The armillary sphere, an astronomical observation device embodying the Orbital Heaven Theory of the Later Han Dynasty in China, holds both historical and scientific significance. It has been produced in various forms by many individuals since its inception in the era of King Sejong in the Joseon Dynasty. A prominent figure in this field was Nam Byeong-cheol (南秉哲, 1817-1863), known for his work 'Uigijipseol' (儀器輯說), published in 1859, which detailed the history, production methods, and usage of the armillary sphere. This text particularly highlights 21 applications of the armillary sphere, divided into 33 measurements, covering aspects like installation, time, and positional measurements, supplemented with explanations of spherical trigonometry. Despite numerous records of the armillary sphere's design during the Joseon Dynasty, detailed usage information remains scarce. In this study, the 33 measurements described in 'Uigijipseol' (儀器輯說) were systematically classified into six for installation, nineteen for position measurement, seven for time measurement, and one for other purposes. Additionally, the measurement methods were analyzed and organized by dividing them into the ecliptic ring, moving equatorial ring, and fixed equatorial ring of the armillary sphere. In other words, from a modern astronomical perspective, the results of schematization for each step were presented by analyzing it from the viewpoint of longitude, right ascension, and solar time. Through the analysis of Nam's armillary sphere, this study not only aims to validate the restoration model of the armillary sphere but also suggests the potential for its use in basic astronomical education based on the understanding of the 19th-century Joseon armillary sphere.

In this study, complaints from visitors in the science museum satisfaction survey were categorized into four primary factors and ten sub-factors. This categorization aimed to provide recommendations for enhancing the Geochang Wolseong Space Creative Science Museum as an illustrative case study. Futhermore, the study examimed the relative importance of each factor by surveying 90 science museum visitors. The following results are obtained. Firstly, it was evident that the Geochang Wolseong Space Creative Science Museum requires urgent improvement. Certainly, in the primary factors, issues related to the utilization environment emerged as the most significant sources of dissatisfaction, while in the sub-factors, the adequacy of fees was identified as the most prominent concern. Secondly, through the result of the IPA (Importance-Performance Analysis) of the complaint factors, four primary issues were identified as top priorities for consideration: fare adequacy, lack of convenient facilities, in sufficient publicity, and a lack of distinctiveness compared to similar facilities. Lastly, when analyzing the relationship between complaints and overall satisfaction, factors related to human service, environment, and educational content had negative effects. In contrast, factors associated with science museum operation exhibited a different trend, suggestinga structural impact relationship with the overall impact of complaints.

In order to study the X-ray radiations from solar type strong interacting binary stars, we have collected X-ray data of 44i Bootis (P=0.2678 days, SP=G2+G2) from the EXOSAT data archive. Preliminarly analysis of a part of these data has been already reported by Vilhu & Heise (1986). In this paper, however, we present a more complete light curve in LE region than the previous work, and some unpublished X-ray light curves and spectrums. Using these new materials a new attempt to find the physical explanation about. some observational characteristic figures in the X-ray light curves and spectrums has been made.

Using a phenomenological model for the accretion onto the magnetic white dwarf, we calclliated some optical line profiles from the magnetosphere of such systems. Line profiles of these systems seem to be produced in the magnetosphere of the compact star due to the reemission of X-ray produced near the stellar surface. Some results of our new calculation and the analysis of these results will be presented. Our results show that the model used here can reproduce the observed optical line profiles and open the possiblity to determine the parameters of individual systems.