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Transcript
We use the web as a tool for ourselves as well as collaborators and the general public
Our home page has links to our various projects:
Observational Solar Physics at Stanford University
Philip Scherrer
The Solar Group is ~30 people working to better understand the Sun and the sources of its variability.
There are several projects including one on the ground, one in space, and one in development for space.
The Michelson Doppler Imager instrument of the
Stanford Solar Oscillations Investigation
onboard the ESA/NASA Solar and Heliospheric Observatory
has been operating since December 1995
The Wilcox Solar Observatory at Stanford has been operating since 1975
MDI
Optics
Solar polar field strength vs. time
Electronics
MDI observations have enabled better
understanding of the interior structure of the
Sun. The techniques of local
helioseismology have been developed with
MDI data and led to plans for SDO/HMI.
MDI was designed and build as part of an
ongoing collaboration with the solar group
at Lockheed-Martin Solar and Astrophysics
Laboratory in Palo Alto.
WSO is dedicated to long-term
daily observations of the large
scale magnetic fields. Data are
used for analyses and correlative
studies worldwide.
All WSO data is freely available.
WSO Magnetic Field
Synoptic maps of observed
photospheric field have
been made since 1976.
Inferred coronal field maps
are available for each
Carrington rotation. These
predict the polarity structure
in the heliosphere.
Far-side of the Sun magnetic fields
Sound speed beneath a sunspot
Internal rotation
We are interested in developing collaborations for studies of the Sun and Space Weather using WSO, MDI, and shortly HMI observations. All data from these projects is freely available via the web. There are more interesting studies to do with this data than can be accomplished by
the just teams at Stanford and our Co-Investigators and other collaborators. Problems that need significant data volumes can be pre-processed at Stanford so the computing requirements for leading-edge helioseismology need not be a deterrent to new investigations.
Observational Solar Physics Group at
Hansen Experimental Physics Laboratory at
Stanford University
Faculty:
Philip Scherrer
Physics & HEPL
Administrative:
Romeo Durscher
Admin Assistant (financial)
Margaret Stehle
Admin. Assistant (documents)
MDI Data and Operations:
Jim Aloise
System Software
Keh-Cheng Chu
Scientific Software
Sarah Gregory
At GSFC, MDI Observer
Jeneen Sommers
Science & Engineering Assoc.
Hao Thai
Science & Engineering Assoc.
Brian Roberts
Computer Operations
HMI Development, VSO Development
Rock Bush
Sr. Research Scientist
Rasmus Munk Larsen Research Scientist
Karen Tian
Research Scientist
SOI (MDI Helioseismology and motions) Analysis:
Tom Duvall, Jr.
NASA visiting scientist
Alexander Kosovichev Sr. Research Scientist
Jesper Schou
Sr. Research Scientist
Sebastian Couvidat
Research Scientist
Laurent Gizon
Research Scientist
Junwei Zhao
Research Scientist
Rick Bogart
Sr. Research Scientist
John Beck
Research Scientist
Shravan Mukunda
Graduate Student – EE
Shalini Krishnamurthy Graduate Student – SCCM
Christina Green
Graduate Student – SCCM
Majid Modarresi
Graduate Student – SCCM
WSO, Space Weather, Corona, MDI magnetic field:
J. Todd Hoeksema
Sr. Research Scientist
Taeil Bai
Sr. Research Scientist
Xue Pu Zhao
Sr. Research Scientist
Yang Liu
Sr. Research Scientist
Elena Benevolenskaya Research Scientist
Keiji Hayashi
Research Scientist
Bala Poduval
Research Scientist
Paul Boerner
Graduate Student - Physics
Education and Public Outreach:
Deborah Scherrer
E/PO Coordinator
Paul Mortfield
Consultant
HMI
SDO
LWS
SEC
NASA
The Helioseismic and Magnetic Imager
for the Solar Dynamics Observatory
of the Living With a Star program
of the Sun Earth Connection Division
of the NASA Office of Space Science
The primary goal of HMI is to study the origin of
solar variability and to characterize and
understand the Sun’s interior and the various
components of magnetic activity.
Launch in April 2008
Overview 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 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
will help to establish the relationships between the internal solar dynamics and related
magnetic activity.
Specific scientific objectives of the HMI investigation are to measure and study:
1.
2.
3.
4.
5.
Convection-zone dynamics and the solar dynamo;
Origin and evolution of sunspots, active regions and complexes of activity;
Sources and drivers of solar magnetic activity and disturbances;
Links between the internal processes and dynamics of the corona and heliosphere;
Precursors of solar disturbances for space-weather forecasts.
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:
Full-disk velocity and line-of-sight magnetic flux images with 1 arc-sec resolution every 50
seconds.
Full-disk vector magnetic images of the solar magnetic field with 1 arc-sec resolution every
10 minutes.
HMI Optics Package
HMI & AIA Joint Science Operations Center Architecture – The Stanford Solar
Group will provide the ground data system for both HMI and Lockheed-Martin’s
AIA instrument on SDO – Together these represent 95% of the SDO data,
about 1.4TBytes/day
GSFC
White Sands
The HMI investigation will provide sufficient computing capability to convert these raw
Fold Mirror
filtergram measurements into a set of observables and derived data products required for
Alignment Mech
the HMI science objectives. The primary observables (Dopplergrams, longitudinal and
Oven Structure
vector magnetograms, and continuum intensity images) will be constructed from the raw
Michelson Interf.
filtergrams and will be made available at full resolution and cadence. Other derived
Lyot Filter
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 and made
available. All HMI data products will be made available to all interested investigators.
Shutters
Limb Sensor
Detector
(Vector)
CEBs
Stanford
HMI & AIA
Operations
Redundant
Data
Capture
System
HMI JSOC Pipeline Processing
System
Primary
Archive
30-Day
Archive
Active Mirror
Polarization Selector
Focus/Calibration Wheels
OP Structure
Telescope
Front Door
HOP
Support Legs (6)
HEB
SDO will carry The Atmospheric Imaging Array
provided by Lockheed Martin Solar and
Astrophysics Lab and the EUV Variability
Experiment provided by the University of
Colorado in addition to HMI.
Offsite
Archiv
e
Offline
Archiv
e
Data
Export
& Web
Service
AIA
Analysis
System
LM-Local
Archive
Catalog
Vents
Limb B/S
Housekeeping
Database
Quicklook
Viewing
Detector
(Doppler)
Front Window
LMSAL
MOC
DDS
Connector Panel
Focal Plane B/S
The web provides access to many of our E/PO activities. See also the poster by John Beck
The HMI team includes researchers from 23 institutions.
Additional collaborations are welcome.
High-Level
Data Import
World
Science Team
Forecast Centers
EPO
Public