• Journal of Oral Medicine and Pain
• /
• v.20 no.1
• /
• pp.159-169
• /
• 1995

The purpose of this study was investigating the effects of pivot splint on width of the temporomandibular joint space in order to get the basic data for clinical applications. Pivot splint could be used for treating the patients with temporomandibular disorders, especially for chronic closed lock which would not be reduced by joint manipulation or with other methods. So it is necessary to have a lot of underlying data for using pivot splint, but there is few available reports related to mechanical principle or clinical results of the splint. Healthy twenty dental students wee collected for this study and pivot splint with 2.5mm high right-side pivot was used. Next, transcanial projection was taken and width of joint space at there mandibular positions were measured : habitual occlusion position, clenching position with splint, and clenching position with splint and mandibular force. The data were processed with SAS statistical program. The obtained results were as follows : 1. Ipsilateral posterior joint space width was increased on clenching the pivot splint, but joint space widths of contralateral side were not significantly changed. 2. Superior and posterior joint space width were increased on clenching the pivot splint with mandibualr force on both ipsilateral and contralateral side. 3. Ipsilateral joint space widths were not significantly changed from habitual occlusion position to clenching the pivot splint with active mandibular force, but in case of with passive mandibular force, posterior joint space width was significantly increased. 4. Correlationships between mandibular positions were more significant at anterior joint space than at superior or posterior joint space. But the correlation between clenching and clenching with mandibular force was significant at all the three joint space.

• The Bulletin of The Korean Astronomical Society
• /
• v.39 no.2
• /
• pp.92.1-92.1
• /
• 2014

In astronomical spectroscopy, stable auto-guiding and accurate target centering capabilities are critical to increase the achievement of high observation efficiency and sensitivity. We developed an instrument control software for the Immersion GRating INfrared Spectrograph (IGRINS), a high spectral resolution near-infrared slit spectrograph with (R=40,000). IGRINS is currently installed on the McDonald 2.7 m telescope in Texas, USA. We had successful commissioning observations in March, May, and July of 2014. The role of the IGRINS slit-viewing camera (SVC) is to move the target onto the slit, and to provide feedback about the tracking offsets for the auto-guiding. For a point source, we guide the telescope with the target on the slit. While for an extended source, we use another a guide star in the field offset from the slit. Since the slit blocks the center of the point spread function, it is challenging to fit the Gaussian function to guide and center the target on slit. We developed several center finding algorithms, e.g., 2D-Gaussian Fitting, 1D-Gaussian Fitting, and Center Balancing methods. In this presentation, we show the results of auto-guiding performances with these algorithms.

• Journal of the Korean Society for Aeronautical & Space Sciences
• /
• v.48 no.10
• /
• pp.745-752
• /
• 2020

A numerical study was carried out to evaluate the aerodynamic characteristics of the supersonic grid fins installed on SpaceX Falcon 9. The unit-grid-fin concept was utilized for more efficient and simpler 3-D steady flow calculations. Pre- and post-correction processes that accounted the interference effects by the angle of attack of the missile, the influences of the outer frame of the grid fin and the connecting rods were improved in the study, and it was demonstrated that the present correction method was more accurate as compared to previous studies. Finally, the present approach was applied to evaluate the aerodynamic characteristics in transonic/supersonic flights of SpaceX Falcon 9 with various angle of attacks.

• Journal of Digital Convergence
• /
• v.18 no.2
• /
• pp.269-276
• /
• 2020

In this study, we will analyze the classroom space of elementary schools that have implemented the Seoul Metropolitan Government's 'Dream Classroom' project and identify satisfaction and needs in terms of users. Primary school was selected and the composition and color of space was investigated by the present ministerial inspection. The survey was conducted on homeroom teachers and analyzed as SPSS/WIN Statistical Programme 22.0. The satisfaction level of space elements was verified by the technical statistical analysis, the general classroom and the 'classroom with dreams' difference in response t-test, the need for planning elements (criticality), and the difference in satisfaction with one way ANOVA. The space had the most separate, primary-colored classrooms. They preferred emotional factors and bright and light atmosphere for the lower grades, and the soft and soft atmosphere for the middle and high school students. The school preferred communication space with the community, proper play and relaxation space for the complex type of classroom. This will help set the direction for elementary school classroom space planning during the Fourth Industrial Revolution.

• Journal of The Korean Astronomical Society
• /
• v.51 no.4
• /
• pp.111-117
• /
• 2018

A numerical method is proposed to calculate the response of detectors measuring particle energies from incident isotropic fluxes of electrons and positive ions. The isotropic flux is generated by injecting particles moving radially inward on a hypothetical, spherical surface encompassing the detectors. A geometric projection of the field-of-view from the detectors onto the spherical surface allows for the identification of initial positions and momenta corresponding to the clear field-of-view of the detectors. The contamination of detector responses by particles penetrating through, or scattering off, the structure is also similarly identified by tracing the initial positions and momenta of the detected particles. The relative contribution from the contaminating particles is calculated using GEANT4 to obtain the geometric factor of the instrument as a function of the energy. This calculation clearly shows that the geometric factor is a strong function of incident particle energies. The current investigation provides a simple and decisive method to analyze the instrument geometric factor, which is a complicated function of contributions from the anticipated field-of-view particles, together with penetrating or scattered particles.

