• 공업화학
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• 제20권6호
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• pp.628-631
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• 2009

최근 광우병 파동과 프리온 단백질의 전염으로 인하여 발생되는 것으로 알려진 크로이츠펠트 야콥병에 대하여 폭넓게 연구되면서 생화학계에서 프리온 단백질에 대한 관심은 상당하다. 본 연구에서는 프리온 단백질의 일부분인 PrP 106-126의 마이크로 몰농도 단위의 정량분석을 실시하였다. 본 연구에서 플로래스카민은 일차 아민과 반응하여 형광을 띠는 물질로써, 알파이미저는 형광의 세기를 측정하는 기기로써 사용되었다. 따라서 합성된 PrP 106-126으로 플로래스카민과 알파이미저를 이용하여 마이크로 몰농도단위의 정량 분석을 위한 조건을 정립하였으며 이를 통하여 표준곡선을 얻을 수 있었다. 이 방법은 차후 변형 프리온 단백질에 대한 응집저해제 및 의약품 연구에 큰 기여를 할 것이다.

• 대한원격탐사학회지
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• 제29권2호
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• pp.173-182
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• 2013

천리안 위성 해양탑재체(Geostationary Ocean Color Imager, GOCI) 대기보정의 근간이 되는 Sea-viewing Wide Field-of-view Sensor(SeaWiFS) 초기 대기보정 기법은 근적외선 파장대의 해수 반사도를 0으로 가정한다. 이러한 가정에 근거하여 근적외선 파장에서 탐지되는 모든 신호는 에어로졸 산란에 의한 반사도로 간주된다. 그러나 이러한 가정은 탁한 해역에서 해수 반사도를 과소 추정하는 문제점을 야기시킨다. 이를 해결하기 위하여 Management Unit of the North Sea Mathematical Models(MUMM) 대기보정 알고리즘이 개발되었다. 이 알고리즘은 근적외선 파장에서 탐지되는 해수 반사도 비율인 ${\alpha}$를 도입하였다. ${\alpha}$는 통계적 방법에 의하여 결정되며 영상 내의 모든 픽셀에 고정적인 값으로 사용된다. 이 알고리즘은 근적외선 해수 반사도가 0.01보다 작은 중간 탁도의 해역에서는 잘 맞는 반면 매우 탁한 해역에서는 ${\alpha}$가 탁도에 따라 변하기 때문에 오차율이 다시 증가한다. 본 연구에서는 매우 탁한 해역 해수 반사도의 정확도를 향상시키고자 ${\alpha}$를 고정하지 않고, 반복계산을 통해 탁도에 적합한 ${\alpha}$를 계산하도록 MUMM 알고리즘을 수정 보완하였다. 그 결과 MUMM 알고리즘의 모든 밴드의 평균 Root Mean Square Error(RMSE)는 0.0048인 반면 수정된 MUMM 알고리즘은 0.002로 개선된 결과를 얻었다.

• 천문학회지
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• 제37권4호
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• pp.211-216
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• 2004

We present the results of an H I aperture synthesis mosaic of the Large Magellanic Cloud (LMC), made by combining data from 1344 separate pointing centers using the Australia Telescope Compact' Array (ATCA) and the Parkes multibeam receiver. The resolution of the mosaiced images is 50" (<15 pc, using a distance to the LMC of 55kpc). This mosaic, with a spatial resolution .15 times higher than that which had been previously obtained, emphasises the turbulent and fractal structure of the ISM on the small scale, resulting from the dynamical feedback of the star formation processes with the ISM. We also have done a widefield panoramic survey of H$\alpha$ emission from the Magellanic Clouds with an imager mounted on the 16-inch telescope at Siding Spring Observatory. This survey produced H$\alpha$ images which are equal to the ATCA survey in area coverage and resolution. This survey allows us to produce a continuum-subtracted image of the entire LMC. In contrast with its appearance in the H$\alpha$ image, the LMC is remarkably symmetric in H I on the largest scales, with the bulk of the H I residing in a disk of diameter 8. $^{\circ}4$ (7.3 kpc) and a spiral structure is clearly seen. The structure of the neutral atomic ISM in the LMC is dominated by H I filaments combined with numerous shells and holes.

• 천문학회보
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• 제42권2호
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• pp.61.2-61.2
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• 2017

We report a fine scale transient brightening event near a pore boundary with the Fast Imaging Solar Spectrograph (FISS) of the 1.6m Goode Solar Telescope (GST), the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO), and Helioseismic and Magnetic Imager (HMI) aboard SDO. The event appears in all AIA extreme ultraviolet bands, also in the two FISS lines, $H{\alpha}$ and Ca II $8542{\AA}$, and lasted for a minute. The brightening occurred at a footpoint of a loop. The conjugate brightening occurred at the other foot point outside the FISS field of view. The brightening near the pore exhibit a redshift of 4.3 km s-1 in the $H{\alpha}$ and about 2.3 km s-1 in Ca II line. Differential emission measure derived from 6 AIA EUV passbands and cloud model fitting of the two FISS lines indicate the temperature increase of between 10,000 and 20 MK at the main event. After the brightening, the upward mass motion appears in the AIA images. We discuss the physical implication of this brightening in the context of magnetic reconnection and coronal heating.

