• Journal of Astronomy and Space Sciences
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• v.18 no.1
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• pp.55-62
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• 2001

We present VRI CCD photometry of W UMa type binary TY UMa. The light curves show that the secondary minimum is deeper than the primary minimum and the maximum I ($0.^{p}25$)is $0.^{m}023$ brighter than the maximum II ($0.^{p}75$). The V light curve has been analyzed and the photometric solutions have been determined by the method of Wilson & Devinney differential correction. We adopted the spot model to explain the asymetric light curve.

• The Korean Journal of Physiology
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• v.17 no.1
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• pp.1-11
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• 1983

1) The two microelectrode method was used to voltage clamp small preparations of rabbit sinoatrial node. The kinetics of hyperpolarization activated inward current, $i_f$ were analysed. 2) The hrperpolarization pulses activated $i_f$ current in the presence of $10^{-7}g/ml$ TTX and 2 mM $Mn^{2+}$. The activation range was in between -45 mV to -75 mV. The current magnitude was increased and time course was faster by strong hyperpolarization pulses. 3) Standard envelope tests indicated that this current is exponentially controlled by single gate. 4) Semilogarithmic plot of $i_f$ activation versus time was found to be linear in the activation range. The decrease in current magnitude and the shifts in activation curve and rate constants curve to the hyperpolarizing direction were obtained with $Ba^{2+}$, indicating that $Ba^{2+}$ shifts the voltage dependence of the gating kinetics, were partially reversed by 24 mM $K^+$.

• Journal of Sensor Science and Technology
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• v.8 no.5
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• pp.388-393
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• 1999

In this study, the $CaSO_4:Eu$ TLDs are fabricated and their trap parameters are determined. The optimum concentration of Eu for fabrication of the $CaSO_4:Eu$ TLD is 0.5 mol% and optimum temperature is $600^{\circ}C$ for 2 hours sintering in air. The glow curve of $CaSO_4:Eu$ consists of two glow peaks and these peaks are isolated by thermal bleaching method. Trap parameters of two glow peaks are measured using the initial rise, the peak shape, the heating rate and the least square curve fitting methods. The activation energies of the glow peak I and II are 1.00 eV and 1.09 eV, and the frequency factors are $7.04{\times}10^{11}\;s^{-1}$ and $5.12{\times}10^{11}\;s^{-1}$ and the kinetic orders are 1.11 and 1.33, respectively.

• Journal of Sensor Science and Technology
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• v.9 no.5
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• pp.341-349
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• 2000

CsI(Br) single crystals doped with 1, 3, 5 or 10 mole% $Br^-$ ions, as an activator, were grown by Czochralski method. The lattice structure of grown CsI(Br) single crystal was bcc and its lattice constant was $4.568\;{\AA}$. The absorption edge of the CsI(Br) single crystals was observed at 243 nm. The spectral range of the luminescence excited by 243 nm of wavelength was $300{\sim}600\;nm$, and its peak emission appeared at 440 nm. The luminescence intensity was maximum when CsI(Br) was doped with 3 mole % $Br^-$ ions. The energy resolutions of the CsI(Br) scintillator doped with 3 mole % $Br^-$ ions were 15.0% for $^{137}Cs$(662 keV), 13.1% for $^{54}Mn$(835 keV), and 18.0% and 6.3% for $^{22}Na$(511 keV and 1275 keV), respectively. The decay curves had fast and slow components, and the fast component was about 41 ns independent on the concentration of the $Br^-$ ions. The time resolution of CsI(Br) scintillators decreased with increasing of the concentration of $Br^-$ ions.

• Journal of Sensor Science and Technology
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• v.8 no.5
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• pp.359-367
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• 1999

CsI(Li) single crystals doped with 0.02, 0.1, 0.2 and 0.3 mole% lithium as an activator were grown by Czochralski method. The lattice structure of grown CsI(Li) single crystal was bcc, its lattice constant was $4.568\;{\AA}$. The absorption edge of CsI(Li) single crystal was 245 nm, and the spectral range of luminescence was $300{\sim}600\;nm$, its maximum luminescence intensity appeared at 425 nm. The energy resolutions of CsI(Li) single crystal doped with 0.2 mole% lithium were 14.5% for $^{137}Cs$(662 keV), 11.4% for $^{54}Mn$(835 keV) and 17.7% and 7.9% for $^{22}Na$(511 keV and 1275 keV), respectively. The relation formula of $\gamma$-ray energy versus energy resolution was ln (FWHM%) = -0.893lnE + 8.456 and energy calibration formula was ${\log}E_r=1.455\;{\log}(ch.)-1.277$. The phosphorescence decay time of CsI(Li) crystal doped with 0.2 mole% lithium was 0.51 s at room temperature, and its time resolution measured by CFT(constant-fraction timing method) was 9.0 ns.