• The Bulletin of The Korean Astronomical Society
• /
• v.37 no.2
• /
• pp.119.1-119.1
• /
• 2012

It is well known that the FLRs are excited by compressional waves via mode conversion, but there has been no apparent criterion on the maximum amplitude in the regime of linear approximations. Such limited range of amplitude should be understood by including nonlinear saturation of FLRs, which has not been examined until now. In this study, using a three-dimensional magnetohydrodynamic (MHD) simulation code, we examine the evolution of nonlinear field line resonances (FLRs) in the cold plasmas. The MHD code used in this study allows a full nonlinear description and enables us to study the maximum amplitude of FLRs. When the disturbance is sufficiently small, it is shown that linear properties of MHD wave coupling are well reproduced. In order to examine a nonlinear excitation of FLRs, it is shown how these FLRs become saturated as the initial magnitude of disturbances is assumed to increase. Our results suggest that the maximum amplitude of FLRs become saturated at the level of the same order of dB/B as in observations roughly satisfies the order of ~0.01. In addition, we extended this study for the plasma sheet boundary layer (PSBL) region. We can discuss the maximum disturbances of the Alfven via mode conversion becomes differently saturated through each region.

• The Journal of Sustainable Design and Educational Environment Research
• /
• v.21 no.3
• /
• pp.14-25
• /
• 2022

This study focuses on the "online education space" in which the need is expected to increase in the school field in the future. As a way to create an online education space that can provide quality online education while sufficiently guaranteeing students' right to online learning, the basic direction, attributes of space, and types of spaces were presented. To this end, the literature reviewing the concept and characteristics of online education and the characteristics and main functions of the online education space was investigated and analyzed. In addition, to supplement the limitations of the literature review, domestic and overseas online education operation and space creation cases were investigated and analyzed. Also, the perception of and demand for online education of teachers who operate online education in the actual education field were investigated. As a result, ① basic principles and directions of online education space creation, ② attributes of online education space (convergence, convenience, de-place), and ③ 33 spaces (see Table 8) required for online education were presented.

• The Bulletin of The Korean Astronomical Society
• /
• v.43 no.1
• /
• pp.67.3-68
• /
• 2018

We plan to automatize the operation of Kyung Hee Astronomical Observatory (KHAO) 76 cm Telescope by adapting KAOS30 (KHU Automatic Observing Software for McDonald 30 inch Telescope). The software is developed to improve the efficiency of the observation system for monitoring transients and variable sources. It has installed and operated at McDonald 30 inch telescope since 2017 August. KAOS76 (KHU Automatic Observing Software for KHAO 76 cm Telescope) consists of four packages: Telescope Control Package (TCP), Data Acquisition Package (DAP), Auto Focus Package (AFP), and Script Mode Package (SMP). Most of the packages can be configured by minimized modifications of the codes because it includes common libraries for FLI instruments and also ASCOM standard. TCP, DAP, and AFP control astronomical devices. SMP supports automatic observing in a script mode. TCP of KAOS76 can communicate with the TCS via ASCOM. Also, KAOS76 has an extra function to compensate the misalignment of the polar axis. In this poster, we show the current status of the observing system with KAOS76.

• Journal of The Korean Astronomical Society
• /
• v.44 no.5
• /
• pp.143-150
• /
• 2011

This paper reports a characteristic motion of a polarity inversion line (PIL) formed at the solar surface, which is newly found by performing a three-dimensional magnetohydrodynamic simulation of flux emergence in the Sun. A magnetic flux tube composed of twisted field lines is assumed to emerge below the surface, forming a bipolar region with a PIL at the surface. A key finding is the successive half-turn rotation of the PIL, leading to the formation of a quadrupolar-like region at the surface and a magnetic configuration in the corona; this configuration is reminiscent of, but essentially different from the so-called inverse-polarity configuration of a filament magnetic field. We discuss a physical mechanism for producing the half-turn rotation of a PIL, which gives new insights into the magnetic structure formed via flux emergence. This presents a reasonable explanation of the configuration of a filament magnetic field suggested by observations.

• The Bulletin of The Korean Astronomical Society
• /
• v.44 no.1
• /
• pp.42.3-42.3
• /
• 2019

The high-resolution near-infrared (NIR) spectroscopy can reveal the evidence of the accretion burst (e.g., the broadened absorption features produced by the Keplerian disk motion) although the moment of the outburst was not caught. The embedded protostar IRAS 16316-1540 observed with the Immersion Grating Infrared Spectrograph (IGRINS, $R={\Delta}{\lambda}/{\lambda}{\sim}45000$) shows the broad absorption features in atomic and CO transitions, as seen in FU Orionis objects (FUors), indicative of an outburst event. We examine whether the spectra of IRAS 16316-1540 arise from the rotating inner hot gaseous disk. Using the IGRINS spectral library, we show that the line profiles of IRAS 16316-1540 are more consistent with an M1.5 V template spectrum convolved with a disk rotation profile than the protostellar photosphere absorption features with a high stellar rotation velocity. We also note that the absorption features deviated from the expected line profile of the accretion disk model can be explained by a turbulence motion generated in the disk atmosphere. From previous observations that show the complex environment and the misaligned outflow axes in IRAS 16316-1540, we suggest that an impact of infalling clumpy envelope material against the disk induces the disk precession, causing the accretion burst from the inner disk to the protostar.