In recent years, museums in Japan have been required to operate in two aspects: as public facilities, with an education especially for local residents and tourism attraction. In this paper, a qualitative study using interviews and secondary data research was conducted using Misato Astronomical Observatory and Kawabe Cosmic Park as case studies. Misato Astronomical Observatory and Kawabe Astronomy Park are both public astronomical observatories in Wakayama Prefecture and have many similarities in terms of the characteristics of their facilities. However, Misato Astronomical Observatory is still in operation, whereas Kawabe Astronomy Park was closed in 2014. The purpose of this paper is to explore the direction of sustained operation of public astronomical observatories by identifying changes in the social environment surrounding the facilities over time, and to provide a preliminary examination of the role that public astronomical observatories should play.
The purpose of this paper is to re-evaluate citizens' activities such as pollution studies in the 1960s and 1970s, and citizens' joint learning activities of natural science by The Association for the Geological Collaboration in Japan ("Chi-dan-Ken") that were active throughout Japan in the same period, from the analytical perspective of science communication introduced in Japan after the 2000s. Through this process, we will reevaluate science communication and social education in Japan. Through this process, we will explore the interface between science communication and social education, and reconsider science communication as social education. As a conclusion of this paper, social education activities of science, including natural science and social science, are science communication activities, There are two sides of the same coin. In other words, science communication activities can be considered as social education activities, and at the same time, it is significant to conduct science learning activities in a broad sense in social education as science communication. In other words, it is essential to discuss the science learning activities of local residents who are tackling contemporary issues from the perspectives of both science communication and social education.
The study purpose is to find out how to do special lessons. Based on the discourse of flight from science, which is one of the issues of science education, we will organize the educational practices in the astronomical field. After that, by introducing the special lesson practice that the author has implemented and considering the ingenuity in implementing it, more effective learning can be expected for children who have overcome the problems of the science special lesson by an outside lecturer. In conclusion, it is necessary for the bearers to work together and respect the learning context of the children so that the special lesson does not become a one-time lesson, and the coordinator for smooth cooperation. Roles exist in each university and region, and it should be considered to borrow their power.
This report considers the significance of learning opportunities furnished by university researchers to community residents through lifelong learning and social education research outreach activities. The subject is a case study concerning the "Workshop of SHIRABEKATA on Earth" (Workshop on How to Examine the Earth), which the Graduate School of Environmental Science, Hokkaido University has continued to hold since 2011. The workshop is an extension course for community residents. University researchers planned this workshop with the express purpose of participant learning. As a result, at least 25% of the participants are familiar with the theme of each session and with the research being conducted based on their learning at the workshop. The learning processes, achievements and feedback of the community residents participating in the workshop provide the researchers, who also act as lecturers, with new perspectives on their own research. A well-planned research outreach activity such as this is useful as an initial step for a university functioning as a Center of Community (COC) because it helps the university and researchers establish a new relationship with community residents. To achieve this, those engaged in university research outreach activities must understand that such activities provide learning opportunities for community residents. They must also improve their competencies in planning and implementing outreach activities. At the same time, regional supporters of life-long learning organizations need to recognize research outreach activities as new occasions for learning. Furthermore, universities need to function as COCs in cooperation with regional learning supporters to create learning opportunities for community residents.
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
(
OXFORD UNIV PRESS
)
59
(
5
)
1017
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1025
2007年10月
[査読有り]
概要を見る
We constructed an imaging polarimeter, PICO, that was optimized for comets and/or cometary objects. PICO has a field-of-view of 5' x 10' and employs a fixed Wollaston prism as an analyzer. In the case of polarimeters using a double-beam prism, such as a Wollaston prism, lateral chromatic aberrations originating from the prism often degrade the image quality and measurement accuracy. However, PICO suffers little lateral chromatic aberration due to compensation provided by newly designed lens systems that generate opposite lateral colors. Owing to this design, PICO can obtain highly resolved and very accurate polarization images throughout the FOV (field-of-view). The total accuracy is estimated to be Delta P similar or equal to [(P/85)(2) + 0.3(2)](1/2)% in polarization degree and theta <= 3 degrees in position angle; these values are satisfactory for cometary studies.
