• Science goals– We have collection of science cases with SOLAR-C (B).
Some of them are new based on sciences newly identified with
Hinode and GBO etc. recently.
But some of them are even “traditional”. It is also true that wecannot solve all the science problems with the existing
instruments.
– We can do lots of science using SOLAR-C.
– What are priorities of science goals in SOLAR-C?
• Some of them can be studied further by data analysis of existing instruments(SOHO, Hinode, and GBOs).
• Some of them can be studied by instruments coming near future (SDO, IRIS,GBOs).

– Unique science in SOLAR-C compared with Hinode, GBO, SDO,and IRIS.
– Synergies among the three instruments.

Mission-wide science goals(Shimizu)	

Mission-wide science goals(Katsukawa)	

HINODE SOT vs SOLAR-C SUVITHINODE SOT	SOLAR-C SUVIT	

320” x 160” (NFI,SP)
220” x 110” (BFI)	

200” x 200”	

Resolution	

0.2” – 0.3”	

(0.05”) 0.1” – 0.16”	

Sampling0.054”/pix (BFI)
0.08”/pix (NFI)
0.16”/pix (SP)	

~0.04” /pix (for filter imaging, low
S/N SP)~0.2”/pix (for high S/N SP)

Spectral coverage
Broad filter: R<10,000

Ca II H (398nm)
Continuums in 380-670nm

Mg II k/h (280nm)
Some continuums

Narrow filter:
R~70,000

Mg I b2, Na I D1, 3x Fe I, Hα(517 – 656 nm)

Ca II IRT, and other photo/chrom.
lines (500 – 870 nm)

Spectro-polarimeter:
R~200,000

Fe I (630nm)

Mg II k/h, Ca II, He I
(280nm, 850nm, 1083nm)# of photo-electrons
S/N~ 4e5/0.16”/sec/Δλ~103 with ~4sec exposure~1e7/0.1”/sec/Δλ~104 with ~10sec exposure

Average telemetry(total)~400kbps> 10Mbps

FOV	•

Sampling– Spatial sampling: 0.1"/pix– Temporal sampling: 1sec
– Wavelength sampling: λ/Δλ=2x105

SOLAR-C vs GBO(Lites)	

SOLAR-C vs GBO(Lites)	

Science targets with the diagnostics ofchromospheric magnetic ﬁelds

SOLAR-C	

MHD wave

Horizontal field
Flux tube

spicule	a	

Prominence formationand eruption

Penumbra micro-jets	
Solar cycle

Ellerman bomb, Jets	

Ground-based telescopes will
do a good job in the area. 	
(Katsukawa)	

Substantial jumps from IRIS?
• IRIS (Interface Region Imaging Spectrograph) isapproved for launch in 2012.
– Spectral lines in 120-280nm with 0.3” and 1-5s cadence to discover how
an outer stellar atmosphere is energized.
– The spectral lines observed with IRIS are suitable to explore theinterface between upper chromosphere and lower transition region.

• Still substantial jumps from IRIS, because the S-C plan-B
can provide unique observations which have never beenrealized:– Quantitative measurements of magnetic fields in the chromosphere– EUV/UV spectral lines used in Solar-C spectrometer will seamlessly
cover from chromospheric temperature through the coronal temperature
with 0.1-0.5” and 1-5 s cadence.
– Energy spectral (thermal and non-thermal) diagnostics in 106-107 K
plasma for flares and active region dynamics.

10 March 2010

SCSDM-2(Shimizu)	 910 March 2010

SCSDM-2

10••Strawman concepts of mission instruments were presented fromeach subWG. We’d appreciate any scientific and technicalcomments from outside of subWGs.
An obvious issue is in the spatial resolution– UV-Vis-NIR telescope• Is 0.05” resolution required?
– Requirements to optical designs (surface roughness etc.)– Requirements to the pointing stability– UV/EUV spectrograph• Is 0.2” resolution required?
– Require image stabilization system– Next generation X-ray imaging telescope• Is 0.2” resolution required?
– Impact to GI vs NI discussion•Resources– Technical feasibility– Community••

Numerical simulation to understand the complex solar atmosphere
Data analysis of specto-polarimetric data

Basic speciﬁcations of the three telescopes
Pixel size and FOV	UV-Vis-NIR telescope

UV/EUV imagingspectrometer
X-ray telescope

FOV

Pixel size

ExposureNote.

Broadband

164" x 164"0.04"< 1sec• 2.5 pix sampling of 0.1" res.
• 4Kx4K detector

Narrowband

246" x 246"

0.06"

< 1sec• 2.5 pix sampling of 0.16" res.
• 4Kx4K detector

Spectrometer246" x 246"

0.06"

1sec
(S/N~1600)• 2.5 pix sampling of 0.16" res.
• 4K pix along slit

0.12"

10sec
(S/N~104)

Spectrometer

1024"x 1024"

0.5"

0.5sec (AR)
5sec(QS)• 0.5"pixel size
• 2Kx2K MCP+CMOS detector

NIImaging

410"x410"

0.1"

1sec (AR)10sec (QS)

• High res imaging with NI telescope• 4Kx4K detector

GIImaging1024"x1024"

0.5"

1sec

Photon count1024"x1024"

2.0"

60sec

• Imaging spectroscopy with GI• 2Kx2K CMOS detector

Size 	
Size (mm)Weight (kg)UV-Vis-NIR telescope (telescope)

φ2300x4300

500

UV-Vis-NIR telescope (focal plane instruments)

2500x400x3000

200

UV/EUV imaging spectrometer	

400x800x4000

120

X-ray telescope	

400x400x4000

100