• 천문학회보
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• 제38권2호
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• pp.86.1-86.1
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• 2013

Observations of a filament showing an activated barb recorded from the at the Dutch Open Telescope (DOT) on 2010 August 20 are presented. The filament developed a barb in 10 minutes, which disappeared within the next 35 minutes. Such a rapid formation and disappearance of a filament barb is unusual, and has been seldom reported. Line-of-sight velocity maps were constructed from images in seven line positions along the H-alpha line. We observe flows in the filament spine towards the barb location prior to its formation, and flows in the barb towards the spine during its disappearance. Photospheric magnetograms from Helioseismic Magnetic Imager on board the Solar Dynamics Observatory were used to determine the changes in magnetic flux in the region surrounding the barb location. The variation of magnetic flux in this duration support the view that barbs are rooted in minor magnetic polarity.

• 대한원격탐사학회지
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• 제18권4호
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• pp.187-199
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• 2002

해수광 특성이 시공간적으로 심하게 변동하는 동중국해 북부해역에서 현장 클로로필 $\alpha$와 OSMI 밴드(412, 443, 490, 555nm) 및 해수 다중 광측정기(PRR-800) 밴드(412, 443, 490, 510, 555, 670, 765nm)간의 관계성을 구한 결과, 클로로필 $\alpha$에 대한 각 밴드별 remote sensing reflectance (Rrs) 값이 맑은 해수(미국 캘리포니아 근해)에서 보다 동중국해 북부해역에서 크게 나타났다. 또한 440nm와 670nm 영역에서 현장 관측 클로로필 $\alpha$에 대한 입자 물질들의 광흡수 값이 맑은 해수의 경우보다 큰 값을 보였다. 그러므로, OSMI밴드에서 클로로필로 인해 최대 흡수가 일어나는 밴드가 443nm을 추정할 수 있었다. 동중국해를 관측한 OSMI 위성의 각 band (412, 443, 490, 555 nm)로부터 nLw (normalized water-leaving radiance)와 현장 클로로필 $\alpha$(Chl $\alpha$)값의 관계성(Chl $\alpha$= f(nLw)을 구하였다. OSMI 밴드에서 클로로필 $\alpha$ 값과 각 밴드별 nLw 값과의 상관성은 412nm에서 최저 상관성을, 555nm에서 최고 상관성을 나타내었다. 클로로필 $\alpha$ 현장 관측 값 및 OSMI 복합밴드 비 값(nLw412/nLw555, nLw443/nLw555, nLw490/nLw555)을 비교 분석한 결과, nLw490/nLw555 비 값과 현장 클로로필 $\alpha$ 값간에 최고 높은 상관성을 나타내었다. 다음으로 nLw443/nLw555 순으로 안정된 값을 보였으나, nLw412/nLw555와 클로로필 $\alpha$ 값간의 상관성이 가장 낮게 나타났다. 3시간이내 현장 측정 클로로필 $\alpha$ 값을 기준으로 OSMI 및 SeaWiFS 위성 자료를 OC2 알고리즘을 이용하여 추정한 클로로필 값간의 차이는 해양의 수평 공간 변동에 관계없이 OSMI 추정 값이 약 0.3mg/m$^3$ 정도 일정하게 낮게 나타났다. 향후 OSMI 위성 밴드를 이용한 클로로필 $\alpha$ 추정시에는 SeaWiFS 위성과 관련된 global algorithms 중에서 490nm와 555nm의 복합밴드를 포함하는 OC2 알고리즘(ocean color chlorophyll 2 algorithm)을 사용하는 것이 OC2 series 및 OC4 알고리즘보다 좋은 추정 값을 도출할 수 있을 것으로 기대된다.

• 대한화장품학회:학술대회논문집
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• 대한화장품학회 2003년도 IFSCC Conference Proceeding Book I
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• pp.162-177
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• 2003

It has been known that the color of skin reflects the blood flow within. In lips, the capillaries close to the skin surface are numerous; hence lips are redder than the rest of face. However, dermatological research on lips is not as advanced as research on facial or body skin, and little was known about the relationship between relatively dull-colored lips and skin blood flow. The physiological differences between colorful and dull-colored lips were studied by a two-dimensional laser Doppler blood flow analyzer, a spectrometer for the measurement of the degree of oxygen saturation, and a confocal microscope for observing inside lips non-invasively. Dull-colored lips and the corner of lips (dull-colored compared to the center) showed relatively poor blood flow and lower oxygenated hemoglobin. It was found that colorful lips (generally the young) had a blood flow that tended to run straight in parallel with the skin surface. This unique blood-capillary structure can express clear red blood. Those with dull-colored lips had lost this unique structure. Their blood ran perpendicularly from the deep of the skin and down back again into the deep part as like the blood circulation patterns of facial skin. Therefore, the lips of the latter group had fewer blood capillaries near skin surface in the lips than that of the colorful-lips group. A lipstick containing a-glucosyl-hesperidin, which is derived from certain citrus fruits and can enhance blood circulation, was applied for evaluating its effects. Blood flow was increased 30 min after the application. After two weeks of daily application, the lips' condition became noticeably less dull. These findings suggest that the decrease of blood flow in dull-colored lips is caused by the loss of the unique capillary structure and the use of the lipstick to increase blood flow can give a vivid color to lips.