• Journal of Astronomy and Space Sciences
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• v.15 no.2
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• pp.335-340
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• 1998

We obtained UV light curves of 44i Bootis, a W UMa type star from the IUE low dispersion spectra. In order to investigate variations of the emission lines from chromospheric activity and transition region, UV line intensity has been measured for CI, CII, ClV, SiIV, HeII lines. Through plotting the line intensity with the orbital phase, we found that emission lines showed maximum at $0^p.2;and;0^p.8$ of the light curves, indicating the chromospheric activity of contact binary, 44i Bootis. We found that the light curves of UV emission lines is strongly modulated by the variation of chromospheric activities of 44i Bootis.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.1
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• pp.60.1-60.1
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• 2012

구경 3.6m의 캐나다-프랑스-하와이 망원경(Canada-France-Hawaii Telescope, CFHT)의 주 초점에 설치된 CFH12K CCD 카메라를 이용하여 늙은 산개성단 NGC 1245와 NGC 2506에 대한 V와 I필터를 이용한 CCD측광을 수행하였다. 관측된 영역은 NGC 1245는 84'${\times}$82', NGC 2506은 42'${\times}$81'이고, 한계등급 V ${\approx}$ 23등급까지 관측하였다. 이론적인 등연령곡선을 사용하여 NGC 1245와 NGC 2506에 대해 각각 물리량 E(B-V) = 0.2, 0.03, (V-M_V)_0 = 12.5, 12.5, log(age) = 9.0, 9.3으로 구하였다. 이로부터 MV ${\approx}$ 10등급까지의 광도함수와 질량함수를 구하였다. NGC 1245와 NGC 2506의 질량함수의 기울기를 각각 ${\Gamma}$ = -1.26${\pm}$0.04, ${\Gamma}$ = -1.27${\pm}$0.07로 얻었고, 이들의 기울기는 태양부근의 낱별의 질량함수의 기울기에 비해 완만하다. 이는 성단에서 질량이 작은 별들의 질량 증발에 의한 역학적 진화의 효과로 보인다. 본 발표에서는 관측 내용과 그 결과를 소개하고자 한다.

• Electrical & Electronic Materials
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• v.1 no.3
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• pp.269-277
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• 1988

P형 Si(100)로 제작한 MOS 커패시터에 $Co^{60}$-.gamma.선을 주사한 후 고주파 C-V특성 곡선으로 부터 방사선 조사에 의해 유발된 산화막안의 트랩전하의 거동 및 Si- $SiO_{2}$계면에서의 트랩밀도 분포의 변화를 검토하였다. 산화막 느랩전하는 .gamma.선 흡수선량 증가와 더불어 증가하다가 $10^{7}$ rad 부근에서부터 서서히 포화하는 경향이 나타났으며 게면트랩밀도의 분포모양은 흡수선량의 증가와 더불어 전형적인 이그러진 W자형에서 넓혀진 V자형 분포로 변화하였으나 최소값은 항상 진성페르미준위( $E_{i}$)부근에 있었으며 그 밀도는 1.0*$10^{11}$~7.5*$10^{11}$[개/$cm^{2}$/eV]로 계산되었다. 또한, 일정 바이어스전압하에서의 조사선량에 따른 $V_{fb}$ 의 변화는 현저하지는 않았으나 바이어스 전압을 +12V로 인가할 때 변화방향의 반전상태가 관측되었다. 그 이유로는 Si측의 계면 부근에서 일어난 눈사태 전자가 산화막내로 주입됨에 따라 도너형 양전하의 수가 감소되기 때문으로 추정되었다.되었다.

• Journal of Korea Society of Industrial Information Systems
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• v.17 no.7
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• pp.51-57
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• 2012

This paper proposes a group key design based on ECDH(Elliptic Curve Diffie Hellman) which guarantees secure V2V and V2I communication. The group key based on ECDH generates the VGK(Vehicular Group key) which is a group key between vehicles, the GGK(Global Group Key) which is a group key between vehicle groups, and the VRGK(Vehicular and RSU Group key) which is a group key between vehicle and RSUs with ECDH algorithm without an AAA server being used. As the VRGK encrypted with RGK(RSU Group Key) is transferred from the current RSU to the next RSU through a secure channel, a perfect forward secret security is provided. In addition, a Sybil attack is detected by checking whether the vehicular that transferred a message is a member of the group with a group key. And the transmission time of messages and the overhead of a server can be reduced because an unnecessary network traffic doesn't happen by means of the secure communication between groups.

• Journal of Astronomy and Space Sciences
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• v.24 no.2
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• pp.99-110
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• 2007

A total of 824 observations (206 in ${\Delta}B$, 206 in ${\Delta}V$, 206 in ${\Delta}R$, 206 in ${\Delta}I$ for CC Com were made on 3 nights from March 3 to April 3 in 2002 using the 61cm telescope with 2K CCD camera of the Sobaeksan Optical Astronomy Observatory of KASI. From our observations 9 times of minimum light were newly determined. Combined analysis of our new BVRI light curves with the double-lined radial velocity curves of Pribulla et al. (2007) were made with the 2004 Wilson-Devinney(WD) binary model code to yield new physical parameters of the CC Com system. Small asymmetries in light curves were explained with the adoption of two hot spots on the cool secondary.