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The ESA Science Programme: Status of Solar and Solar Terrestrial Missions and other initiatives of interest for Space Weather
Hermann J. Opgenoorth
ESA – ESTECSolar and Solar Terrestrial Missions Division (SCI-SH)Research and Scientific Support Department (RSSD)
SOHO CLUSTER
XMM NEWTON
HERSCHEL
INTEGRAL
ULYSSESHUYGENS ISO HST CLUSTER II
MARSEXPRESS
XEUS
SMART 1
IRSIDARWIN
GAIA LISA
JWST
SOLARORBITER
F 2VENUSEXPRESS* PLANCK
BEPI COLOMBO
ROSETTA
LTP
Tim
e →
Mandatory Programme DisciplineProspects
M3
Ulysses
Joint ESA-NASA Mission The Heliosphere in 4-D : Spatial 3-D and Time
Earlier anticipated end of Mission: 30. Sept. 2004
Recent ESA-SPC decision to extend the scientific operations by 3.5 years - March 2008: allowing third polar pass
Now discussed in NASA Advisory Structure Senior Review in 2005 - (under threat from recent NASA MO&DA cuts…)
Key Scientific Goals in the Context of Extension:Key Scientific Goals in the Context of Extension:- Energetic particle and dust dynamics: effect ofEnergetic particle and dust dynamics: effect of reversed field polarity on latitude dependencereversed field polarity on latitude dependence- Reconfirm the north-south heliospheric asymmetryReconfirm the north-south heliospheric asymmetry- 3-D structure of CMEs and heliospheric current3-D structure of CMEs and heliospheric current sheet in conjunction with ecliptic S/C like STEREOsheet in conjunction with ecliptic S/C like STEREO
SOHO: Solar Cornerstone Mission
Presently THE Solar Observatory:ESA / NASA Collaboration since 1995Currently 4 year mission extension 2003-2007 Future extension(2007-2009) proposal in 2006 Also s c ”SOHO Bonus Mission” discussed to provide Coronagraph to International Living With a Star - ILWS
Cluster:ESA’s Magnetospheric Cornerstone Mission
Earlier ESA-SPC decision : Earlier ESA-SPC decision : 100 % orbital data coverage 100 % orbital data coverage and 3 yr mission extension: and 3 yr mission extension: 2003 - 20052003 - 2005 Second extension for 2+2 years until December 2009 decided in Febr. 2005 SPCNow at largest separation
• First 3-D satellite mission ever
• ESA - NASA Collaboration
- since 2000
Solar wind
Cluster new regions: subsolar point and auroral accelerationCluster new regions: subsolar point and auroral acceleration
2001
2009
Magnetopause:Subsolar point
Cluster Extension
Double Star – Cluster: Evolution of Reconnection
Strong flow of plasma observed first atDouble Star and 5 min later at Cluster
DSP
Cluster
From Pitout et al., 2005
Cluster Extension
Solar wind
• Crossing of tail at 8-10
Earth radii
• Current Disruption: key
process for substorms
Cluster at new region: Near-Earth Current DisruptionCluster at new region: Near-Earth Current Disruption
Near-Earth tail:Current Disruption
2001
2009
Cluster Extension
Complementarity of Themis and Cluster• THEMIS will be launched in 2006 with 1st tail season in February 2007
THEMIS’s tail science benefits from Cluster’s Solar Wind and ionospheric monitoring and half a year later
Cluster tail science benefits from THEMIS’s upstream, sheath and magnetopause monitoring.In addition: vaste ground based network in Canada and Europe for Cluster / Themis
•From V. Angelopoulos, Berkeley, USA
Cluster
Themis
Cluster Extension
DOUBLE STAR China / ESA Collaboration
Two satellites equipped mainly with Cluster Spare Instruments in Magnetospheric Polar and Equatorial orbits DSP-E: 550 km x 9 Re & DSP-P: 350 km x 4 R
• Commissioning Phase completed - ok, except attitude control• Excellent science results - in particular in coord. with Cluster • 1.5 yrs mission extension recently decided (May 2005 SPC)
Double Star
Extension summer 2005: Tail
• Cluster: 14-16 Re sep.1000-10000 km
• DSP TC-1: 9 Re apog. above equator
• DSP TC-2: 7 Re apogee in tail
09 Sept. 2005, 16:00 UT
5 Re
<== Observe NENL and/or Bursty Bulk Flow at Cluster and then
monitor Current Disruption and BBF breaking at DSP
==> Observe Current Disruption at DSP and then
outgoing “rarefaction-wave” at Cluster.