The NASA's Deep Impact mission was the first impact experiment to a cometary nucleus. The target of the mission was Comet 9P/Tempel, one of the Jupiter family comets. The impact was performed on July 4th, 2005. Imaging polarimetric observations were carried out by Polarimetric Imager for Comets (PICO) mounted on the Lulin One-meter Telescope (LOT) at Lulin Observatory, Taiwan. Intensity and linear polarization degree maps were obtained on July 3-5, 2005. Impact ejecta plume was clearly recognized in the enhanced intensity map. Furthermore, arc-shaped region of high polarization was recognized in the polarization map. Dust grains in this region had larger expansion velocity than the grains which provided the brightest area in the intensity map. comparing our results with the MIR spectroscopy obtained by Subaru Telescope we conclude that very small carbonaceous grains might be responsible for the region of high polarization. (C) 2007 Elsevier Inc. All rights reserved.
T Yanagisawa, A Nakajima, K Kadota, H Kurosaki, T Nakamura, F Yoshida, B Dermawan, Y Sato
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
(
OXFORD UNIV PRESS
)
57
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2
)
399
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408
2005年04月
[査読有り]
概要を見る
We have devised an automatic detection algorithm for unresolved moving objects, such as asteroids and comets. The algorithm uses many CCD images in order to detect very dark moving objects that are invisible on a single CCD image. We carried out a trial observation to investigate its usefulness, using a 35-cm telescope. By using the algorithm, we succeeded to detect asteroids down to about 21 mag. This algorithm will contribute significantly to searches for near-Earth objects and to solar-system astronomy.
F Yoshida, B Dermawan, T Ito, Y Sawabe, M Haji, R Saito, M Hirai, T Nakamura, Y Sato, T Yanagisawa, R Malhotra
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
(
OXFORD UNIV PRESS
)
56
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6
)
1105
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1113
2004年12月
[査読有り]
概要を見る
The asteroid (832) Karin is the largest member of the Karin family. which is thought to have been formed by a catastrophic collision 5.8 Myr ago. We performed photometric observations of Karin from 2003 July to September. and we report here on its lightcurve and colors in several visible bands. The rotational synodic period of Karin was determined to be 18.35 +/- 0.02 hr. Its absolute magnitude (H) and the slope parameter (G) of the Solar phase curve were 11.49 +/- 0.02 and 0.19 +/- 0.04, respectively. Based on our color observations. we confirmed that Karin is an S-type asteroid. In addition, we found that there is likely to be a color variation over the Surface of Karin. We infer that the color variation is due to the difference between the fresh surface. excavated by the family-forming disruption, and the weathered surface, exposed to space radiation and particle bombardment over a long period.
Kasuga, T, Watanabe, J, Ebizuka, N, Sugaya, T, Sato, Y
Astronomy and Astrophysics
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E D P SCIENCES
)
424
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3
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L35
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L38
2004年09月
[査読有り]
概要を見る
This paper shows the first observational result of a spectrum of a June Bootid meteor obtained by the High-Definition TV observational system. The very faint spectrum appeared at 15(h)59(m)29.69(s) on 2004 June 23 UT, which was about 5th magnitude. Wavelengths between 360-620 nm were observed, and the strong emissions of neutral atoms as MgI, FeI and NaI were identified. Emissions of single ionized atoms were not observed. The abundances of metallic atoms, their excitation temperature were obtained under the Local Thermal Equilibrium (LTE) conditions. The results, Fe/Mg=0.15 and Na/M=0.00027 suggest the possibility that the abundances of June Bootid meteor are extremely different from the solar system abundances. The excitation temperature value, 3867+/-13 K is low in agreement with their slow moving velocity.
B Dermawan, T Nakamura, H Fukushima, H Sato, F Yoshida, Y Sato
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
(
OXFORD UNIV PRESS
)
54
(
4
)
635
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640
2002年08月
[査読有り]
概要を見る
Near-Earth asteroid (25143) 1998 SF36 is now planned as the target for the Japanese MUSES-C sample return mission. We conducted extensive photometric observations at NAO-Mitaka from 2001 February 15 until March 19 to obtain its physical properties, such as asteroid's colors, rotation period, phase curve, and light curves. The colors of this asteroid were found to be S-type and in agreement with the spectroscopic result by Binzel et al. (2001, Meteor. Planet. Sci., 36, 1167). From the phase curve of this object, the visual absolute magnitude is obtained to be 18.61 +/- 0.18; we suggest that the albedo may be higher than that for typical S-type asteroids, after applying a known empirical relation between phase curve slope and geometric albedo. We also reveal that the synodic rotation period of this asteroid is 12.13 +/- 0.02hr and the peak-to-peak light variation amplitude at zero phase angle has been shown to be similar to 0.49 mag, which implies the ratio of the longest and intermediate ellipsoidal axes for the asteroid greater than or similar to 1.6.
