Transcript Slide 1

8:30-9:10 AM: Philip Scherrer,
What Can We Hope to Learn from SDO
Overview of SDO
HMI Investigation
HMI Instrument
MDI Status
Excellent Condition
Half Way
Solar-Heliospheric Activity Research and Prediction Program
SDO-EVE
MEGS - Multiple Euv Grating Spectrograph
ESP - Euv Spectrophotometer
OFS - Optics Free Spectrometer
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 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:
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.
HMI Major Science Objectives
J – Sunspot Dynamics
I – Magnetic Connectivity
B – Solar Dynamo
C – Global Circulation
A – Interior Structure
D – Irradiance Sources
H – Far-side Imaging
E – Coronal Magnetic Field
NOAA 9393
Far-side
G – Magnetic Stresses
F – Solar Subsurface Weather
Name
Role Institution
Philip H. Scherrer
John G. Beck
Richard S. Bogart
Rock I. Bush
Thomas L. Duvall, Jr.
Alexander G. Kosovichev
Yang Liu
Jesper Schou
Xue Pu Zhao
Alan M. Title
Thomas Berger
Thomas R. Metcalf
Carolus J. Schrijver
Theodore D. Tarbell
J. Leonard Culhane
Richard A. Harrison
Bruce W. Lites
Steven Tomczyk
Sarbani Basu
Douglas C. Braun
Philip R. Goode
Frank Hill
Rachel Howe
Jeffrey R. Kuhn
Charles A. Lindsey
Jon A. Linker
N. Nicolas Mansour
Edward J. Rhodes, Jr.
Juri Toomre
Roger K. Ulrich
Alan Wray
J. Christensen-Dalsgaard
Bernhard Fleck
Douglas O. Gough
Takashi Sekii
Hiromoto Shibahashi
Sami K. Solanki
Michael J. Thompson
PI
A-I
Co-I
Co-I
Co-I
Co-I
A-I
Co-I
Co-I
Co-I
A-I
Co-I
Co-I
Co-I
Co-I
Co-I
A-I
Co-I
Co-I
Co I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Co-I
Stanford University
Stanford University
Stanford University
Stanford University
NASA Goddard Space Flight Center
Stanford University
Stanford University
Stanford University
Stanford University
LMSAL
LMSAL
LMSAL
LMSAL
LMSAL
MSSL, University College London, UK
Rutherford Appleton Laboratories, UK
High Altitude Observatory
High Altitude Observatory
Yale University
Colorado Research Associates
NJIT, Big Bear Solar Observatory
National Solar Observatory
National Solar Observatory
University of Hawaii
Solar Physics Research Corp.
Science Applications Intnl. Corp.
NASA Ames Research Center
University of Southern California
JILA, Univ. of Colorado
University of California, Los Angeles
NASA Ames Research Center
TAC, Aarhus University, DK
European Space Agency
IoA, Cambridge University, UK
National Astron. Obs. of Japan, JP
University of Tokyo, JP
Max-Planck-Institut für Aeronomie, DE
Imperial College, UK
Phase B,C,D
HMI Investigation
E/PO Science Liaison
Data Pipeline and Access
Program Manager
Time-Distance Code
Inversion Code
Vector Field Observable Code
Instrument Scientist
Coronal Code
HMI Instrument
* Vector Field Calibration
* Vector Field Calibration
AIA Liaison
HMI Calibration
HMI CCD Cameras
HMI CCD Camera Electronics
Vector Field Inversions
Vector Field Inversions
* Ring Analysis Code
* Farside Imaging Code
* Magnetic and Helioseismic Code
* Ring Analysis Code
* Internal Rotation Inversion Code
* Limb and Irradiance Code
* Farside Imaging Code
* Coronal MHD Model Code
* Convection Zone MHD Model Code
* Helioseismic Analysis Code
* Sub-Surface-Weather Code
* Magnetic Field Calibration Code
* Convection Zone MHD Model Code
* Solar Model Code
ILWS Coordination
* Local HS Inversion Code
Phase-E
Solar Science
Surface Flows
Near Surface Flows
Irradiance and Shape
Helioseismology
Helioseismology
Active Region Fields
Helioseismology
Coronal Field Models
Solar Science
Active Region Science
Active Region Science
Active Region Science
Active Region Science
Active Region Science
Active Region Science
Active Region Science
Active Region Science
Helioseismology
Helioseismology
Fields and Helioseismology
Helioseismology
Helioseismology
Irradiance and Shape
Helioseismology
Coronal Physics
Convection Physics
Helioseismology
Helioseismology
Solar Cycle
Convection Physics
Helioseismology
Atmospheric Dynamics
Helioseismology
Helioseismology
Helioseismology
AR Science
Helioseismology
* Phase D only
HMI Organizational Structure
