• International Journal of Oral Biology
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• 제46권4호
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• pp.160-167
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• 2021

Nypa fruticans Wurmb (NFW) contains a large amount of phenolic acid and flavonoids, and is popular as a superfood in Myanmar. NFW has various biological activities, such as anti-inflammatory, anti-oxidant, and neuroprotective properties; however, the anti-cancer effect of NFW have not been reported. In this study, we investigated the anticancer activity of water extracts of NFW (WeNFW) and the underlying mechanism in human FaDu hypopharyngeal squamous carcinoma cells. The WeNFW inhibited FaDu cell growth in a dose-dependent manner without affecting normal cells (L929), as determined by an MTT assay and Live and Dead assay. In addition, the concentrations of WeNFW without cytotoxicity (0.025, 0.05, and 0.1 mg/mL) inhibited wound healing and colony formation. Furthermore, WeNFW significantly induced apoptosis through the proteolytic cleavage of caspase-3 and -9, poly (ADP-ribose) polymerase, and downregulation of Bcl-2 and upregulation of Bax in FaDu cells, as determined by DAPI staining, FACS analysis, and western blot analysis. Taken together, these results suggest that WeNFW exhibits potent anti-cancer effects by suppressing the growth of oral cancer cells, wound healing and colony formation activity. Via mitrochondrial-dependent apoptotic pathways in human FaDu hypopharyngeal squamous carcinoma cells. Therefore, WeNFW can provide a natural chemotherapeutic drug for oral cancer in humans.

• 한국가금학회지
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• 제35권4호
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• pp.391-398
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• 2009

본 시험은 4가지의 유도환우 방법을 이용한 환우 후의 산란계의 생산성을 비교 검토하기 위해 수행하였다. 공시계는 산란율 80% 이상, 평균 체중 $16{\pm}0.3\;kg$의 62주령 White Leghorn 120수를 공시하였다. 4가지 환우 방법은 ; 1) 환우 시험 개시 후 10일째까지 절식, $11{\sim}13$일째 제한 급이, 14일째부터 고에너지 사료 자유 급이 (FW1), 2) 저에너지 사료 자유 급이 (FW2), 3) 환우용 사료를 26일째까지 일일 수당 60 g, 27일째부터 28일째까지 일일 수당 90 g씩 제한 급이(NFW1), 4) 환우용 사료 자유 급이. 처리구는 4종류의 환우 방법에 대조구를 포함하여 총 5처리구를 설정하였으며, 처리구당 2반복, 반복당 12수씩 완전임의 배치하였다. FW1과 FW2 처리구는 환우 처리 후 $3{\sim}4$일째에 산란이 완전정지하였으며, NFW1과 NFW2 처리구는 $16{\sim}18$일째에 산란의 거의 정지하였다. 산란율의 회복은 NFW2구가 28일, NFW1구가 30일부터 재 산란이 시작되고, 각각 38일과 41일째에 산란이 50%에 이르렀으며, 54일, 62일째에 각각 산란율 80% 이상을 유지하였다. 이것과 비교하여 환우 처리 후, 저에너지 사료 급이구 FW1와 고에너지 사료 급이구 FW2구는 산란율의 회복이 FW1구가 28일, FW2구가 26일부터 재 산란이 시작되고, 각각 47일과 41일째에 산란율이 50%에 이르렀으며, 70일, 64일째에 각각 산란율 80% 이상을 유지하였다. 환우 14일째간의 무게는 27.6과 32.2 g, 난포수란관의 무게는 22.0과 24.9 g으로 환우처리구에서 무게가 크게 감소하였다(P<0.05). 환우 후 계란 품질은 환우 처리구에서 난중, 난각 두께, 난각 강도 및 하우유니트가 개선되었으나(P<0.05), 난황색은 차이가 없었다(P>0.05).

• 한국생물환경조절학회:학술대회논문집
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• 한국생물환경조절학회 2003년도 춘계 학술대회 논문집
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• pp.112-118
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• 2003

분화 양액 재배에 있어서 저면 관수 방식은 두상 관수 방식 보다 더 널리 사용되고 있다. 저면 관수 방식의 장점으로는 지상부에 물이 닿지 않아 고품질의 식물체 생산 가능, 균일한 크기의 식물체 생산 가능, 물과 양분의 사용의 줄임 등이 있다 (Newman, 1999). 현재 유럽은 저면 관수방식의 대표적인 ebb-and-flow 시스템이 상용화 되어있으며, 북미에서도 점점 그 사용 비율이 증가하고 있다 (Biernbaum, 1990). (중략)

• 천문학회보
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• 제42권2호
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• pp.73.3-73.3
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• 2017

Environment has a significant impact on the evolution of dark halo profiles. We used a cosmological N-body simulation based on WMAP5 cosmology to study environmental effects on halo profiles. Host haloes located in sparse regions are highly concentrated, and more massive haloes have higher concentration index. This is because mass accretion affects only the outer part of the halo and consequently increase the virial radius having no effect on the scale radius. Conversely, host haloes located in dense regions have low concentration index. This is because frequent mergers affect even the inner part of the halo. So, scale radius increases with the growth of virial radius. Evolutions of subhalo profiles are essentially different from those of host haloes because subhaloes undergo tidal stripping. The stripping begins once a subhalo approaches closer than ~3 virial radii of the host halo. During the stripping, the inner part of the subhalo keep following NFW profile, but the mass of the outer part gradually decreases. As a result, when the subhalo reaches the pericenter of its host, only about inner 30% of the subhalo follows the NFW profile.