XY
XZ
Double Star
Extension summer 2006: Tail
• Cluster: 14-16 Re sep 1000-10000km
• DSP TC-1: 9 Re gradual sep. in Y
• DSP TC-2: apogee in southern hemisphereXZ plane
XY plane
TC-1
11 Sept 2006 00:00
=> Observe the azimuthal extent and dynamics of current disruption
Double Star
Cluster
DSP TC-1
DSP TC-2
• Cluster at northern
magnetopause/cusp
10000 km separation• TC-1 near the cusp• TC-2 at southern cusp
and in inner magneto-
sphere on dayside
Extended mission spring 2006: Cusp
XZXY
Double Star
• DSP TC-2 and IMAGE both in the southern hemisphere
• “Stereo” ENA images of the ring current from the southern hemisphere
• Observations require geomagnetic storms
22 Dec 2005, 00 UT
TC-2
IMAGE
Extended mission : winter 2005
Solar Orbiter ESA-ILWS Flagship in the long term
• Selected as ESA Flexi-mission • launched within 10 yrs - lifetime 5 + 2 yrs• confirmed as part of ”COSMIC VISION”
• Formal negotiations about a potential NASA contribution ( or collaboration with Solar Sentinels ) in progress…
- Inner Heliosphere In-Situ observations and simultaneous Solar Remote Sensing
- Orbit up to 35 deg out of the ecliptic, i.e. topside view of polar regions and CME’s
- observe the far-side of the Sun from a co-rotating vantage point at 0.22 AU, equivalent to 48 Solar radii…
Solar Orbiter Status
(Confirmed as part of Cosmic Vision by SPC, June 2004)
Mission profile: • Launch by Soyuz-Fregat 2-1b (either Oct 2013 or March 2015)• Cruise phase (SEP / Chemical Propulsion): 1.8 / 3.3 yrs• Nominal science mission duration: 2.8 yrs• Extended mission (high-latitude phase): 2.4 yrs• Minimum perihelion distance: 48 solar radii (0.222 AU)• Maximum solar latitude: 35° (in extended phase)SPACECRAFT – two industrial studies completed (Sci-A)
– 6 month delta-study (chem. prop.) completed
PAYLOAD – definition completed Particles and Fields Package Remote-sensing Package
PLAN : Science Management Plan to SPC in February 2006- coordinated AO with NASA (Solar Sentinels) Summer 2006
S-O Mission duration and solar cycle SEP vs. Ballistic Mission
0
20
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2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 2021 2022 2023 2024 2025 2026 2027
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Ballistic 2012
SEP 2013
Ballistic 2013
Ballistic 2015
The Solar-B satellite
• JAXA successor to Yohkoh (Solar A)
• Japan/US/UK mission (Norway, ESA)
• Launch in Aug. 2006 aboard M-V rocket from Uchinoura Space Centre (USC)
• Polar sun-synchronous orbit. 600 km altitude
– Nearly continuous solar view (with no day/night cycling for nine months each year)
• A coordinated set of optical, UV, and X-ray instruments to understand the dynamic Sun.
• Mass: 900 kg • Power: 1000W• Telemetry: 4Mbps • Data Recorder: 8Gbit• Attitude: Solar pointed• Stability: 0.7 arcsec/1s• Launch: Summer 2006
Solar-B Science Goals - Understanding the Dynamic Sun
• To understand the creation and destruction of the Sun's magnetic field.
• To understand the modulation of the Sun's Luminosity.
• To understand the generation of UV and X-ray radiation.
• To understand solar wind and eruptions.
• Provide the first accurate measurements of magnetic fields and electric currents that will reveal the causes of eruptions in the solar atmosphere
Solar-BThe 3 Instrument Suite
• 0.5m Optical Telescope +FPP (Focal Plane Package)– Spectro-Polarimeter– Broadband Filtergraph– Narrowband Filtergraph
• XRT (X-Ray Telescope)– 9 filters: hot-very hot corona
• EIS (EUV Imaging Spectrograph)– 2x40 Å wide wavelength – region in EUV covering
transition region - corona
ESA Support to Solar-B
• ESA, in sub-contractual collaboration with the Norwegian
Space Centre, will provide one additional downlink contact
to Solar-B for each of the 15 orbits per day
• This will considerably improve the overall scientific data return
and the cadence of observations from the Solar-B mission
• The European scientific community
will be catered with processed data
through a dedicated Solar B data
centre at the University of Oslo
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
• Reasons: Antenna redundancy, possibility to track all 15 orbits every day and Norwegian interest in the mission.