Principal
Investigator
P. Scherrer
Co-I
Science Team
HAO
S. Tomczyk
Data
Processing
& Analysis
Support
LMSAL Lead
A. Title
Education &
Public Outreach
Stanford University
Program Manager
R. Bush
SU Ground
Data
System
LMSAL HMI
Development
Instrument
Scientist
J. Schou
MSSL/RAL
Camera
System
HMI Master Schedule
Task Name
3
UK
CCDs Detector
Camera
LMSAL
Program Phase
Reviews
Deliveries
Focal Plane Assembly
Lyot
Michelsons
Filter Oven
Optical Elements
HMI Mechanism
Optics Package
Electronics & Software
HMI Instrument
2003
2002
4
1
A
SRR
2
2004
3
1
4
2
3
2005
4
1
2
3
bridge B
Fabricate
1
2
3
GSFC
SU
Ground System
Development
1
2
3
4
1
2
E
Instrument Delivery
Launch
Test
Develop
Test
Develop
Assemble &Test
Test
Assemble
I&T
Develop
Develop
Develop
Design
Assemble & Align Integrate Oven & Focal Plane
Develop
Calibration
Integrate Acceptance
RESERVE
I&T
Spacecraft I&T and Flight
4
Test
Design/Fabrication
Develop
4
2008-2013
2007
C/D
Initial Confirmation Review CDR
PDR
Confirmation Review
Develop
2006
Env. test Launch prep
MO&DA
Commission
System Engineering
Development
Prototype
Production
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:
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
Doppler Velocity
Cadence
Precision
Zero point accuracy
Dynamic range
Vector Magnetic Field
45 s
13 m/s
0.05 m/s
±6.5 km/s
Line-of-Sight Magnetic Flux
Cadence
45 s
Precision
10 G
Zero point accuracy
0.05 G
Dynamic range
± 4 kG
Continuum Intensity
Cadence
45 s
Precision
0.3%
Accuracy pixel to pixel
0.1%
Cadence
Precision:
Polarization
Sunspots (1kG<|B|<4kG)
|B|
Azimuth
Inclination
Quiet Sun (0.1kG<|B|<2kG) *
|B|
Total flux density
Azimuth
Inclination
90 s
0.22%
18G
0.6º
1.4º
220 G
35 G
15º
18º
FeI 6173Å instead of NiI 6768Å
HMI Filter Profiles
HMI Observing Sequence
Time (sec)
λ
D
o
V
P
p
e
o
T
u
p
c
l a
n
l e
t o
r i z
i n
r
r
a
8
g
S
S
0
16
I 1
e
e
t i o
q
I 2
L
R
q
L
L
2
=
I
+
2
V
=
L
L
P
R
1
R
=
-
V
=
2
R
I 5
L
2
I
40
I 4
R
1
C
32
I 3
R
1
n
24
C
P
L
1
1
=
I
+
Q
+
V
R
R
3
2
I
–
4
a
Q
+
V
R
R
3
3
=
+
a
U
4
–
I 5
L
4
I
85
I 4
L
3
b
77
I 3
L
4
=
69
I 2
L
C
b
61
I 1
C
2
a
53
I C
R
1
45
b
V
L
I C
R
3
C
3
4
=
I
4
–
a
U
C
-
b
V
Details of the HMI observing sequence: Time indicates the beginning of the exposures at a given wavelength. The
Wavelength Tuning positions I1 through I5 are spaced evenly 75 mÅ apart, with I3 centered on the line (see Figure
C.8). Doppler Seq and Vector Seq indicate the order and polarizations settings for the two cameras, with the states
L, R, 1, 2, 3, 4 identified by Polarization. For a²=2/3 and b²=1/3, Q, U and V have identical noise equal to 0.22% in
the continuum. IC is a continuum filtergram taken in linear polarization.
Sample MDI Filtergrams
Sample MDI Observables
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.
Lev.
Description
Examples
Rate
[GB/day]
Rate
[TB/yr]
Cache
[day]
Archived
[%]
Raw
Telemetry
-
600
200
30
100
0
Filtergrams
-
1000
400
100
100
Observables
VLOS, BLOS, Ic,
Vector Field
Parameters
400
160
600
30
10
3
3000
100
<1
<1
2000
100
1
2
3
Reorganized
data
Inferences
Spatial/temporal
Samples,
Averages; Synoptic
Maps
Global Modes,
Analysis Maps,
Farside Images,
Coronal Fields
HMI Data Archive
HMI
0.02
Ops
600
SDO
Telemetry
HMI Dataflow Concept
(Gigabytes/day)
1000
400
Data Capture
Lev 1
30d Cache
Online
Data
Telem
Archive
Analysis
Archive
10
ReOrg
Data
Inferences
<1
30d cache
Net Access
HMI Data Analysis Pipeline
HMI Education/Public Outreach Partnerships
Institution
Student K-14 Teacher Assess Multi- Distance Distri- Access Public/
Involve Curric- Workment
media Learning bution of
to
infomal
ment
ulum
shops Support Develop Support Materials Under- education
Develop
ment
served
ment
Stanford
X
X
LMSAL
X
X
Stanford-Haas
X
The Tech Museum
X
X
Chabot SSC
X
Morrison
Planetarium /CA
Academy of
Sciences
X
X
X
X
X
X
IIISE
X
X
X
X
X
X
X
X
X
X
X
X
X
X
X
X
X
X
Lawrence Hall of
Science
NASA-CORE
X
X
X
X
X
X
X
X
X
X
First HMI Science Team meeting in spring 2003
For continuing HMI information see:
http://hmi.stanford.edu