8:30-9:10 AM: Philip Scherrer,

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• 830-910 AM Philip Scherrer,
• What Can We Hope to Learn from SDO
• Overview of SDO
• HMI Investigation
• HMI Instrument

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MDI Status Excellent Condition Half Way
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Solar-Heliospheric Activity Research and
Prediction Program
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• SDO EVE Science Overview
• The EVE program has 4 primary science objectives.
• Advance current understanding of how and why the
  solar EUV spectral irradiance varies
• Specify the solar EUV spectral irradiance and its
  variability on multiple time scales
• Improve the capability to predict the EUV
  spectral irradiance variability
• Understand the response of the geospace
  environment to variations in the solar EUV
  spectral irradiance and the impact on human
  endeavors

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SDO-EVE
MEGS - Multiple Euv Grating Spectrograph
ESP - Euv Spectrophotometer
OFS - Optics Free Spectrometer
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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.
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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.
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• 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
• 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 and 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 description of these tasks reflects our
  current level of understanding and will obviously
  evolve in the course of the investigation.

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• The HMI instrument will produce filtergrams in a
  set of polarizations and spectral line positions
  at a regular cadence for the duration of the
  mission.
• These are combined on the ground to produce
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• 1-arc-second resolution full-disk Doppler
  velocity and line-of-sight magnetic flux
  images at least every 50 seconds
• 1-arc-second resolution full-disk
  vector-magnetic images of the longitudinal solar
  magnetic field at least every 90 seconds

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FeI 6173Å instead of NiI 6768Å
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HMI Filter Profiles
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HMI Observing Sequence
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Sample MDI Filtergrams
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Sample MDI Observables
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The HMI investigation will provide sufficient
computing capability to convert these raw
filtergram measurements into a set of observables
and derived data products that satisfy the HMI
science objectives The primary observables
(Dopplergrams, longitudinal and vector
magnetograms, and continuum intensity images)
will be 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 will be produced. Open
data policy ALL data products will be freely
available as soon as they are created.
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Lev. Description Examples Rate GB/day Rate TB/yr Cache day Archived
Raw Telemetry - 600 200 30 100
0 Filtergrams - 1000 400 100 100
1 Observables VLOS, BLOS, Ic,Vector Field Parameters 400 160 600 30
2 Reorganizeddata Spatial/temporal Samples, Averages Synoptic Maps 10 3 3000 100
3 Inferences Global Modes, Analysis Maps, Farside Images, Coronal Fields lt1 lt1 2000 100
HMI Data Archive HMI Data Archive HMI Data Archive HMI Data Archive HMI Data Archive HMI Data Archive HMI Data Archive
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HMI Dataflow Concept (Gigabytes/day)
0.02
HMI
Ops
SDO
Online Data
Telemetry
30d Cache
lt1
30d cache
Analysis Archive
Telem Archive
Net Access
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HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships HMI Education/Public Outreach Partnerships
Institution Student Involvement K-14 Curric-ulum Development Teacher Work-shops Assessment Support Multi-media Development Distance Learning Support Distri-bution of Materials Access to Under-served Public/ infomal education
Stanford X X X X X X X X X
LMSAL X X X X X X
Stanford-Haas X X X X X
The Tech Museum X X X X X
Chabot SSC X X X X X
Morrison Planetarium /CA Academy of Sciences X X X X
Lawrence Hall of Science X X X X X
IIISE X X
NASA-CORE X
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First HMI Science Team meeting in spring 2003
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• For continuing HMI information see
• http//hmi.stanford.edu