Download SDO Systems Retreat

Solar Dynamics Observatory (SDO)
Project Manager:
Ken Schwer
[email protected]
Project Scientist:
Barbara Thompson
[email protected]
Deputy Project Manager:
DPM Resources:
Business Manager:
Rob Lilly
Tom Miller
Wanda Harrell
LIVING WITH A STAR (LWS) GOAL
Develop the scientific understanding necessary to
effectively address those aspects of the connected
Sun-Earth system that directly affect life and society
2 SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 2
What SDO is designed to do
In order to meet the needs of the Living With a Star program and
determine the drivers and diagnostics of solar activity and
variability which affect Earth and humanity, the Solar Dynamics
Observatory must:
• Provide nearly continuous coverage of solar activity
• Provide coverage of the regimes (interior, photosphere,
corona) in which the activity occurs
• Provide sufficient data on the types of phenomena
which impact Earth, near-Earth space and humanity
• Observe over the relevant timescales (seconds to
years) of solar variability
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 3
SDO OVERVIEW
•
•
•
•
First Living With a Star (LWS) Mission, part of Sun-Earth Connection theme
Will characterize the dynamic state of the Sun enhancing the understanding of solar
processes and space weather.
NASA GSFC will manage the mission, build the S/C in-house, manage and integrate the
instruments, develop/manage the Ground System & Mission Operations, and perform
Observatory environmental testing at GSFC
SDO Investigations:
– Helioseismic Magnetic Imager (HMI); PI: Phil Scherrer – Stanford; Images the Sun’s helioseismic and
magnetic fields to understand the Sun’s interior and magnetic activity
– Solar Heliospheric Activity Research & Prediction Program (SHARPP); Atmospheric Imaging Assembly
(AIA) & Guide Telescope (GT) and White light coronagraph (KCOR); PI: Russ Howard – NRL; Images
the corona to link changes to surface and interior changes
– Extreme Ultraviolet Variability Experiment (EVE); PI: Tom Woods – LASP, Univ. of CO; measures the
solar extreme ultraviolet (EUV) irradiance to understand variations
•
August 2007 EELV launch from KSC into GEO-Transfer Orbit (GTO), circularize to GEOSync Orbit, inclined 28.5 degrees
– Provide continuous high rate data (150 Mbps) stream to dedicated ground station
– Spacecraft: robust, three-axis stabilized, solar-tracking with low jitter
•
Design Drivers: Continuous high data rate/volume, Geosynchronous orbit (mass to
orbit, radiation), 5 year mission life, Instrument pointing and stability
4
SDO Observatory Concept
AIA
SPECTRE
KCOR
AIA
Magritte
HMI
EVE
5
SDO investigations in brief
The science of SDO will be performed by its three investigations:
EUV Variability Experiment (EVE, PI: Tom Woods, University of Colorado):
–
–
Measure the EUV spectral irradiance from 0.1 to 105 nm at a cadence of 10 seconds.
EVE will specify the spectral irradiance with a sensitivity that allows us to gauge the energy input
into the complex processes of the Earth's atmosphere and near-Earth space. Its temporal
resolution will allow us, for the first time, to understand the flare-induced impacts on these
processes.
Helioseismic and Magnetic Field Investigation (HMI, PI: Phil Scherrer, Stanford
University):
–
–
–
Measure the Doppler shifts due to oscillation velocities over the entire visible disk.
High-resolution measurements of the longitudinal and vector magnetic field over the whole visible
disk of the Sun.
HMI will observe the interior processes governing the transition from solar minimum to solar
maximum, will be able to probe the dynamics of the near-surface shear layer to observe local
strong flux regions before they reach the photosphere, and will measure the highly variable
magnetic field.
Solar-Heliospheric Activity Research and Prediction Program (SHARPP, PI: Russell
Howard, Naval Research Laboratory):
–
–
–
Seven telescopes with the spatial resolution of TRACE but a full-Sun field of view to provide
chromospheric and coronal images at a 10-second cadence.
A high-cadence coronagraph to connect those measurements to the inner heliosphere.
SHARPP will capture the initiation and progression of dynamic processes, with the spatial
resolution necessary to understand their connection to the magnetic field and the spectral
coverage to infer the processes at multiple temperatures.
