speaker: s. kamio solar seminar 2006.02.27
DESCRIPTION
DOT tomography of the solar atmosphere Leenaarts, J. and Wedenmeyer-B ö hm, S. 2005 A&A 431, 681 Comments on the optimization of high resolution Fabry-P é rot filtergraphs Sharmer, G. B. 2006 A&A 447, 1111. Speaker: S. Kamio Solar Seminar 2006.02.27. Dutch open telescope. - PowerPoint PPT PresentationTRANSCRIPT
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DOT tomography of the solar atmosphereLeenaarts, J. and Wedenmeyer-Böhm, S. 2005 A&A 431, 681
Comments on the optimization of high resolution Fabry-Pérot filtergraphsSharmer, G. B. 2006 A&A 447, 1111
Speaker: S. KamioSolar Seminar 2006.02.27
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Dutch open telescope
• 45cm diameter with open design• High resolution (0.2") image by Speckle reconstruction• Ongoing projects
BBSO/NST(1.6m), GREGOR(1.5m), ATST(4m), DOT++(1.4m)
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G-band image
• bright points in the intergranular lanesmagnetic flux
Movies available at http://dot.astro.uu.nl/(79" x 63")
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Reversed granulation
dark intergranular-lane (G-band) bright cell-boundary (Ca II H)
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Simulations
• CO5BOLD code(Wedenmeyer 2003)radiation + hydrodynamicsnon-magnetic
• 140x140x200 grids• Synthesize Ca II H spectra
with SPANSAT(396.0-396.8nm)
• blue continuum (396.0nm)in stead of G-band
5600km
5600km1400km
1710km
photosphere
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Results
• simulation reproducesactual contrast
• Not all dark intergranular lanes show bright in Ca II H
blue continuum Ca II H core
Obs
Calc
Calc + smear
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Brightness distribution
• solid curves are derived from simulations.
• solid curve 2 (smear with realistic Airy function) is close to the observation
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Fourior analysis
• Phase differenceG-band -- Ca II H
• Power spectrain good agreement
Obs
Simulation
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Conclusions
• High resolution G-band and Ca II H images were obtained with DOT
• Results of non-magnetic hydrodynamics simulations agree well with observations
• Reversed granulation (i.e. dark intergranular lane and Ca II H brightening) can be explained by non-magnetic process
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Fabry-Pérot interferometer (FPI)
• Basic parametersReflectivity: R and cavity distance: d
• Benefithigh transmission, rapid tuning, no-polarization,spectral resolution 2x105
• ShortcomingsTelecentric optics, wings of transmission profile
R
/
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FPI systems
• VTT/TESOS (Kentischer et al. 1998)Triple FPI
• THEMIS/IPM (Cavallini 1998)UBF + FPI
• THEMIS/IBS (Cavallini et al. 2003)dual FPI
• IMAX/SUNRISE (Martinez-Pillet 2004)• ATST ?
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Calculation
• 2 FPI system
• Parameters: d1, d2, R1, and R2
• Estimate parasitic light, ghost intensity, and FWHM
• Cavity error < 2 nm
d1 d2
R1 R2
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Paracitic light level
R=83%
R=89%
R=94%
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Results
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Conclusion
• Cavity ratio has a significant impact on FPI system performance
• Homogeneity can be achieved by lowering reflectivity of small cavity FPI
• Optimal setupLow resolution & low reflectivity +high resolution & high reflectivity (cavity ratio 0.3-0.4)
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Template
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