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 Spectro-Polarimeter (CRISP) TRIPPEL spectrograph

TRIPPEL Spectrograph Tri-Port Polarimetric Echelle Littrow Grating, Slit Prefilter needed! R ∼ 200000 3800 – 10800 Å (in principle) λ window 10-15 Å

SST/TRIPPEL

SST/TRIPPEL: one CCD row

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, H α 6563, O I 7773, Ca II 8542

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

Scanning through Fe I 6301.5 Å with CRISP Stokes I

One million spectra! Scanning through Fe I 6301.5 Å with CRISP Stokes I

SST/CRISP: Three sample spectra from the scan just showed.

SST/CRISP Equivalent width of Fe I 6301.5 Å

What does the sun offer?

What does the sun offer?

What does the sun offer? A fantastic and colourful lab for radiation+ magnetic fields+ hydrodynamics + ...!

The Rosetta Stone!

SST Simulation

The Chromosphere, SST H- α van Noort & Rouppe van der Voort 2005

Solar Dynamics Observatory: Flare

The sun offers diversity to test your spectral diagnostics. • Centre-to-limb variation • Granulation • Latitude • Activity

What is the importance of atomic excitation by collisions with neutral hydrogen? What is the solar oxygen abundance? SST/TRIPPEL: Pereira, Asplund, Kiselman 2009 Centre-to-limb variation calibrates O+H inelastic collisions 8.68

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 C I 538.03 nm Na I 616.08 nm Fe I 616.54 nm Ca I 616.64 nm Ca I 616.90 nm 1 . 0 0 . 8 0 . 6 0 . 4 0 . 2 537 . 95 538 . 00 538 . 05 538 . 10 616 . 00 616 . 05 616 . 10 616 . 15 616 . 45 616 . 50 616 . 55 616 . 60 616 . 55 616 . 60 616 . 65 616 . 70 616 . 85 616 . 90 616 . 95 C I 711.14 nm C I 711.32 nm S I 768.61 nm K I 769.90 nm O I 777.19 nm 1 . 0 0 . 8 0 . 6 0 . 4 0 . 2 711 . 05 711 . 10 711 . 15 711 . 20 711 . 25 711 . 30 711 . 35 711 . 40 768 . 55 768 . 60 768 . 65 768 . 70 769 . 85 769 . 90 769 . 95 777 . 10 777 . 15 777 . 20 777 . 25 O I 777.41 nm O I 777.53 nm Al I 783.53 nm Al I 783.61 nm Si I 869.46 nm 1 . 0 0 . 8 0 . 6 0 . 4 0 . 2 777 . 35 777 . 40 777 . 45 777 . 50 777 . 45 777 . 50 777 . 55 777 . 60 783 . 50 783 . 55 783 . 60 783 . 65 783 . 50 783 . 55 783 . 60 783 . 65 869 . 40 869 . 45 869 . 50 869 . 55 Wavelength [nm] Wavelength [nm] Wavelength [nm] Wavelength [nm] Wavelength [nm]

Is the solar spectrum latitude dependent? Is the solar spectrum latitude dependent? 1 . 00 0 . 98 0 . 96 0 . 94 C I 0 . 92 0 . 90 711 . 28 711 . 30 711 . 32 711 . 34 711 . 36 Wavelength [nm] Observe at constant distance from disk centre ( μ = √ 2) but at different latitudes.

Is the solar spectrum latitude dependent? No! Difference in abundance derived by a polar and an equatorial observer.

Interested in observing next year – talk to me soon. Interested in observing this year – talk to me today!