Svalbard Ground Station for Solar-B
International Living with a Star - ILWS (presently involving more than 25 space agencies SC: CNSA, CSA, ESA, (R)FSA, JAXA, NASA )
Stimulate, strengthen and coordinate space researchto understand the governing processes of the connected Sun-Earth system as an integrated entity. (governing processes = ”which affect life and society” => SpaceWeather)
simultaneous and coordinated observations at strategic locations in the entire system
(supported by advanced analysis and model tools)
MISSION:
Earth’s Interior - Baseline mission
Earth’s Environment“One man’s noise is another man’s data”
SWARM Mission Living Planet ESA - EOP
Selected by Earth Observation Program Board - Launch 2009
Electric Field Instrument (Ion Drift Meter) provided by CSA in collaboration with ESA Science Programme
Optimisation of GEOSPACE science - additional electroninstrument “Conducto-meter”discussed…
L1 ＋ polar trip-star project
New KuaFu - New KuaFu - selected for Phase Bselected for Phase BSolar Storm, Aurora and Space Weather Exploration Solar Storm, Aurora and Space Weather Exploration
Launch Date: 2012
Pre-study supported by the National NSF of China
KuaFu-A at L1 Solar EUV emission White light CME Radio wave measurement local plasma and magnetic field High energy particles
KuaFu-B1+B2 polar orbit
24 hours Aurora Image Apogee + Perig. Magnetic field High energy particles
Solar Wind, Aurora and Storms exploration (SWASE) - recently de-selected
Near-Earth SolarWind Monitor
Aurora Monitor
Magnetosphere Monitor
Ionosphere & Thermosphere Monitor
Proposed by: Professor Z.X.Liu of CSSAR, Chinese Academy of Sciences (elements of SWASE will be added to “New KuaFu”)
ESA’s Cosmic Vision, 2015-2025
Themes:1. What are the conditions for life and planetary formation?2. How does the Solar System work?
1. From the Sun to the edge of the Solar System“First, the hierarchy of scales in the magnetosphere (e.g. M3,
Magnetospheric SWARM)”
2. Gaseous Giants and their Moons3. The Building Blocks of the Solar System: Asteroids and Small Bodies
3. What are the fundamental laws of the Universe?4. How did the Universe originate and what is it made of?
Giovanni Bignami, chairman SSAC, 10 May 2005
Three scales of plasmas – shocks as an example
Orientation, motion, curvature,
foreshock
Shock
Ion reflection, reformation,
thermalisation, downstream waves
Electron reflection, acceleration, electric
fields
Cross-Scale – key conceptsCross-Scale – key concepts Spacecraft on a hierarchy of scales
Electron group Electron instruments 3 axis electric and magnetic fields
Ion group Fast ion instruments Magnetic field instruments
Fluid group Bulk plasma and field instruments Energetic particles
Note Need different instrumentation at each scale Other agencies could provide one or more scales
Cross-Scale - The ESA context
• Cosmic Vision 2015-2025
• Relative to other CV mission concepts, Cross-Scale is:– Cheap: <€300M, baseline of single Soyuz-Fregat launch– Quick: early in programme - by 2015?– Easy: no technological show-stoppers
• Potential for international collaboration: JAXA– SCOPE: 5-s/c mission for cross-scale plasma dynamics– Led by M. Fujimoto ISAS
First inter-agency discussions at two ESA /JAXA Bilaterals
European ILWS Strategy in an Overview
Major ESA Support
or ESA – ledModest ESA Support
Strong ESA/SCI endorsement
1 Sun and Solar Wind
Energy Source
Soho & Ulysses ext.
Solar Orbiter
BC–MMO SolarSent.
Solar – B grnd. stat.
Coronagraph
Stereo grnd. stat
L1 mission(s)> KuaFu
Solar - ISS
Proba - 2
2a Ionosphere -
Thermosphere
Energy depositionSwarm
To be identified
Demeter
Ravens -> KuaFu
2b Magnetosphere
Energy conversion
Cluster / DSP extension
M 3 development
NLM’s
candidates tbi
Orbitals
Frisbee
National Multi-Sats
3 Sun and Climate
End-to-End Observ. _ TSI M of Opp / C-Ph
Picard & Earthshine _
4 Data Exploitation,
Analysis & Models
Cluster Active Archive (CAA)
SDO DB or EN-SVO
Stereo / Solar–B GrSt
Model and Theory
Space Weather / GB
SCOPE – the Japanese connectionSCOPE – the Japanese connection
Proposed ISAS five-spacecraft mission
Focus on electron dynamics at shocks and reconnection sites
Potential for incorporating SCOPE as the inner scale of Cross-Scale
This is only one possible scenario!
Double Star
From Cornilleau et al., 2005
Cluster
DSP-TC-1
Magnetopause EXAMPLE :
M-Pause crossing
on Febr. 22, 2004TC1: 19:30 UT sub-solar
Cluster: 20:10 UT high lat.
=> Delta t = 40 min
[Crossings so far:
21 within 1 hour and
only 4 within 15 mins]
Double Star
From Cornilleau et al., 2005
10 times higher wave power at subsolar MP as compared to high latitude MP ==> Reconnection more likely at subsolar MP ?
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