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 6
The Science of SDO
•
SDO is the first mission in the "Living With a Star" program. LWS is a program
within NASA's Sun-Earth Connections theme.
•
Living With a Star is a program which addresses the question "How and why
does the Sun vary, how does the Earth respond, and what are the impacts on
humanity?" Specifically, SDO will address the following LWS goals:
–
Understand solar variability and its effects on space and Earth environments.
–
Obtain information for mitigating undesirable effects of solar variability on human
technology.
–
Understand how solar variability can affect life on Earth:
•
To enable better understanding of global climate change caused by both natural (solar variability,
volcano eruptions) and human drivers.
•
To better predict how stellar variability affects life in other stellar systems.
•
SDO builds on the tremendous success of recent missions such as SOHO,
TRACE, TIMED and SORCE (among others). We ensure the scientific success of
SDO by learning from our previous success, taking into account the unique
assets and challenges of SDO.
•
The international partnership of LWS is called International Living With a Star
(ILWS).
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 7
The Science of SDO
The goal of SDO is to answer the following questions:
1. What mechanisms drive the quasi-periodic 11-year cycle of solar activity?
2. How is active region magnetic flux synthesized, concentrated, and dispersed
across the solar surface?
3. How does magnetic reconnection on small scales reorganize the large-scale
field topology and current systems? How significant is it in heating the corona
and accelerating the solar wind?
4. Where do the observed variations in the Sun’s EUV spectral irradiance arise,
and how do they relate to the magnetic activity cycles?
5. What magnetic field configurations lead to the CMEs, filament eruptions, and
flares that produce energetic particles and radiation?
6. Can the structure and dynamics of the solar wind near Earth be determined
from the magnetic field configuration and atmospheric structure near the solar
surface?
7. When will activity occur, and is it possible to make accurate and reliable
forecasts of space weather and climate?
From the SDO Science Definition Team Report, July 2001
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 8
Research and Data Analysis
Science Questions
SDT -> AO
AO Measurement
Objectives
Level 1 Science
Measurement
Requirements
SDO Investigations:
• Develop Instrumentation to meet
Level 1 Measurement Requirements
• Propose Science Investigations to
answer Science Questions
• Communicate results through
scientific journals and E/PO program
Data Products
Research and
Data Analysis
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
E/PO Program
Page 9
Investigation Science Objectives
The PI Teams, in response to the AO, have devised investigations designed to answer all seven of
these questions. Each investigation has defined a set of Investigation Science Objectives:
EVE
E-1. Specify the solar EUV spectral irradiance and its variability on multiple time scales
E-2. Advance current understanding of how and why the solar EUV spectral irradiance varies.
E-3. Improve the capability to predict the EUV spectral irradiance variability.
E-4. Understand the response of the geospace environment to variations in the solar EUV spectral irradiance and the impact on
human endeavors.
HMI
H-1. Convection Zone dynamics and solar dynamo
H-2. Origin and Evolution of sunspots, active regions and complexes of activity
H-3. Sources and drivers of solar activity and disturbances
H-4. Links between the internal processes and dynamics of the corona and heliosphere
H-5.Precursors of solar disturbances for space weather forecasts
SHARPP
S-1. Link solar magnetic features to irradiance variability at earth
S-2. Link observed/derived plasma characteristics to the associated magnetic structures throughout the photosphere,
chromosphere, transition region, and corona, as they evolve over the solar cycle
S-3. Determine the nature of the coronal heating mechanism(s)
S-4. Understand the origin of flares and their relation to CME’s
S-5. Detect and measure reconnection signatures (e.g., Jets) characteristic of competing CME initiation models
S-6. Understand the origin and nature of global waves and dimmings that accompany many fast CME’s
S-7a. Determine the effects of ambient magnetic field topology and complexity will have on the initiation and propagation of CMEs
S-7b. Determine the factors associated with geoeffectiveness of CMEs over the solar cycle
S-8. Understand the heating and initiation of the fast wind in coronal holes
S-9. Understand active region expansion, streamer formation, and the nature of the slow wind
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 10
Linkage from Science Goals to Objectives
By satisfying the Investigation Science Objectives, the Science Goals of SDO are addressed, as shown in
the following table ("X" denotes an Objective that directly addresses a Science Goal, while "S" indicates an
Objective which supports the goal.)
