• 소성∙가공
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• 제9권6호
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• pp.590-597
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• 2000

A finite element formulation lot the simulation of axisymmetric sheet hydroforming is proposed, and an implicit program is coded. In order to describe normal anisotropy of steel sheet, Hill's non-quadratic yield function (Hill, 1979) is employed. Frictional contacts among sheet surface, rigid tool surface, and flexible hydrostatic pressure are considered using mesh normal vectors based on finite element of the sheet. Applied hydraulic pressure is also considered as a function of forming rate and time and treated as an external loading. The complete set of the governing relations comprising equilibrium and interfacial equations is approximately linearized for Newton-Raphson algorithm. In order to verify the validity of the developed finite element formulation, the axisymmetric bulge test is simulated. Simulation results are compared with other FEM results and experimental measurements and showed good agreements. In axisymmetric hydroforming processes of a disk cover, formability changes are observed according to the hydraulic pressure curve changes.

• 천문학회보
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• 제39권1호
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• pp.58.2-58.2
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• 2014

The Arches cluster is a young (2-4 Myr), compact (~1 pc), and massive (${\sim}2{\times}10^4M_{\odot}$) star cluster located ~30 pc away from the Galactic center (GC) in projection. Being exposed to the extreme environment of the GC such as elevated temperature and turbulent velocities in the molecular clouds, strong magnetic fields, and larger tidal forces, the Arches cluster is an excellent target for understanding the effects of star-forming environment on the initial mass function (IMF) of the star cluster. However, resolving stars fainter than ~1 $M_{\odot}$ in the Arches cluster partially will have to wait until an extremely large telescope with adaptive optics in the infrared is available. Here we devise a new method to estimate the shape of the low-end mass function where the individual stars are not resolved, and apply it to the Arches cluster. This method involves histograms of pixel intensities in the observed images. We find that the initial mass function of the Arches cluster should not be too different from that for the Galactic disk such as the Kroupa IMF.

• 한국윤활학회:학술대회논문집
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• 한국윤활학회 2001년도 제33회 춘계학술대회 개최
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• pp.401-405
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• 2001

The effects of oxide layer formed on TiN coated ball and counter-body have been investigated from the frictional point of view during sliding tests. AISI52100 steel ball was used for the substrate of coated specimens. Two types of coated specimens were prepared by depositing TiN coating with 1 and 4$\mu\textrm{m}$ in coating thickness. AISI1045 steel was used for the disk type counter-body. To investigate the effect of oxide layer on the contact parts of two materials, the tests were performed both in ambient for forming oxide layer on the contact parts and in nitrogen environment to avoid oxidation.

• 천문학회보
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• 제46권1호
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• pp.51.1-51.1
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• 2021

Spiral arms greatly affect gas flows and star formation in disk galaxies. We use local 3D simulations of vertically-stratified, self-gravitating, gaseous disks under a stellar spiral potential to study the effects of spiral arms on galactic star formation as well as formation of gaseous spurs/feathers. We adopt the TIGRESS framework to handle radiative heating and cooling, star formation, and ensuing supernova (SN) feedback. We find that more than 90% of star formation takes place inside spiral arms. The global star formation rate (SFR) in models with spiral arms is enhanced by less than a factor of 2 compared to the no-arm counterpart. This supports the picture that spiral arms do not trigger star formation but rather redistribute star-forming regions. Correlated SN feedback produces interarm feathers in both magnetized and unmagnetized models. These feathers live short, have parallel magnetic fields along their length, and are bounded by SN feedback in the lateral direction, in contrast to instability-induced feathers formed in our previous isothermal simulations.

