• 제목/요약/키워드: UV Lines

검색결과 151건 처리시간 0.021초

ON THE LONG TIME SPECTRAL VARIABILITY OF NGC 5548

  • ISMAILOV, NARIMAN Z.;BASHIROVA, ULVIYYE Z.
    • 천문학논총
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    • 제30권2호
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    • pp.531-533
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    • 2015
  • We have investigated the long term variability of the intensities of the broad-line region emission lines in the UV spectra of Seyfert I galaxy NGC 5548 from 1973-1996. We have obtained the following results: 1) a high level correlation between the intensities of emission lines as well as between intensities of emission lines and continuum fluxes was discovered. With increasing wavelength the correlation in both cases becomes weaker, 2) the relationship between the intensity of emission lines and the flux radiation in the continuum can be expressed by a power law function with coefficients of ${\alpha}{\approx}0.8-1.1$ for different lines. When the difference between the wavelengths of spectral lines and the continuum is increased, the value of the power function decreases, and 3) it was found that the magnitude of the variability of the line intensities are weaker than the range of variability of the continuum fluxes. The magnitude of the variability of the line intensities and the continuum fluxes increase at longer wavelengths.

44i BOO의 자외선 방출연구 (UV LINE EMISSIONS OF 44i BOOTIS)

  • 한동주;김용기;한원용;이우백
    • Journal of Astronomy and Space Sciences
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    • 제15권2호
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    • pp.335-340
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    • 1998
  • IUE 저 분산 관측자료를 가지고 W-UMa 형 별인 44i Boo의 자외선 광도곡선을 완성하였다. 채층과 전이영역으로부터 나오는 방출선의 변화를 알아보기 위해서 CI, CII, CIV, SiIV, Hell 선의 방출선 세기를 계산하였다. CIV 방출 선이 가장 강한 방출을 보였으며, CII, Hell, CI, SiV의 순서로 방출선의 세기가 관측되었음이 확인되었다. 또한 방출선의 세기가 주기적으로 변하고 있음을 확인하였고, 모든 방출 선들이 위상 0.2와 0.8부근에서 상대적으로 강한 방출 선을 보인다. 이는 44i Boo의 표면에서 채층 및 전이영역의 활동성으로 인해 자외선 방출이 불 균일하게 나오고 있음을 나타내는 것이라고 해석할 수 있다. 채층 활동의 변화로 인해 관측시간이 서로 다를 때 자외선 방출선의 변광 형태도 달라지고 있음을 확인하였다.

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W UMa형 별들의 UV 방출선 연구 (UV LINE EMISSIONS OF W UMa STARS)

  • 김용기;한동주
    • Journal of Astronomy and Space Sciences
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    • 제17권1호
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    • pp.39-44
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    • 2000
  • lUE 저분산 자로플 가지고 44i Boo, W UMa, AW UMa및 VW Cep에서 나오는 자외선 방출선들의 특징을 조사하였다 단파장영역과 장파장영역에서의 방출선 선세기를 구하여, 이를 자$\boxUl$선 등급으로 변환하여 광도곡선을 얻었다 단파장 영ff에서 나오는 방출선인 C I, C II, C IV, SiIV, N V에 대한 선세기를 구한 결파, C IV가 모든 별에서 가장 센 방출을 보였으며. Si IV와 NV는 비교적 작은 양의 선세기를 나타내었다. 4개의 W UMa 별 쿵에근 44i Boo가 가장 높은 선세기를 보였으며, 단과장 영역에서는 위상 0.2와 0 8부근에서 자외선 팡도가 maximup을 보이는 변광을 확인하였다 또한, 전이영역에서 나오는 C IV, Si IV, N V 방출선을 합하여 이를 극소기의 태양값과 비교하여 태양보다 최대40배의 높은 활동성을 가지고 있음을 알았다. 짧은 주기를 갖는 별,즉 44i Boo, W UMa, AW UMa순으로 전이영역의 헐동성이 감소하는 것으로 나타났다. 장 파장 영역에서는 AW UMa와 VW Cep의 Mg ll 방출선을 조사하였는데, 단파장의 방출선 보다 뚜렷한 주기적 변광을 보였으며, 이를 이응하여 두 별의 유효온도를 추정하였다..

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NONTHERMAL BROADENING OF UV LINES OBSERVED AT THE LIMB OF THE QUIET SUN

  • LEE HVUNSOOK;YUN HONG SIK;CHAE JONGCHUL
    • 천문학회지
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    • 제33권1호
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    • pp.57-73
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    • 2000
  • We have done a spectroscopic study of the solar transition region using high resolution UV & EUV data obtained by SUMER(Solar Ultraviolet Measurements of Emitted Radiation) on board SOHO(Solar and Heliospheric Observatory). Optically thin and conspicuous emission lines observed at the solar limb are carefully selected to acquire average values of physical parameters for the quiet region as a function of radial distance. Our main results found from the present study can be summarized as follows. 1) Nonthermal velocities estimated from various UV lines do not decrease with height at least within one total line intensity scale height above the limb. 2) Nonthermal velocity distribution with temperature is very similar to that of the disk center, in the sense that its peak is located around $2{\times}10^5 K$, but the value is systematically larger than that of the disk. 3) It is found that nonthermal velocity is inversely proportional. to quadratic root of electron density up to about 10 arc seconds above the limb, i.e. ${\xi}\~N_e^{-1/4}$, implying that the observed nonthermal broadening can be attributed to Alfven waves passing through the medium. 41 Electron density estimated from the O V 629/760 line ratio is found to range from about $1{\times}10^{10}cm^{-3}$ to $2{\times} 10^{12}cm^{-3}$ in the transition region.

