Slide 1

Spectrum of stars observed with Bisei astronomical observatory and self-made fiber type spectroscope Kazuki Kunitomo, Ryo Isii, Kazuki Kunitomo, Ryo Isii, Yasuhiro Nakada, Yukihiro Matsumoto, Yasuhiro Nakada, Yukihiro Matsumoto, Kazuki Hama, Yuuya Miyamoto Kazuki Hama, Yuuya Miyamoto Okayama Shoka University High School nature Okayama Shoka University High School nature science science Slide 2 Analysis Date Uranus HR6705 HR7328 HR7462 HR7479 HR7635 HR7950 HR7963 HR8023 HR8276 Date : From July 31 to August 2, 2006 Place : Bisei Astronomical Observatory Devices used for analysis Telescope : 101cm reflecting telescope of Cass grain type Spectroscope : The low decentralization spectroscope CCD camera : DU-440BV of electronic cooling made by ANDL co,Ltd Analytical software Be Spec Makali Slide 3 Analysis Processes It uses and it first processes it with a dark, frame flat frame of the heavenly body frame and the comparison light frame Extraction of spectrum data Extraction from comparison source of light image Identification of wavelength Wavelength calibration Strength calibration Output of graph Spectrum of Uranus Slide 4 Uranus numberelementa wavelength Hr4337.5 H4876.0 Ne 5435.0 H 5735.4 Na5946.2 XeI 6189.5 H6563.3 H6666.1 O 6876.4 Absorption line O 7633.1 Slide 5 Sun Sun numberelementa wavelength Ca4452.7 Ti4535.3 Fe 14873.7 Fe 150339 Mg 15172.8 Fe 15267.2 Fe 15322.3 Fe 15408 Fe 15487.5 Fe 15597.7 Fe 15715.7 Slide 6 Surface external temperature and Maximum extremely a wavelength of Uranus The law of Vienna T 0.29 Maximum extremely a wavelength T Surface external temperature Maximum extremely a wavelength 4962.8 Surface external temperature 5843.5K The spectrum a type G Sun Surface external temperature about K The spectrum a type G Slide 7 HR6705 numberelement a wavelength Fe4294.05 Fe4332.37 Fe4378.06 He4858.12 Mg5168.33 Fe5266.67 Na5890.48 H6562.64 O 6870.13 Absorption line O 7599.02 Slide 8 number element a wavelength 3894.62 3931.89 4281.37 4362.63 4852.22 5164.3 5267.04 5894.89 6499.63 6566.52 6872.82 Absorption line Absorption line Absorption line Slide 9 numberelementa wavelength Fe4308.68 Ti4457.07 Xe4529.7 H4861.02 Mg5183.81 Fe5268.55 Ca5588.04 Na5890.17 Ti6162.32 H6562.62 O2O26562.62 Absorption line Absorption line O27185.17 Slide 10 numberelementa wavelength Ti3918.17 Ar4303 Cr 483. C25154 Fe5253 Na5885.57 Ca6492.25 H6559.31 O26866.03 Absorption line Slide 11 HR HR numberelementa wavelength Ca4226.09 Fe4303.69 Mg5206.37 Fe5207.49 Fe5328.74 Hg5783.88 Na5892.42 Fe6256.69 O6360.38 Fe6495.6 H6562.67 O26871.46 Absorption line O27604.97 Slide 12 HR7950 numberelementa wavelength H3793.79 H3830.89 CN3884.51 N3964.78 N4097.75 Fe4337.05 Absorption line H6561.75 Slide 13 HR7963 numberelementa wavelength H3828.74 C3882.15 N3962.96 N4095.1 Fe4335.16 Cr4808.66 Cd5122.09 H6557.46 O26871.4 Absorption line Slide 14 HR8023 numberelementa wavelength CN3881.9 N3963.32 N4095.12 Fe4335.09 He4538 He4682.58 He4859.16 C25127.28 Ne 5411.02 H6561.54 Absorption line TiO7275.15 Slide 15 HR8276 numberelementa wavelength CN3884.09 N3969.16 N4096.82 Fe4336.59 He4860.24 Ha6562.11 O26871.41 Absorption line O27620.16 Slide 16 Processes Results Heavenly body Maximum extremely a wavelengt h Surface external temperatu re The spectrum a type documents HR6705 4813.9 5918K KK HR7328 5357.98 5412.48KGG HR7462 5335.8 5434KGK HR7479 4795.7 6047K F G HR7635 6071 4776K K M HR7950 4188.6 6923K F A HR7963 3804.1 7623K A B HR8023 3736.2 7761K A O HR8276 4253.6 6817K FF Slide 17 spectroscope of making by oneself The solar spectrum was observed with the self-made spectroscope. Slide 18 Examination The solar spectrum decided to be observed taking picture of the cloud by using 16cm reflecting telescope for the observation this time. The fluorescent lamp was used as a comparison source of light. Macari was used for the analysis. It characterizes, and absorption lines in the atmosphere are seen in any graph. Slide 19 The future When the Bisei astronomical observatory was compared to what observed with the spectroscope of making by oneself, the wavelength that was able to be identified was different. I want to analyze it in detail in the future. Moreover, it wants to observe the spectrum of the fixed star with the self-made spectroscope and to analyze it. Thank you for listening.