• 천문학회보
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• 제36권1호
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• pp.47.1-47.1
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• 2011

We studied the evolution of the two mass components system with NFW initial density distribution by direct integration of the Fokker-Planck equations. The low mass component is regarded the dark matter particles while the high mass component is assumed to be conglomerates of baryonic matter in order to depict the 'stars'. While the true mass ratio between these two types of particles should be extremely large, our adopted mass ratio is about 1000 beyond which the dynamical evolution and density distribution tend to converge. Since the dynamical evolution is dominated by the dynamical friction, the high mass component slowly moves toward the central part, and eventually undergoes the core collapse. The system reaches the core-collapse at about $7.1{\times}10^{-3}$ $t_{fh}$ in NFW models, where $t_{fh}$is the dynamical friction time at half-mass radius. The distribution of the high mass component is well fitted by the Sersic profiles or modified Hubble profile when the mass segregation is established. From these results, the surface brightness of elliptical galaxies may be explained by the high mass component experiencing dynamical friction by the dark matter particles. In order for the mass segregation to be effective within Hubble time, the mass of the luminous component should be greater than $10^5M_{\bigodot}$.

• 천문학회지
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• 제46권1호
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• pp.1-32
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• 2013

We construct several Milky Way-like galaxy models containing a gas halo (as well as gaseous and stellar disks, a dark matter halo, and a stellar bulge) following either an isothermal or an NFW density profile with varying mass and initial spin. In addition, galactic winds associated with star formation are tested in some of the simulations. We evolve these isolated galaxy models using the GADGET-3 N-body/hydrodynamic simulation code, paying particular attention to the effects of the gaseous halo on the evolution. We find that the evolution of the models is strongly affected by the adopted gas halo component, particularly in the gas dissipation and the star formation activity in the disk. The model without a gas halo shows an increasing star formation rate (SFR) at the beginning of the simulation for some hundreds of millions of years and then a continuously decreasing rate to the end of the run at 3 Gyr. Whereas the SFRs in the models with a gas halo, depending on the density profile and the total mass of the gas halo, emerge to be either relatively flat throughout the simulations or increasing until the middle of the run (over a gigayear) and then decreasing to the end. The models with the more centrally concentrated NFW gas halo show overall higher SFRs than those with the isothermal gas halo of the equal mass. The gas accretion from the halo onto the disk also occurs more in the models with the NFW gas halo, however, this is shown to take place mostly in the inner part of the disk and not to contribute significantly to the star formation unless the gas halo has very high density at the central part. The rotation of a gas halo is found to make SFR lower in the model. The SFRs in the runs including galactic winds are found to be lower than those in the same runs but without winds. We conclude that the effects of a hot gaseous halo on the evolution of galaxies are generally too significant to be simply ignored. We also expect that more hydrodynamical processes in galaxies could be understood through numerical simulations employing both gas disk and gas halo components.

• 한국생물환경조절학회:학술대회논문집
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• 한국생물환경조절학회 2007년도 춘계 학술대회 및 정기총회
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• pp.119-122
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• 2007

• 산업경영시스템학회지
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• 제32권4호
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• pp.124-127
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• 2009

When multiple rates of return occur, none of them is an accurate portrayal of project acceptability or profitability. For the simple investment situation, it was known that the IRR can serve as an appropriate index for either accepting or rejecting the investment. But, in this situation, we present that the IRR criterion is not same to DCF criterion. On the contrary we can easily show that the RRR criterion is completely consistent with the DCF criterion. Thus, the RRR is very well match for an accurate portrayal of project acceptability or profitability.

• 천문학회지
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• 제38권2호
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• pp.191-195
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• 2005

We used Subaru observations of A1689 (z = 0.183) to derive an accurate, model-independent mass profile for the entire cluster, r$\le$2Mpc/h, by combining magnification bias and distortion measurements. The projected mass profile steepens quickly with increasing radius, falling away to zero at r${\~}$1.0Mpc/h, well short of the anticipated virial radius. Our profile accurately matches onto the inner profile, r $\le$200kpc/ h, derived from deep HST / ACS images. The combined ACS and Subaru information is well fitted by an NFW profile with virial mass, $(1.93 \pm 0.20) {\times}10^{15} M_{\bigodot}$, and surprisingly high concentration, $C_{vir} = 13.7^{+1.4}_{-1.1}$, significantly larger than theoretically expected ($C_{vir} {\le}4$), corresponding to a relatively steep overall profile. These results are based on a reliable sample of background galaxies selected to be redder than the cluster E/SO sequence. By including the faint blue galaxy population a much smaller distortion signal is found, demonstrating that blue cluster members significantly dilute the true signal for r $\le$ 400kpc/ h. This contamination is likely to affect most weak lensing results to date.

• 천문학회보
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• 제42권1호
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• pp.51.2-51.2
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• 2017

Diffuse radio relics are often detected in merging galaxy clusters and are emitted by synchrotron process. Radio relics are believed to trace the shock waves in the intracluster medium induced by ram pressure during a major cluster merger. Radio halos and relics are found in approximately 50 galaxy clusters to date that are all in a state of merging. The rarest of these galaxy clusters contain pairs of relics of similar brightness as well as a radio halo. The massive galaxy cluster PLCKG287.0+32.9 belongs to this rare population and is the second most significant detection from the Planck SZ All-sky Survey. Perhaps even more intriguing is that the radio relics are observed at vastly different distances from the X-ray peak requiring a complex merging scenario. In this study, we use weak-lensing to peer deeper into the merging scenario by reconstructing the dark matter distribution. We relate the mass distribution to the radio, X-ray, and optical emissions to provide constraints for future simulations of the merger. Fitting an NFW profile to the tangential shear we infer the mass of the cluster and discuss its implications for the merging scenario.