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1.B – Solar Dynamo

The Helioseismic & Magnetic Imager on the Solar Dynamics Observatory. J. T. Hoeksema for The HMI Team – Stanford University, LMSAL, HAO, ++. 1.B – Solar Dynamo. 1.J – Sunspot Dynamics. 1.C – Global Circulation. 1.I – Magnetic Connectivity. 1.A – Interior Structure. 1.D – Irradiance Sources.

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1.B – Solar Dynamo

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  1. TheHelioseismic & Magnetic Imageron theSolar Dynamics Observatory J. T. Hoeksema for The HMI Team – Stanford University, LMSAL, HAO, ++ 1.B – Solar Dynamo 1.J – Sunspot Dynamics 1.C – Global Circulation 1.I – Magnetic Connectivity 1.A – Interior Structure 1.D – Irradiance Sources 1.E – Coronal Magnetic Field 1.H – Far-side Imaging 1.F – Solar Subsurface Weather 1.G – Magnetic Stresses 1.A Sound speed variations relative to a standard solar model. 1.B Solar cycle variations in the sub-photospheric rotation rate. 1.C Solar meridional circulation and differential rotation. 1.D Sunspots and plage contribute to solar irradiance variation. 1.E MHD model of the magnetic structure of the corona. 1.F Synoptic map of the subsurface flows at a depth of 7 Mm. 1.G EIT image and magnetic field lines computed from the photospheric field. 1.H A ctive regions on the far side of the sun detected with helioseismology. 1.I Vector field image showing the magnetic connectivity in sunspots. 1.J Sound speed variations and flows in an emerging active region. HMI Observables HMI Sun-Test Data Products Fold Mirror Assembly BDS Beam-splitter Assembly Michelson Interferometer Alignment Mechanism Filter Oven Assembly Lyot Filter Assembly Oven Controller E-Box Focus Mechanism ISS Mirror Assembly Hollow Core Motors Secondary Lens Assembly Structure Focal Plane Assembly ISS Beam-splitter Assembly Limb Sensor Assembly ISS Pre-Amp Electronics Box Camera Electronics Box Telescope Assembly Primary Lens Assembly Front Window Assembly Front Door Assembly First Dopplergram First Magnetogram HMI Principal Optics Package Components Mechanical Characteristics: 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 Z Optical Characteristics: Effective Focal Length: 495 cm Telescope Clear Aperture: 14 cm X Y ABSTRACT Investigators using the Helioseismic and Magnetic Imager (HMI) will study the origin of solar variability and will characterize and understand the interior of the Sun and the various components of magnetic activity. HMI is part of the Solar Dynamics Observatory (SDO) a satellite scheduled for launch into geosynchronous orbit in 2009. SDO is NASA’s first Living With a Star (LWS) mission. HMI will measurement motions of the solar photosphere to study solar oscillations and will measure polarization to study the vector magnetic field. HMI will help establish the relationships between the internal dynamics and magnetic activity in order to understand solar variability and its effects. The prime goal of the mission is to develop the knowledge needed for a reliable predictive capability, one of the key elements of the International Living With a Star (ILWS) program. The Michelson Doppler Imager (MDI) instrument on SOHO has been making helioseismic and magnetic field observations of the Sun since the beginning of Solar Cycle 23. HMI will continue these important measurements from space into the next solar cycle. The HMI instrument is an evolution of the successful MDI design with key improvements in resolution, image cadence, continuity, and vector magnetic field measurement capabilities. Filtergrams of the Fe I spectral line at 617.3 nm made with the HMI tunable narrow band filter system determine motions of the solar photosphere to study solar oscillations. Polarization measurements in this same spectral line enable determination of all three components of the photospheric magnetic field. The web site hmi.stanford.edu provides more information.

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