunable filter, a Lyot
filter with one tunable element and two tunable Michelson interferometers, has a
tuning range of 600 m and a FWHM filter profile of 76 m.
Images are made in a sequence of tuning and polarizations at a 4-second cadence
for each camera. One camera is dedicated to a 45s Doppler and line-of-sight field
sequence while the other to a 90s vector field sequence. All of the images are
downlinked for processing at the HMI/AIA Joint Science Operations Center at
The data volume is large, more than a terabyte per day. Thus we encourage users to export
only the data they actually need for immediate analysis. We are committed to provide tools
to allow subsetting of the data and of providing multiple access tools appropriate for
different data volumes for different users.
Dopplergrams, Line-ofSight magnetograms,
Continuum Proxy Intensity,
6173A line width, line depth
respectively, observed at
Final products available
after mid June will not have
the _test suffix to the
project name. Units are m/
s, gauss, DN/s, mA, and
Stokes I,Q,U,V at 12 minute 24 quantities are saved for
each time step. IQUV for
each of 6 filter tuning
The solid lines show the HMI filter transmission profiles at 76 m spacing. The
black dashed line is the profile used for the continuum filtergram. The dotted
line shows the Fe I line profile.
Contributors to the HMI development up through launch include:
*Tom Duvall, Jr.
Gregory L. Card
Rebecca C. Elliott
Arturo Lopez Ariste
U. of Hawaii
*Jeff. R. Kuhn
*Ed J. Rhodes, Jr.
S. Paul Rajaguru
Sheffield Univ. UK
Univ. Tokyo, JP
e2v - CCDs
RAL - Cameras
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