• Journal of the Korea Institute of Information Security & Cryptology
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• v.14 no.6
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• pp.47-56
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• 2004

Automatic code generating function for security protocol of SPEAR II and IFAD VDM-SL Toolbox supporting formal specification is presented in this paper. Among the functions of these tools we compare and analyze the aspects of functions, users, operation and code generation. And we suggest direction to the developing of safe security S/W. The automatic code generating function for security protocol gives the direction for developing of the safe secure software in formal specification method.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.110.2-110.2
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• 2011

Nishikida et al. (2006) presented the first far-ultraviolet (FUV) em${\lambda}$ission-line images of the Vela supernova remnant (SNR) obtained with FIMS/SPEAR instrument. Those include C III ${\lambda}$977, O VI ${\lambda}{\lambda}$1032, 1038, Si IV+O IV] ${\lambda}{\lambda}$1393, 1403 (un-resolved), C IV ${\lambda}{\lambda}$1548, 1551 emission-line images. As a following work, we re-constructed these emission-line images using the new-version processed FIMS/SPEAR data. Additionally, we made N IV] ${\lambda}$1486, He II ${\lambda}$1640.5, O III] ${\lambda}{\lambda}$1661, 1666 emission-line images. The new-version images cover the whole region of the Vela SNR and show more resolved features than the old-version. We compare these FUV emission-line images with other wavelength (X-ray, optical, etc.) images obtained in previous studies.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.70.1-70.1
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• 2010

We present the far-ultraviolet (FUV) emission line morphologies in the whole region of the supernova remnant G65.3+5.7 using the FIMS/SPEAR data. The morphologies of the C IV ${\lambda}{\lambda}1548$, 1551, $H2{\lambda}1608 $, He II ${\lambda}1640$, and O III] ${\lambda}{\lambda}1661$, 1666 lines appear to correlate clearly with the optical emission line images or the ROSAT X-ray (0.11-0.284 keV) image obtained in some of the previous studies. We found that a foreground dust cloud, resonant scattering, and incompleteness of radiative shocks have made the definite differences between the morphologies of the above FUV emission lines. We also present the FUV spectra and line intensities from a few sub-regions.

• The Korean Journal of Malacology
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• v.28 no.3
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• pp.255-258
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• 2012

Forty four specimens (22.5-34.2 cm ML) of Heterololigo bleekeri were collected around Dokdo, East Sea on March 1, 2012. It was identified as H. bleekeri based on the following combination of morphological character: mantle very elongate; fin large, thick, length two-thirds of mantle length; arms very short and small in relation to body size, are formula III>II>IV>I.

• Korean Journal of Food Science and Technology
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• v.49 no.3
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• pp.343-348
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• 2017

The aim of this study was to compare the anti-inflammatory effects of ethanol extracts of root peel and spear of mulberry (RME and SME, respectively) in lipopolysaccharide (LPS)-stimulated RAW 264.7 macrophages. Both extracts significantly inhibited the production of reactive oxygen species (ROS), nitric oxide (NO), and interleukin-6 (IL-6). However, prostaglandin $E_2$ ($PGE_2$) levels decreased in LPS-stimulated RAW 264.7 cells treated with SME. Additionally, the extracts reduced inducible NO synthase (iNOS) expression and cyclooxygenase-2 (COX-2) in mRNA levels. Although ROS production was lower in the RME-treated cells than in the SME-treated cells, the levels of other inflammatory parameters, including IL-6 and $PGE_2$, and mRNA levels of iNOS and COX-2 reduced more in the SME-treated cells. These results indicate that SME showed higher anti-inflammatory activities than RME. Therefore, SME can be used as a functional food ingredient to enhance health.

• Journal of The Korean Astronomical Society
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• v.38 no.2
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• pp.69-72
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• 2005

The FIMS (Far-ultraviolet IMaging Spectrograph; also known as SPEAR, Spectroscopy of Plasma Evolution from Astrophysical Radiation) is the primary payload of the STSAT-1, the first Korean science satellite, which was launched in September, 2003. The FIMS performs spectral imaging of diffuse far-ultraviolet emission with the unprecedented wide field of view and the relatively good spectral resolution. We present far-ultraviolet spectral observations of highly ionized interstellar medium including supernova remnants, superbubbles, soft X-ray shadows, and the molecular hydrogen fluorescent emission lines. The FIMS has detected He II, C III, 0 III, O IV, Si IV, O VI, and $H_2$ fluorescent emission lines. The emission lines arise in shocked or thermally heated and in photo-ionized gases. We present an overview of the FIMS instrument and its initial observational results.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.99.2-99.2
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• 2012

We updated the far-ultraviolet (FUV) spectral images of the entire Vela supernova remnant (SNR) using newly processed FIMS/SPEAR data. In the present study, we compare the newly produced FUV images with the X-ray and $H{\alpha}$ images, and examine how the Vela SNR evolves and interacts with the ambient medium on a global scale. The comparison with X-ray images has revealed a FUV filamentary feature corresponding with the boundary of the northeast-southwest asymmetry of the X-ray shell. The relatively low O IV] ${\lambda}1404$ to O III] ${\lambda}{\lambda}1661$, 1666 ratio estimated on the FUV filament is compatible with the previous proposal that the observed asymmetry of the Vela SNR could be due to the ${\gamma}2$ Velorum stellar wind bubble (SWB). The southwest FUV features surrounding a faint extended X-ray region are characterized as the region where the Vela SNR is interacting slightly stronger with ambient mediums within the dim X-ray southwest section. From a comparison with the $H{\alpha}$ image, we identify a ring-like $H{\alpha}$ feature overlapped with an extended hot X-ray feature of similar size and two local peaks of C IV ${\lambda}{\lambda}1548$, 1551 emission. Their morphologies are consistent with the expected shape when the $H{\alpha}$ ring is in direct contact with the near or far side of the Vela SNR. We suggest that the B3V-type star HD 76161 found at the center of the $H{\alpha}$ ring would be the exciting source of the H II region.