• 천문학회보
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• 제42권2호
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• pp.50.2-50.2
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• 2017

Spatial distribution of atmosphereless bodies in the solar system provides an important clue as to their origins, namely asteroids from Mainbelt or comets from outer solar system. It is, however, difficult to distinguish asteroids and dormant comets due to their similar appearances. In this study, we conducted a unique observation to differentiate asteroids and dormant comets in terms of 'polarimetry'. We observed (331471) 1984 QY1 (hereafter QY1) at large phase angles using the Multi-Spectral Imager (MSI) on the 1.6-m Pirka Telescope from UT 2016 May 25 to June 24. QY1 is a dormant comet candidate in terms of the dynamical properties (i.e. the Tisserand parameter with respect to Jupiter, TJ = 2.68). We analyzed the polarization degree of QY1 as a function of phase angle and found its maximum polarization degree, $Pmax=8.68{\pm}0.28%$ and $8.72{\pm}0.38%$, in RC-and V-band, respectively, around the phase angle of ${\alpha}=100^{\circ}$. In addition, we obtained the geometric albedo, $pV=0.16{\pm}0.02$ by means of an empirical slope-albedo law. The polarimetric properties and the albedo value we acquired are similar to those of S-type asteroids rather than cometary nuclei. In this presentation, we introduce our observation and findings. In addition, we further discuss a dynamical transportation process from Mainbelt to the current orbit.

• 천문학회보
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• 제35권1호
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• pp.27.2-27.2
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• 2010

We have studied the formation of coronal holes (CHs) associated with halo CMEs. For this study, we used multi-wavelength data from Yohkoh Soft X-ray Telescope (SXT), GOES Soft X-ray Imager (SXI), SOHO EIT 195 ${\AA}$, SOHO MDI magnetogram, MLSO He I 10830 ${\AA}$, and BBSO H-alpha. The CHs are characterized by open magentic field regions with low emission, density, and temperature and their open fields drive high speed solar winds which cause geomagnetic storms. So far, the formation and the evolution of CHs are not well understood. The formation of the dark region associated with the eruption of a CME is well known as "coronal dimming" which may be caused by the mass depletion near the CME footpoint. It is different from a typical CH since it persists for only one or two days. In this study, we present three cases that show the formation of coronal holes which are associated with three halo CMEs: 1) 2000 Jul 14, 2) 2003 Oct 28, 3) 2005 May 13. In the first case, hot plasma was ejected during a weak eruption and then filled out the pre-existing CH. After the halo CME occurred, the hot plasma region becomes a CH again. In the second and the third cases, we found newly formed CHs just after their associated CMEs. All three coronal holes are associated with strong flares and persist over 3 days until they disappeared by the solar rotation. Examining the MDI magnetograms, we found that the magnetic polarity of each CH region has one polarity. Based on these results, we suggest that the coronal holes can be formed by the CMEs and they should be distinguished from the coronal dimming.

• 천문학회지
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• 제37권1호
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• pp.41-53
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• 2004

It has been a big mystery what drives filament eruptions and flares. We have studied in detail an X1.8 flare and its associated filament eruption that occurred in NOAA Active Region 9236 on November 24,2000. For this work we have analyzed high temporal (about 1 minute) and spatial (about 1 arcsec) resolution images taken by Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory, Hoc centerline and blue wing ($-0.6{\AA}$) images from Big Bear Solar Observatory, and 1600 ${\AA}$ UV images by the Transition Region and Corona Explorer (TRACE). We have found that there were several transient brightenings seen in H$\alpha$ and, more noticeably in TRACE 1600 ${\AA}$ images around the preflare phase. A closer look at the UV brightenings in 1600 ${\AA}$ images reveals that they took place near one end of the erupting filament, and are a kind of jets supplying mass into the transient loops seen in 1600 ${\AA}$. These brightenings were also associated with canceling magnetic features (CMFs) as seen in the MDI magnetograms. The flux variations of these CMFs suggest that the flux cancellation may have been driven by the emergence of the new flux. For this event, we have estimated the ejection speeds of the filament ranging from 10 to 160 km $s^{-1}$ for the first twenty minutes. It is noted that the initiation of the filament eruption (as defined by the rise speed less than 20 km $s^{-1}$) coincided with the preflare activity characterized by UV brightenings and CMFs. The speed of the associated LASCO CME can be well extrapolated from the observed filament speed and its direction is consistent with those of the disturbed UV loops associated with the preflare activity. Supposing the H$\alpha$/UV transient brightenings and the canceling magnetic features are due to magnetic reconnect ion in the low atmosphere, our results may be strong observational evidence supporting that the initiation of the filament eruption and the preflare phase of the associated flare may be physically related to low-atmosphere magnetic reconnection.