HMI Major Science Goals
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 Sun's interior and the various components of magnetic activity. The HMI investigation is based on measurements obtained with the HMI instrument, one of the three instruments that make up 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 specific 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, which is where the Earth is. Solar variability that affects the Earth is called "space weather". HMI observations will help establish the relationships between internal dynamics and magnetic activity. In turn this will lead to better understanding of solar variability and its effects. This will lead to reliable predictive capability, one of the key elements of the Living With a Star (LWS) program. HMI investigation goals are to observe and understand these interlinked processes of magnetic activity and internal dynamics including:
- 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.
The HMI instrument design and observing strategy are based on the highly successful MDI instrument, with several important improvements. HMI will observe the full solar disk in the Fe I absorption line at 6173Å with a resolution of 1 arc-second. 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.
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 Stanford University.
HMI Science: Solar Interior Dynamics and
Photospheric Magnetic Fields
The downward propagating waves are refracted upward by the temperature gradient and the upward propagating waves are reflected inward by the drop in density at the surface.
The travel times of these waves depend on the temperature, composition, motion, and magnetic fields in the interior. The visible surface moves when the waves are reflected.HMI measures this motion enabling the wave frequency, phase, and amplitude to be measured.
Analysis of travel times over a multitude of interior paths enables inference of internal conditions.
How HMI Works: HMI measures a long sequence of Dopplergrams (maps of solar surface velocity) and magnetograms (maps of magnetic field at the Sun's visible surface, the photosphere.) Each map of motion or magnetic field is computed on the ground from a set of 12 images of the Sun, each obtained with a different combination of wavelength tuning and polarization direction. The wavelength tuning compared to the chosen solar spectral absorption line is shown in this figure. The black line at the top shows the solar iron spectral line profile. The. colored lines show the HMI filter transmission profiles at 7.6 pm tuning spacing.
The black dashed line is the profile used for the continuum filtergram. A picture is made for each tuning and the results are used to compute velocity and magnetic field strength at each pixel. The polarization selector needed for magnetic field measurements is a set of waveplates that can be rotated to different angles for detection of different polarization parameters (called Stokes I,Q,U,V) The wavelength selection and tuning is accomplished with a set of successively narrower bandpass filters. These are the front window, blocking filter, a five element Lyot filter, and two Michelson interferometers. The last three filter stages can be tuned by rotating retarder waveplates. The combination results in a 7.6 pm bandpass that can be tuned over 68 pm and is centered on the 617.3 pm solar line. (1 pm = 10 mÅ)
History / Background / Prior missions
The need for an instrument like HMI was recognized in 1996 with the conceptual design developed in 1998. The SDO mission definition study in 2001 clarified the requirements, with real work on HMI beginning after a competitive selection process in 2002. The Helioseismic and Magnetic Imager is a new and improved version of the Michelson Doppler Imager (MDI) instrument on the Solar and Heliospheric Observatory (SOHO). SOHO is a joint project of the European Space Agency and NASA. MDI was developed starting in 1988 by the same collaboration between Stanford and Lockheed teams that developed HMI. SOHO was launched in December 1995. SOHO/MDI is presently still operating well and has completed helioseismic and magnetic field observation of the Sun for all of solar cycle 23 and the beginning of cycle 24. HMI will continue these important measurements from space into the next solar cycle. We hope and anticipate that SDO/HMI will enable deeper understanding of solar processes during most of solar cycle 24.
SDO web link: http://sdo.gsfc.nasa.gov
HMI web link: http://hmi.stanford.edu
HMI/AIA JSOC data center: http://jsoc.stanford.edu
WWW Access Statistics for the servers of the Solar Physics Research Group.
Page last revised Friday, March 4, 2011