The Solar Optical Telescope for the Hinode Mission: An Overview

Tsuneta, S.; Ichimoto, Kiyoshi; Katsukawa, Y.; Nagata, Shinji; Otsubo, Masahisa; Shimizu, Toshifumi; Suematsu, Y.; Nakagiri, M.; Noguchi, Motokazu; Tarbell, T. D.; Title, A. M.; Shine, R. A.; Rosenberg, W. J.; Hoffmann, C.; Jurcevich, B.; Kushner, G.; Levay, M.; Lites, B. W.; Elmore, D.; Matsushita, Tadashi; Kawaguchi, Noboru; Saitō, Hideo; Izumi, Mitsuru; Hill, L. D.; Owens, J. K.

doi:10.1007/978-0-387-88739-5_8

Cited by 31 publications

(34 citation statements)

References 41 publications

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“…Therefore, baffles are set at the entrance of the system to keep the stray light out, and baffles are used to correct or limit the light into the aperture with the help of a Lyot stop installed behind the focal plane. Similar trade offs in designs can be found in STEREO [8,9], SMEI (Solar Mass Ejection Imager) and HERSCHEL (Helium Resonance Scattering in Corona & Hemisphere) [7]. The thermal design and stray light elimination design of these solar telescopes previously indicated that there are some links and constraints between the traditional thermal design and the traditional stray light elimination design.…”

supporting

confidence: 52%

“…For example, in order to cool the focal plane with a huge thermal flux, the heat stop is installed behind of the focal plane in the ATST (Advanced Technology Solar Telescope) [6], but the aluminum HDM (Heat Dump Mirror) is installed behind the focal plane in the SOLAR-B [7]. However, the heat stop and the aluminum HDM are two primary stray light sources in the two systems due to diffraction around the two parts.…”

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confidence: 99%

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Thermal analysis of the baffle structure of the Solar Space Telescope

Wang

2010

Sci. China Phys. Mech. Astron.

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The SST (Space Solar Telescope) is an astronomical telescope with a primary mirror of 1 m in diameter. It observes the sun with a small view field to ensure that its high spatial resolution imaging has 0.1″-0.15″ and high SNR (signal to noise ratio). Surrounding the small view field is still the sun, which is an intense source of both heat and stray light. The baffles (the main baffle, the aperture, and the outer baffle), which are used to eliminate the stray light, will change the thermal flux in the SST and will weaken the effect of the thermal control design. In this study, the compatibility analysis of the thermal effect of baffle structures in SST is performed. The GCF (Geometry Composing Function) and BRDF (Bidirectional Reflectance Distribution Function), which are two inherent related parameters in the compatibility analysis, are derived. The objective and method of the compatibility analysis are determined. With the thermal analysis software, the temperature fields are calculated for different lengths of the main baffle, different radii of apertures, different lengths of the outer baffle with a 3′ tilt angle and 16′ tilt angle, and different tilt angles of the outer baffle with a 200 mm length. A series of configurations and sizes of the baffles are studied with the goals of both thermal control and elimination of stray light. The design of the baffle structure of SST is achieved: the main baffle of length 4100 mm, the internal shield of radius 494 mm, the outer baffle of length 200 mm, and the outer baffle of tilt angle 3′ are successfully designed. This paper presents the relationship between the thermal control design and stray light elimination plan in the SST. The aims of the optimal design of the baffle structure of SST are reached. The thoughts and methods of the optimal analysis are also useful for similar optical telescopes designed for solar observation.

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supporting

confidence: 52%

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confidence: 99%

Thermal analysis of the baffle structure of the Solar Space Telescope

Wang

2010

Sci. China Phys. Mech. Astron.

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“…The G-band (430 nm) data with a 2 minute cadence were obtained with the Broadband Filter Imager (BFI) of Solar Optical Telescope (SOT) [10] on board Hinode. The vector magnetograms and other thermodynamic parameters were obtained with a Milne-Eddington Stokes inversion [11,12] Since the active region is not located at the center of solar disk, the projection effect was corrected with coordinate transformation.…”

Section: Data Setsmentioning

confidence: 99%

The change of magnetic inclination angles associated with the X3.4 flare on December 13, 2006

Jing

Tan

et al. 2009

Sci. China Ser. G-Phys. Mech. Astron.