Instrument Science Objective
Science Quest ion
E- E- E- E- H- H- H- H- H- S- S- S- S- S- S- S- S- S- S1 2 3 4 1 2 3 4 5 1 2 3 4 5 6 7a 7b 8 9
What mechanisms drive the quasi-periodic 11-year
cycle of solar activity?
S
How is act ive region magnetic flux synt hesized,
concent rated, and dispersed across t he solar
surface?
S
How does magnet ic reconnection on small scales
reorganize the large-scale field topology and
current systems? How significant is it in heat ing
the corona and accelerat ing the solar wind?
S
Where do the observed variations in t he SunΥs
EUV spectral irradiance arise, and how do they
relate to the magnet ic activity cycles?
X
X
X
X
X
What magnet ic field configurat ions lead t o t he
CMEs, filament erupt ions, and flares that produce
energet ic particles and radiat ion?
S
X
Can the structure and dynamics of the solar wind
near Eart h be determined from the magnet ic field
configuration and at mospheric struct ure near the
solar surface?
S
S
X
X
X
S
X
S
X
X
X
When will act ivity occur, and is it possible to make
accurate and reliable forecasts of space weather
and climate?
X
X
X
S
X
X
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
S
X
S
S
X
X
S
S
X
X
X
X
X
S
S
X
X
X
S
X X
X
X
X
X
X
X
X
S
S
X
S
X
X
X
S
Page 11
SDO Measurement Objectives
1. Provide data for near-surface diagnostics of the dynamics of the solar interior that are sufficient for both global and local
helioseismology. (Dopplergrams)
2. Provide information about the global solar magnetic field, the active region evolution, small-scale features, and sources of
irradiance variations. (Longitudinal and Vector Magnetic Field Images, Atmospheric Images, Spectral Irradiance Measurements)
3. Characterize the rapid evolution of plasma in the chromosphere and lower corona with a field of view and spectral coverage
sufficient to facilitate linkage with the coronagraph images and to help interpret the EUV spectral irradiance measurements.
(Atmospheric Images, Coronagraphic Images, Spectral Irradiance Measurements)
4. Characterize the solar extreme ultraviolet (EUV) irradiance on timescales ranging from seconds to years to understand the solar
variation caused by solar magnetic field evolution, and to study the solar induced variations of the Earth's ionosphere and
thermosphere. (Longitudinal and Vector Magnetic Field Images, Atmospheric Images, Spectral Irradiance Measurements)
Science Question
Measurement Objective
Wha t mechan is ms drive the qua si-periodic 11-year
1 (2, 3, 4 are seconda ry)
cyc le of solar activit y?
How is active region magne tic flux synthes iz ed,
1, 2, 3 (4 is second ary)
conc entrated, and dispersed across the solar surface?
How does magne tic reconnec tion on small scale s
2, 3 (4 is second ary)
reorganize the large-scale field topology and current
systems? How s ignifi cant is it in hea ting the corona
and accele rating the solar wind?
Whe re do the observed variations in the SunΥs EUV
2, 3, 4
spectral ir radiance aris e, and ho w do th ey relate to the
magne tic activit y cy cles?
Wha t magne tic field conf igurations lead to the CMEs, 2, 3
filament eruptions , and flares that produce energ etic
particles and radiation?
Can the structure and dyna mi cs of the solar wind nea r 2, 3
Earth be determined from the magne tic field
configur ation and atmosphe ric structure nea r the sola r
surface?
When will activit y occur, and is it possible to make
2, 3, 4 (1 is second ary)
accura te and relia ble forecasts of space wea ther and
clim
ate?
