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Supporting stellar research by observing the sun
Dan Kiselman
Centrum/avdelning/enhet... Astronomy Department National infrastructure
2012
Host university
Supporting stellar research by observing the sun Dan Kiselman - - PowerPoint PPT Presentation
Supporting stellar research by observing the sun Dan Kiselman - - PowerPoint PPT Presentation
Supporting stellar research by observing the sun Dan Kiselman Host university 2012 National infrastructure Centrum/avdelning/enhet... Astronomy Department IAC SST 0.97 m vacuum Schupmann refractor Adaptive optics CRisp Imaging
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SST 0.97 m vacuum Schupmann refractor Adaptive optics CRisp Imaging Spectro-Polarimeter (CRISP) TRIPPEL spectrograph
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TRIPPEL Spectrograph
Tri-Port Polarimetric Echelle Littrow Grating, Slit R ∼200000 3800 – 10800 Å (in principle) λ window 10-15 Å Prefilter needed!
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SST/TRIPPEL
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SST/TRIPPEL: one CCD row
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CRISP = CRisp Imaging Spectro-Polarimeter
- Double FPI
- λ = 5100 Å – 8600 Å
- R = 225000 ...... 70000
- Prefilters: Mg I 5173,
Fe I 5250, C I 5380, Fe I 5576, Na I 5896, Fe I 6173, Fe I 6302, Hα 6563, O I 7773, Ca II 8542
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
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Scanning through Fe I 6301.5 Å with CRISP Stokes I
One million spectra!
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SST/CRISP: Three sample spectra from the scan just showed.
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SST/CRISP Equivalent width of Fe I 6301.5 Å
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What does the sun offer?
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What does the sun offer?
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What does the sun offer?
A fantastic and colourful lab for radiation+ magnetic fields+ hydrodynamics + ...!
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The Rosetta Stone!
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Simulation
SST
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van Noort & Rouppe van der Voort 2005
The Chromosphere, SST H-α
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Solar Dynamics Observatory: Flare
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The sun offers diversity to test your spectral diagnostics.
- Centre-to-limb variation
- Granulation
- Latitude
- Activity
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Centre-to-limb variation calibrates O+H inelastic collisions SST/TRIPPEL: Pereira, Asplund, Kiselman 2009 What is the importance of atomic excitation by collisions with neutral hydrogen?
8.68
What is the solar oxygen abundance?
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537.95 538.00 538.05 538.10 0.2 0.4 0.6 0.8 1.0
C I 538.03 nm
616.00 616.05 616.10 616.15
Na I 616.08 nm
616.45 616.50 616.55 616.60
Fe I 616.54 nm
616.55 616.60 616.65 616.70
Ca I 616.64 nm
616.85 616.90 616.95
Ca I 616.90 nm
711.05 711.10 711.15 711.20 0.2 0.4 0.6 0.8 1.0
C I 711.14 nm
711.25 711.30 711.35 711.40
C I 711.32 nm
768.55 768.60 768.65 768.70
S I 768.61 nm
769.85 769.90 769.95
K I 769.90 nm
777.10 777.15 777.20 777.25
O I 777.19 nm
777.35 777.40 777.45 777.50 Wavelength [nm] 0.2 0.4 0.6 0.8 1.0
O I 777.41 nm
777.45 777.50 777.55 777.60 Wavelength [nm]
O I 777.53 nm
783.50 783.55 783.60 783.65 Wavelength [nm]
Al I 783.53 nm
783.50 783.55 783.60 783.65 Wavelength [nm]
Al I 783.61 nm
869.40 869.45 869.50 869.55 Wavelength [nm]
Si I 869.46 nm
BG: the sun’s abundance pattern is subtly different from that of solar twins. Is the solar spectrum latitude dependent? SST/TRIPPEL: Kiselman, Pereira Gustafsson, et al. 2011
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711.28 711.30 711.32 711.34 711.36 Wavelength [nm] 0.90 0.92 0.94 0.96 0.98 1.00
C I Observe at constant distance from disk centre (μ=√2) but at different latitudes. Is the solar spectrum latitude dependent? Is the solar spectrum latitude dependent?
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Difference in abundance derived by a polar and an equatorial observer. Is the solar spectrum latitude dependent?
No!
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