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Recent studies showed a consistent pattern of changes in the sunspot structure associated with major flares: part of the peripheral penumbral regions vanishes during flares, and meanwhile, the umbral cores and/or inner penumbral regions are darkened. To understand the underlying physics of these observations, we compare the magnetic inclination angle in the decayed peripheral and the enhanced inner penumbral regions before and after the 4B/X3.4 flare of 2006 December 13 by using the highresolution vector magnetograms from Hinode. We find that the mean inclination angle in the decayed penumbra increases after the flare while that in the enhanced penumbra near flaring neutral line decreases. The result confirms the previous idea that two components of a δ sunspot become connected after flares. As a result of new connection, peripheral penumbral fields change from a more inclined to a more vertical configuration and transverse fields in umbral core and inner penumbral regions increase substantially (Liu et al. 2005). The flare-associated changes of Doppler width as well as other parameters (the transverse field strength, continuum intensity and filling factor) are also presented.Sun: magnetic fields, Sun: photosphere, Sun: flares As shown by magnetogram data from both groundbased and space-borne instruments, photospheric magnetic fields can experience some rapid, significant and permanent changes during X-and M-class solar flares. For instance, Wang et al. [1] detected a permanent increase in the magnetic flux of the leading polarity of active regions and a decrease in the following polarity based on a sample of six Xclass flares. Sudol and Harvey [2] conducted a survey of 15 X-class flares and found that abrupt and persistent changes in the photospheric magnetic flux are common features associated with X-class flares. At least two-third of the field changes occurred in the penumbral regions of sunspots. With the advanced non-linear force-free field modelling techniques [3] , Jing et al. [4] investigated the altitude variation of magnetic shear associated with the X3.4 flare of 2006 December 13. They found that magnetic shear increased after the flare around the flaring magnetic neutral line (NL) below a height of ∼8 Mm and decreased from that height to ∼70 Mm. Citation: Li Y X, Jing J, Tan C Y, et al. The change of magnetic inclination angles associated with the X3.4 flare on

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“…We use a series of image sequences obtained in 25 October 2008 (near 03 h 18 UT) in the Ca II H emission line; the wavelength pass-band being centered at 398.86 nm with a FWHM of 0.3 nm. A fixed cadence of 8 s is used (with an exposure time of 0.5 s) giving a spatial full resolution of the SOT-Hinode (Tsuneta et al, 2008) limited by the diffraction at 0''16 (120 km); a 0''0541 pixel size scale is used.…”

Section: Observationsmentioning

confidence: 99%

Contribution to the modeling of solar spicules

Tavabi

Koutchmy

Ajabshirizadeh

2011

Advances in Space Research

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Solar limb and disc spicule quasi- periodic motions have been reported for a long time, strongly suggesting that they are oscillating. In order to clear up the origin and possibly explain some solar limb and disc spicule quasi-periodic recurrences produced by overlapping effects, we present a simulation model assuming quasi- random positions of spicules. We also allow a set number of spicules with different physical properties (such as: height, lifetime and tilt angle as shown by an individual spicule) occurring randomly. Results of simulations made with three different spatial resolutions of the corresponding frames and also for different number density of spicules, are analyzed. The wavelet time/frequency method is used to obtain the exact period of spicule visibility. Results are compared with observations of the chromosphere from i/ the Transition Region and Coronal Explorer (TRACE) filtergrams taken at 1600 angstrom, ii/ the Solar Optical Telescope (SOT) of Hinode taken in the Ca II H-line and iii/ the Sac-Peak Dunn's VTT taken in H{\alpha} line. Our results suggest the need to be cautious when interpreting apparent oscillations seen in spicule image sequences when overlapping is present, i.e.; when the spatial resolution is not enough to resolve individual components of spicules.Comment: 20 pages, 7 figures, 1 tabl

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The Solar Optical Telescope for the Hinode Mission: An Overview

Cited by 31 publications

References 41 publications

Thermal analysis of the baffle structure of the Solar Space Telescope

Thermal analysis of the baffle structure of the Solar Space Telescope

The change of magnetic inclination angles associated with the X3.4 flare on December 13, 2006

Contribution to the modeling of solar spicules

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