1. Linking in-situ measurements with SPICE
Giulio Del Zanna
Helen Mason
DAMTP, CMS, University of Cambridge
G. Del Zanna - Solar Orbiter meeting 2012

2. SPICE EUV Spectrometer
Heritage: SOHO SUMER,CDS; Hinode EIS
704 – 790, A 1st order
Line intensities, Doppler velocities (3 km/s), line widths.
Electron temperatures, densities,
chemical abundances.
Complete temperature coverage from chromosphere to flaring corona
About 1”/ pixel (175 km at perihelion – Hi-C !)
Four slits: 2’’x14’, 4’’x14’, 6”x14”, 30’’x14’.
Maximum raster area: 16’x14’
Exposure times: from seconds
ESA is the lead funding agency. Contributions from Germany, France, Norway, Switzerland and United Kingdom. Instrument development led by the Rutherford Appleton Laboratory (Consortium Lead – Andrzej Fludra)
For details, see poster:
Fludra et al: SPICE EUV Spectrometer for Solar Orbiter
G. Del Zanna - Solar Orbiter meeting 2012

3. SPICE science questions
How and where do the solar wind plasma (fast and slow) and magnetic field originate in the corona?
What are the source regions of energetic particles?
How is the structure of ICMEs related to their origin?
“Critical new advances will be achieved by flying a spacecraft combining remote and in-situ observations into the inner solar system.”
How close ?
(C.N.Rizzi)
G. Del Zanna - Solar Orbiter meeting 2012

4. In-situ v, T, el. abundances
FIP effect
Freezing-in T
R. Von Steiger
+ distribution functions, magnetic field at source & in-situ
Can we relate them to the SPICE measurements during near-corotation ?
G. Del Zanna - Solar Orbiter meeting 2012

5. Science questions SPICE can address
1) Origin of the slow solar wind. At the coronal hole boundary?
2) Origin of the fast solar wind. From the interplume regions?
3) Do active regions contribute to the solar wind?
Long-lasting open field regions associated with
1) coronal holes
2) coronal outflows in Active Regions
By extrapolating B, measure (SPICE) Te (Mg IX); Doppler-shifts, line broadenings; FIP effect (e.g. Mg/Ne), we can link SPICE/EUI to in-situ measurements.
G. Del Zanna - Solar Orbiter meeting 2012

6. CH plumes/jets contributions to the fast solar wind?
Plumes are extended structures in open-field regions. Helios pressure-balance structures?
plumes (Del Zanna 1999)
Hassler et al. (1999)
(DeForest et al. 2001)
CH will be prominent during the first phase of the mission.
Plumes are cooler and denser (Del Zanna+1999), will have bright emission in SPICE lines (0.8 MK). They have a very small FIP bias (Del Zanna 1999, +2001,+2003).
CH (and QS) network and cell-centres show FIP effect (Del Zanna & Bromage 1999), with the lowest Mg/Ne abundance in the CH network.
G. Del Zanna - Solar Orbiter meeting 2012

7. Active region coronal outflows (Hinode/EIS)
Visible only in lines with Te> 1MK.
Located in the middle of sunspots and plage (not all plage regions have blueshifts !).
Spatially concentrated lower down but have a large spatial expansion.
Long-lasting, and follow the magnetic field emergence. (Del Zanna 2007,2008)
G. Del Zanna - Solar Orbiter meeting 2012

8. AR contribution to the solar wind
Del Zanna, Aulanier Klein & Torok (2011,A&A)
Interchange reconnection close to the null point. Upflows driven by a rarefaction wave (see hydrodynamic modelling in Bradshaw, Aulanier & Del Zanna, 2011).
A fraction of the outflowing plasma contributes mass and momentum into the solar wind.
Solar orbiter observations are needed to confirm this scenario.
G. Del Zanna - Solar Orbiter meeting 2012

9. G. Del Zanna - Solar Orbiter meeting 2012
Due to telemetry limits, most studies will record only a few selected line profiles.
Need for careful planning ! See SPICE posters: 1) Andretta et al., 2) Teriaca et al.
G. Del Zanna - Solar Orbiter meeting 2012

10. SOHO CDS NIS: first EUV calibrated radiances along a cycle
He I
O IV (0.25 MK)
Mg X (1 MK)
Fe XVI (2-3 MK)
Are used for the SPICE count rates modeling.
Del Zanna et al. (2010, A&A)
Del Zanna & Andretta (2011, A&A)
G. Del Zanna - Solar Orbiter meeting 2012

11. G(T) of main SPICE lines
CHIANTI v.7
G. Del Zanna - Solar Orbiter meeting 2012

12. Measuring Te with Mg IX One of the best Te diagnostic for 1 MK plasma.
Large discrepancies between observed and calculated radiances were resolved with the first atomic calculations (Del Zanna et al. 2008).
SOHO/GIS off-limb Del Zanna (1999)
2p2 1D 2
749.5 A
2s 2p 1P 1
2s 2p 3P 1
706 A
2s2 1So
G. Del Zanna - Solar Orbiter meeting 2012