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Instrument
EVE, HMI,
SHAR PP
EVE, HMI,
SHAR PP
EVE, HMI,
SHAR PP
EVE,
SHAR PP,
HMI
HMI,
SHAR PP
HMI: Doppergrams,
Londitudinal and Vector
Magnetic Field Images
EVE: Spectral Irradiance
Measurements
SHARPP: Atmospheric and
Coronagraphic Images
HMI,
SHAR PP
EVE, HMI
SHAR PP,
Page 12
To meet the Science Measurement Objectives for Full Mission Success,
the following Measurement Requirements must be performed by SDO:
Spectral Irradiance Measurements in the .1 to 105 nm range and continuum emission, at a cadence of
no slower than 20 seconds, for input to ionospheric and upper atmospheric models important for the
LWS Program. At least 18 emission lines at a spectral resolution of 0.1 nm. The absolute accuracy of
these emissions should be 25% or better for the duration of the prime mission. These 18 emission
lines shall be chosen to adequately characterize the solar EUV spectrum variations for LWS/Geospace
applications. EVE
Dopplergrams. Full-disk, 1.5-arcsec resolution photospheric velocity measurements every 50 seconds
with an accuracy of TBD m/sec. More than 95% of the dopplergrams must be recovered, with 99.99%
data completeness. HMI
Longitudinal Magnetograms. Full-disk, 1.5-arcsec resolution longitudinal magnetic field images every
50 seconds. Measurement of these features requires a noise level of 17 Gauss (G) with a dynamic
range of +-3 kG. HMI
Vector photospheric magnetic field observations over the whole disk with 1.5-arcsec resolution every
10 minutes with a polarization accuracy of .3%. HMI
Atmospheric Images. Full-disk 1.32-arcsec resolution images of the solar atmosphere in seven
wavelengths spanning the temperature range 20,000 to 3 million Kelvin (K) with a cadence of one set
every 10 seconds. Intercalibration of intensity between the images to ~20%. Field of view in
appropriate temperature regimes should extend to 1.35 solar radii to facilitate linkage with white-light
coronagraph (see below) observations. SHARPP
White light coronagraphic polarization and brightness images with a time cadence of 60 seconds per
sequence, with a pixel size of 15 arcseconds in the range 2 to 15 solar radii and an accuracy of 10%.
SHARPP
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 13
Defining the Minimum Mission
Instrument Science Objective
Science Quest ion
E- E- E- E- H- H- H- H- H- S- S- S- S- S- S- S- S- S- S1 2 3 4 1 2 3 4 5 1 2 3 4 5 6 7a 7b 8 9
What mechanisms drive the quasi-periodic 11-year
cycle of solar activity?
S
How is act ive region magnetic flux synt hesized,
concent rated, and dispersed across t he solar
surface?
S
How does magnet ic reconnection on small scales
reorganize the large-scale field topology and
current systems? How significant is it in heat ing
the corona and accelerat ing the solar wind?
S
Where do the observed variations in t he SunΥs
EUV spectral irradiance arise, and how do they
relate to the magnet ic activity cycles?
X
X
X
X
X
What magnet ic field configurat ions lead t o t he
CMEs, filament erupt ions, and flares that produce
energet ic particles and radiat ion?
S
X
Can the structure and dynamics of the solar wind
near Eart h be determined from the magnet ic field
configuration and at mospheric struct ure near the
solar surface?
S
S
X
X
X
S
X
S
X
X
X
When will act ivity occur, and is it possible to make
accurate and reliable forecasts of space weather
and climate?
X
X
X
S
X
X
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
S
X
S
S
X
X
S
S
X
X
X
X
X
S
S
X
X
X
S
X X
X
X
X
X
X
X
X
S
S
X
S
X
X
X
S
The table
indicates that
most of the
Science
Questions can be
addressed in the
event of a single
instrument failure.
Page 14
A-2.1.1.1
FULL MISSION SUCCESS CRITERIA
The following measurements shall be obtained over the prime mission life of five
years to obtain full mission success:
All three investigations operating 80% of the time over the course of 5 years.
Instrument performance commensurate with the Science Instrument Full
Performance Requirements.
A-2.1.1.2
MINIMUM MISSION SUCCESS CRITERIA
Tables A-1 and A-2 indicate that most of the Science Goals of SDO can be
addressed in the event of an instrument failure. Therefore, the minimum success
criteria for the SDO are as follows:
Two out of the three investigations operating 40% over the course of 5 years.
Instrument performance commensurate with the Science Instrument Minimum
Performance Requirements.