• 대한화장품학회지
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• 제32권3호
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• pp.201-208
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• 2006

본 연구는 예로부터 민간요법 및 한방에 유용한 약재로 사용되어지고 있는 관중(Dryopteris crassirhizoma Nakai)을 이용하여 Propionibacterium acnes에 대한 항균활성을 평가하고, 이를 토대로 여드름 억제 및 치료에 관련된 화장품 소재를 개발하는데 그 목적이 있다. P. acnes에 대한 관중 crude 추출물 및 헥산분획물의 minimum inhibitory concentration (MIC) 및 paper disk diffusion assay로 항균 효과를 측정하였으며, 추출물에 대한 온도 및 pH 변화에 따른 안정성을 평가하였다 추출물을 이용한 P. acnes에 대한 MIC 값은 관중 crude 추출물은 0.008 mg/mL, 헥산추출물은 0.001 mg/mL로 측정되었으며, 이는 대조군으로 사용한 항생제인 triclosan의 MIC 값(0.004 mg/mL)과 비교했을 때 시료가 관중 crude 추출물 및 헥산 분획물임을 고려하면 매우 항균활성이 높은 것으로 평가되었다. 추출물에 대한 paper disk diffusion assay를 수행한 결과, 대조군으로 사용한 triclosan과 대비, 높은 활성을 나타내는 것으로 측정되었으며, HaCaT 세포에 대한 독성은 $20{\mu}g/mL$ 이하의 농도에서는 나타나지 않았다. 관중추출물의 온도, pH 안정성을 평가한 결과, 25, 70, 80, 90, 100, $121^{\circ}C$ 등 다양한 온도 조건과 $pH 2{\sim}pH 11$의 변화에 있어서도 그 효능이 변하지 않고 안정된 상태로 유지되는 것으로 관찰되었다.

• 공업화학
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• 제20권3호
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• pp.317-321
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• 2009

고체 산화물 전해질로 사용되고 있는 초 이온 전도체인 $K^+-{\beta}/{\beta}"-Al_2O_3$의 고온 상관계와 소결성 분석을 위하여 $K_2O-LiO_2-Al_2O_3$ 삼성분계로부터 고상반응을 통하여 순수한 $K^+-{\beta}/{\beta}"-Al_2O_3$ 분말을 합성한 후 slip casting방법과 냉간정수압성형에 의하여 tube와 disk형을 각각 제작하였다. Slip casting은 40 wt%의 고체함량을 가지는 슬러리를 사용해 알루미나 몰드에서 이루어졌고 냉간정수압성형은 20 MPa의 압력하에서 수행되었다. 성형체들은 $1600^{\circ}C$, $1700^{\circ}C$, $1750^{\circ}C$에서 각각 소결하여 성형방법에 따른 상관계와 소결밀도를 조사하였다. 냉간정수압성형에 의한 시편이 $1700^{\circ}C$까지 ${\beta}"-Al_2O_3$의 상분율이 월등히 높은 반면, 소결밀도에 있어서는 slip casting방법의 경우가 다소 높았다. 소결 시 상대밀도는 $1750^{\circ}C$에서 1 h 경과 후, 두 경우 모두 약 83%를 나타내었다. 90 min 이상 소결하였을 때는 입자의 과대성장과 기공으로 인해 오히려 밀도가 낮아졌다.

• 대한소아치과학회지
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• 제49권3호
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• pp.321-328
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• 2022

이 연구는 Streptococcus mutans 바이오필름에 대한 에리스로신 매개 광역동 치료에서 potassium iodide (KI)의 효과를 평가하는 In vitro 실험이다. S. mutans ATCC 25175를 배양하여 hydroxyapatite disk에 바이오필름을 형성하였다. 광감각제인 에리스로신을 20 μM, KI를 각각 10, 50, 100 mM로 희석하여 적용한 뒤 광역동 치료를 시행하였다. 생존한 세균의 수는 colony forming units (CFU)/mL로 산정하였으며 Bonferroni 사후 분석을 통해 그룹 간 차이의 유의성을 확인하였다. Confocal laser scanning microscopy (CLSM)을 이용하여 세포 생존율을 시각적으로 평가하였다. 실험 결과 KI를 적용한 후 광역동 치료를 시행한 실험군에서 KI의 농도의 관계 없이 현저한 CFU의 감소가 관찰되었다(p < 0.05). 또한 10 mM KI에 비해 100 mM KI를 적용한 실험군에서 유의한 CFU의 감소가 관찰되었다(p < 0.05). CLSM 관찰 시에도 동일한 결과를 확인하였다. KI는 모든 농도에서 S. mutans 바이오필름에 대한 에리스로신 매개 광역동 치료의 효과를 유의하게 향상시켰다. 이는 바이오필름 상태의 균주에 대한 광역동 치료의 낮은 감수성을 보완할 수 있지만, 추가적인 연구를 통한 최적의 임상 프로토콜 확립이 필요하다.