13. Te in coronal holes Temperatures with the new atomic model are higher.
E.g. an inter-plume Te= at 1.3R revised to K (Del Zanna+2008)
Mg IX 706
Mg IX 749
SUMER (2006) ‘New’ Te obtained including photoexcitation and density effects. (Del Zanna, Wilhelm, Teriaca, in prep.)
G. Del Zanna - Solar Orbiter meeting 2012

14. SPICE lines for on-disk abundance studies
CHIANTI
Mg VIII, Ne VIII
Fe VIII (?), Ar VIII
Obtaining abundances is not straightforward. Several lines will need to be observed.
G. Del Zanna - Solar Orbiter meeting 2012

15. Laboratory Astrophysics
ASTRONET: laboratory astrophysics should be an integral part of the R&D of new missions.
After 8 years, atomic data and line identifications for Hinode EIS are nearly complete but not finished ! Accuracy and completeness of the atomic data for SPICE need to be assesed.
Atomic data calculations APAP Network
Atomic data benchmarking and line identifications (Del Zanna)
Atomic data provision – CHIANTI
G. Del Zanna - Solar Orbiter meeting 2012

16. G. Del Zanna - Solar Orbiter meeting 2012
Conclusion
We will need to identify the best SPICE diagnostic lines and operating modes (e.g. spatial resolution), depending on the science. Contributions form the community are needed.
We will need to coordinate with other instruments and missions.
Good chance to link in-situ measurements with remote-sensing and address some of the main Solar Orbiter science questions.
G. Del Zanna - Solar Orbiter meeting 2012

17. G. Del Zanna - Solar Orbiter meeting 2012
EXTRA SLIDES
G. Del Zanna - Solar Orbiter meeting 2012

18. Te in coronal holes Temperatures with the new atomic model are higher.
E.g. an inter-plume Te= at 1.3R revised to K (Del Zanna+2008)
Mg IX 706
Mg IX 749
new
SUMER (2006) ‘New’ Te obtained including photoexcitation and (small) density effects. (Del Zanna, Teriaca, Wilhelm)
old
G. Del Zanna - Solar Orbiter meeting 2012

19. Elemental abundances with SPICE
Incorrect abundances (by a factor of 10) can be obtained
Skylab plume
Te of maximum emissivity in ionization equilibrium
Actual Te
FIP=0
FIP=10
Widing & Feldman (1992)
Del Zanna et al. (2003)
G. Del Zanna - Solar Orbiter meeting 2012

20. G. Del Zanna - Solar Orbiter meeting 2012
Mg IX on-disk
Is the line usable or blended (with what ?) ?
On-disk (Curdt et al. 2001): black: QS red:Sunspot; blue:CH
Ca III (no) O II? (Edlen 1933) unlikely C V (no) Ni III (no) Si IV (Edlen 1963, Toresson 1960) 3d-5f weak transitions.
G. Del Zanna - Solar Orbiter meeting 2012

21. Elemental abundances and FIP
The variability in abundances in the SW can be used as a proxy to identify source regions, combining remote-sensing with in-situ
G. Del Zanna - Solar Orbiter meeting 2012
Del Zanna & Mason (2012)

22. G. Del Zanna - Solar Orbiter meeting 2012
Coronal outflows
(Del Zanna 2007,2008)
Visible only in lines with Te> 1MK.
Located exactly in the middle of sunspots and plage (not all plage regions have blueshifts !).
Spatially concentrated lower down but have a large spatial expansion.
Long-lasting, and follow the magnetic field emergence.
G. Del Zanna - Solar Orbiter meeting 2012

23. off-limb contribution
G. Del Zanna - Solar Orbiter meeting 2012

24. Simulations for METIS
Off-limb He II observations are strongly contaminated by Si XI. Modeling depends strongly on Te
G. Del Zanna - Solar Orbiter meeting 2012
Andretta, Telloni Del Zanna (2012)

25. G. Del Zanna - Solar Orbiter meeting 2012
Low-FIP low-Te lines
Fe VIII ?
Fe VIII Ekberg & Feldman (2003), but intensity is brighter than expected !
G. Del Zanna - Solar Orbiter meeting 2012

26. G. Del Zanna - Solar Orbiter meeting 2012

27. G. Del Zanna - Solar Orbiter meeting 2012
Mg IX
G. Del Zanna - Solar Orbiter meeting 2012

28. Benchmarking the atomic data - SOHO GIS
Del Zanna ( PhD thesis)
SOHO
Grazing Incidence Spectrometer
Off-limb spectrum
Excellent agreement with QS data.
With new atomic data, Te in lane at 1.3 Ro from K (Wilhelm et al. 1998) revised to K (Del Zanna et al. 2008).
G. Del Zanna - Solar Orbiter meeting 2012

29. Benchmark with SOHO SUMER off-limb QS
Isothermal plasma at
T=1.35 MK (Feldman et al. 1999)
Excellent agreement with the results from
the first R-matrix calculation for Be-like Mg (Del Zanna Rozum Badnell 2008).
G. Del Zanna - Solar Orbiter meeting 2012

30. G. Del Zanna - Solar Orbiter meeting 2012
Te from Mg IX - SUMER
G. Del Zanna - Solar Orbiter meeting 2012