yunnan one meter infrared solar tower jun lin. why is ynst? after solar-b launch, what can we do by...
TRANSCRIPT
Why is YNST?
After Solar-B launch, what can we do by using of ground-based telescope ?
Detailed chromosphere diagnostics
Special magnetic field observations (IR, hyperfine-structure of atoms)
Higher angle resolution
----- B. W. Lites ( at THEMIS user meeting )
What is YNST?
• An optical system of 1-meter aperture: resolution < 0.3 arcsec (200 km), vacuum tube, AO
• Symmetric structure for accurate measurement of magnetic field:
Gregorian telescope, 10-4 polarization analyzer, I, Q, U, V
• Focal instrument of high resolution: Filter-based image Fabry-Perot filter, magnetograph, high spectral resolution
• Multi-wavelength observations: Multi-wavelength spectrograph, Near-Infrared detectors • High accuracy tracking and pointing system: Auto guiding system, correlating tracker
YNST’s Spectral Range
• The Sun will be observed within the range from 3,000 to 25,000 Å.
• This range spans the spectrum from UV to near IR.
• Information includes those of the photosphere, the chromosphere, and the corona.
• Spectral lines include both magnetic field and plasma flow sensitive ones.
General Information of Fuxian Lake & Cape Eagel
• The distance from Kunming City: 60 km
• Altitude: 1712 m
• Longitude: 102°57'11"
• Latitude: 24°34'47"
• Maximum Width: 11.5 km
• Maximum Length: 31.5 km
• Maximum Depth: 155.0 m
• Surface Area: 211.0 km2
• Number of Clear Days/year: > 275
• Average Wind Speed: < 6 m/s
• Water Integration : 11mm (average over a year)
• Average r0: 12.3 cm (average over a year), 11.5 cm ( median of a
year)
Parameters for Each Component(F/45.9 Modified Gregorian System)
• Window glass: H = 65 mm, D = 1,200 mm
• M1 : D = 980 mm, F/2.45 (paraboloid)
• M2 : D = 257.8 mm, F/9 (ellipse,-0.327)
• M3 : D = 234.3 mm, F/45.9 (ellipse,-0.453)
• M4 : 43.4 mm × 65 mm (flat)
• Exit pupil: D = 152 mm M5
• View field: 3 arcmin
• Alt-azimuth mount, friction transmission
Spectrograph and Other Instruments
Multi-wavelength spectrograph
Other instruments
H 6563
CaII 8542
HeI 10830
To adaptive lab
Parameters for Spectrometer
Grating constant: 1200 g/mm; Blaze angle: 36 °48'; Incident angle: 33.5Collimating concave mirror f = 6000 mm Focusing concave mirror f = 5000 mm
Lines Orders Wavelength(Å) Diffraction Angle(°) Linear Dispersion(Å/mm)HeD3 1 5878 8.81 1.647 H 1 6563 13.63 1.620 CaII 1 8542 29.18 1.455 (Filter-based image, absence in ONSET)HeI 1 10830 48.39 1.107FeXIII ? 10746+10798 ? ?H 2 3646 18.85 1.577K+H 2 3934+3968 23.08 1.533H 2 4861 37.93 1.315D1, 2 2 5885 59.13 0.855G-band ? 4300~4310 ? ?Fe I ? 6301.5+6302.5 ? ?
Spectral Lines of Interest (Ph+Ch)
• FeI (6301.5+6302.5): Photospheric line sensitive to magnetic field.
• H: Traditional line used to observe flares.• CaII (8542): Chromospheric line sensitive to magneti
c field.• HeI (10830): Good for observations of the filament
magnetic field.
YNST’s Scientific Goals & Tasks
• Observational data of high resolutions in both time and space for magnetic field of fine structures.
• Properties of tiny fibrils, or flux tubes of kilo-gauss magnetic field.
• Coupling of magnetic field and mass motions, and energy transportation from the photosphere to the corona.
• Conducting multi-wavelength observations and data analyses; providing forefront observational data and opportunities to the research communities.