SDO System Requirements Review/System Concept Review (SRR/SCR) – April 8-10, 2003
Page 15
SDO PROJECT STATUS
Project
JAN FEB MAR
Ground System
JAN FEB MAR
Science Team
Ground Network
System Engineering
Data Distribution
S/C Subsystems
Mission Ops. & MOC
Launch Services
SOCs
Procurement
Summary Assessment
Technical Cost Schedule Management
Cost
Spacecraft
Schedule
Y
Instrument
Manpower
Ground System
Instrument
JAN FEB MAR
HMI
Y
Y
Y
SHARPP
Y
Y
Y
EVE
Launch Vehicle
LEGEND
GOOD SHAPE
Y
MINOR PROBLEM
R
MAJOR PROBLEM
16
SIGNIFICANT EVENTS
•
•
•
•
•
Successfully completed EVE, HMI, & SHARPP Instrument Systems Requirements
Retreats.
Completed all necessary draft documentation (37 items) & 2 weeks of dry-runs in
preparation for the SRR/SCR (1st external review).
Successfully conducted SRR/SCR.
–
2.5 days, 940 pages, 46 items of documentation available (hard copy & electronic) for review.
–
Also conducted (1/2 day) Project Management splinter (WBS, cost/schedule estimates, make/buy,
dependencies/agreements, project controls, information mgmt., risk mgmt., E&PO).
HQ’s considering adding another small instrument(s) to SDO mission
–
DORADE (Davos Observatory RADiometer Experiment), which is a pair of radiometers for total
solar irradiance measurement. HQ trying to work a no cost deal with ESA/Swiss.
–
HQ’s also trying to sell excess EELV capability (approx. 700 kg) or partner with another agency to
offset costs.
Working POP 03-1 exercises.
–
Do not descope science or the mission at this time.
–
Determine phasing for 4/08 launch in order to support a possible L.V. partnership with DOD.
–
Stay in-guide for FY04 & FY05 and determine launch date & new total.
17
SDO CRITICAL MILESTONE CHART
Critical Milestone
1.
Internal System Requirements Retreat
2.
Instrument System Requirements Reviews
(SRR) Complete @ Instrument Facilities
3.
External SRR/Systems Concept Review
(no earlier than)
4.
Initial Confirmation Review (no earlier than)
5.
Mission Preliminary Design Review
Jan Feb Mar Apr May Jun Jul
Aug Sep Oct Nov Dec
1 2/10
1 3/20
1 2
4/8
5/30
1
(no earlier than)
12/12
6.
7.
8.
Explanation of Missed Milestones:
5
Completed grassroots schedule estimates. Additional time to PDR required, still 6 months contingency
to 8/07 launch.
18
SDO Project Summary Schedule
‘99
CY 2000
Q4
Q1 Q2 Q3 Q4
CY 2001
Q1 Q2 Q3 Q4
CY 2002
CY 2003
CY 2004
Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4 Q1 Q2 Q3 Q4
Pre-Form
CY 2005
CY 2006
CY 2007
CY 2008
Q1 Q2 Q3 Q4
Q1 Q2 Q3 Q4
Q1 Q2 Q3 Q4
Q1 Q2 Q3 Q4
Formulation
Phase C/D
Implementation
Ops
(5 Yrs B/L)
Phase A Phase B
4/03 5/03 12/03 1stQ
3rdQ
9/06
5/07 8/07
CDR
PER
PSR
MISSION MILESTONES
LAUNCH
SRR/ ICR
SCR
INSTRUMENT DEVELOPMENT
PDR CR
AO Rel
1/02 Inst. Selections
8/02
Phased del.
2/06–4/06 7/06
Ship
Procure
Build/Test
Concepts/Design/Long Lead
AO Process
3 mo.s
9/02
Award Contracts
SPACECRAFT DEVELOPMENT
6/05
In-House ATP
Procure
Build Comp.s
S/C Bus Studies
Integration of
Instruments,
3 mo.s
2/06
S/C Int.
5 mo.s
Concepts/Design/Long Lead
4/07
10/06
OBSERVATORY ENVIRONMENTAL TEST
3/05
GROUND SYSTEMS DEVELOPMENT
I&T Rel.
Obs Env.
(6 mo.s) 2.5 mo.s
2/06
Ops. Rel.
3/07
Procure
Concepts/Design
LAUNCH VEHICLE DEVELOPMENT
Freeze
Procure/Develop/Test
Facilities Ready
Contract
Award
6 mo.s
6/06
LV Development/Integration (36 mo.s)
2 wks
8/07
8/04
K. O. Schwer
April 3, 2003
Legend:
or
End of the Month
Milestone
Ship
6/07
Progress Bar
Reserve
(6 months)
Launch
19