• 천문학회지
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• 제38권2호
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• pp.249-252
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• 2005

We present results of the velocity-resolved spectroscopy of the [Fe II] $\lambda$1.644${\mu}m$ emission toward outflow sources with the Subaru Telescope at the angular resolution of 0.apos;16 ${\~}$ 0.apos;5 arcseconds. The observed sources are L1551 IRS 5, DG Tau, HL Tau and RW Aur, which are located in the Taurus-Aurigae Molecular Cloud, one of the closest star forming regions (0.apos;1 = 14 AU). We were able to resolve outflow structure in the vicinity of the sources at a scale of a few tens of AU. The position-velocity diagram of each object shows two velocity components: the high velocity component (HVC: 200 - 400 km $s^{-l}$) and the low velocity component (LVC: 50 - 150 km $s^{-l}$), which are clearly distinct in space and velocity. The HVC may be a highly collimated jet presumed from its narrow velocity width and high velocity. The LVC, on the other hand, may be a widely opened disk wind inferred from its broad velocity width and low velocity. The spectrum taken perpendicular to the L1551 IRS 5 outflow at its base shows that the LVC has a spatially wide subcomponent, supporting the above interpretation. We demonstrated that the [Fe II] 1.644 $\mu$ spectroscopy is a very powerful tool for the studies of fast jets and winds that directly emanate from star-disk systems.

• 천문학회보
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• 제39권1호
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• pp.56.2-56.2
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• 2014

We present [Fe II] 1.64 ${\mu}m$ imaging observations for jets and outflows from young stellar objects over the northern part (${\sim}24^{\prime}{\times}45^{\prime}$) of the Carina Nebula, a massive star forming region. The observations were performed with IRIS2 of Anglo-Australian Telescope and the seeing was ~1.5". Eleven jets and outflows features are detected at eight different regions, and are termed as Ionized Fe Objects (IFOs). The [Fe II] features have knotty or elongated shapes, and the detection rate of IFOs against previously identified YSOs is 1.4%. Four IFOs show anti-correlated peak intensities in [Fe II] and $H{\alpha}$, where the ratio I([Fe II])/I($H{\alpha}$) is higher for longish IFOs than for knotty IFOs. We estimate the outflow mass loss rate from the [Fe II] flux using two different methods. The jet-driving objects are identified for three IFOs (IFO-2, -4, and -7). The ratios of the outflow mass loss rate over the disk accretion rate for IFO-4 and -7 are consistent with the previously reported values ($10^{-2}-10^{+1}$), while the ratio is higher for IFO-2. This excess may result from underestimating the disk accretion rate. Other YSO physical parameters show reasonable relations or trends.

• 천문학논총
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• 제30권2호
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• pp.645-647
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• 2015

We have initiated a Very Long Baseline Interferometer (VLBI) monitoring project of 36 methanol maser sources at 6.7 GHz using the Japanese VLBI Network (JVN) and East-Asian VLBI Network (EAVN), starting in August 2010. The purpose of this project is to systematically reveal 3-dimensional (3-D) kine-matics of rotating disks around forming high-mass protostars. As an initial result, we present proper mo- tion detections for two methanol maser sources showing an elliptical spatial morphology, G 002.53+00.19 and G 006.79-00.25, which could be the best candidates associated with the disk. The detected proper motions indicate a simple rotation in G 002.53+00.19 and rotation with expansion in G 006.79-00.25, respectively, on the basis of disk model fits with rotating and expanding components. The expanding motions might be caused by the magnetic-centrifugal wind on the disk.