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THE SWINGS EFFECTS OF THE A-X SYSTEM AND v''= 1-0 BAND OF CO

  • KIM SANG-JOON
    • 천문학회지
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    • 제29권2호
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    • pp.223-243
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    • 1996
  • We have constructed a line-by-line model of the A-X system of CO in order to analyze the CO bands appearing in the UV spectra of comets. The model includes electronic, rotational, vibrational transitions, excitations by solar UV radiation, and effects of neutral and electron collisions. The major bands of the A-X system occur in the $1200 - 1800{\AA}$ range where the temporal variation of solar irradiation is significant. The solar spectrum in this spectral range shows many emission lines, which cause a significant Swings effect. We derived fluorescence efficiencies of the bands as functions of heliocentric velocity and cometocentric distance using a high resolution spectrum of the sun. We compared our model with a spectrum of comet P/Halley obtained with the IUE, and estimated that the UV Swings effects are less than 20 fluorescence efficiencies for the most bands of the A-X system. We discuss the temporal variation of solar UV irradiation and its effects on the fluorescence efficiencies. The study of the A-X system also requites knowledge of vibrational and rotational fluorescent processes in the infrared and radio regions because the majority of CO molecules in the coma is in the ground rotational states. The solar infrared spectrum near 5 microns, where the fundamental band of CO occurs, contains strong absorption lines of the fundamental band and hot bands of CO and its isotopes. We derived fluorescence efficiencies of the infrared band as functions of heliocentric velocity and cometrocentric distance. The solar absorption lines near 5 microns cause a 20 reduction of the g-factor of the fundamental band at heliocentric velocities close to 0 km/sec. We discuss the effects of neutral and electron collisions on the fluorescence efficiencies of the infrared and UV bands.

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Investigating the relation between AGN gas metallicity and their host galaxy stellar metallicity using a sample of local Seyfert 1 galaxies

  • 신재진;우종학
    • 천문학회보
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    • 제36권2호
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    • pp.72.1-72.1
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    • 2011
  • We investigate the relation between AGN gas metallicity and their host galaxy stellar metallicity using a sample of local Seyfert 1 galaxies. Stellar metallicity is measured from stellar absorption lines while AGN gas metallicity is derived from the flux ratios of UV emission lines. We use a high quality spectra obtained from the Lick AGN Monitoring Project, to obtain pure host galaxy spectra based on the spectral decomposition analysis, leading to accurate measurements of the Mg2 (5175) and Fe (5270) indices. In the case of AGN gas metallicity, we measure the ratio of NV1240 to CIV1549 lines using UV spectra from the archival IUE and HST STIS data. We will present the results of metallicity measurements and comparison between AGN and stellar metallicity, and discuss the implications of the results.

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Peculiar Features in the Emission Lines of Symbiotic Stars AG Draconis and UV Aurigae

  • Kim, Soo Hyun;Yoon, Tae Seog;Oh, Hyung-il
    • 천문학회보
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    • 제43권2호
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    • pp.59.3-59.3
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    • 2018
  • 공생별 AG Dra와 UV Aur에 대해 지난 10여년간 보현산천문대 1.8m망원경과 고분산 에셀 분광기 BOES(BOao Echelle Spectrograph)로 분광관측을 수행해 왔다. 최근 2017년 11월 - 2018년 6월 관측에서, AG Dra의 Fe II 방출선과 UV Aur $H{\alpha}$ 방출선이 예년과 다른 변화 모습을 보이고 있음을 찾아내었다. 이에 대한 변화 원인을 공전주기, 밝기 변화 또는 다른 이유와 연관지어 설명하고자 한다.

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INVAR 마스크 응용 반도체 기판 소재의 고체 UV 레이저 프로젝션 어블레이션 (DPSS UV Laser Projection Ablation of IC Substrates using an INVAR Mask)

  • 손현기;최한섭;박종식
    • 한국레이저가공학회지
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    • 제15권4호
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    • pp.16-19
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    • 2012
  • Due to the fact that the dimensions of circuit lines of IC substrates have been forecast to reduce rapidly, engraving the circuit line patterns with laser has emerged as a promising alternative. To engrave circuit line patterns in an IC substrate, we used a projection ablation technique in which a metal (INVAR) mask and a DPSS UV laser instead of an excimer laser are used. Results showed that the circuit line patterns engraved in the IC substrate have a width of about 15um and a depth of $13{\mu}m$. This indicates that the projection ablation with a metal mask and a DPSS UV laser could feasibly replace the semi-additive process (SAP).

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Effects of Radioprotectors on DNA Repair Capacity of Tumor Cells

  • Kim, Choon-Mi;Kim, Mi-Kyung
    • Archives of Pharmacal Research
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    • 제16권4호
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    • pp.259-264
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    • 1993
  • Three cell lines, CHO, L929 and B16 which are non-tumorigenic and cancer cells, respectively, were first tested for their survival in the presence of radioprotective ginseng protein fraction(GPF0. The influence of three radioprotectors-CPF, cysteamine, and 1-Methyl-2-bis[(2-methylthio)vinyl] quinolinium iodide (MVQI) on DNA repair capacity of UV damaged cells survival test, the GPF showed higher cytotoxicity in L929 and B16 than in CHO cells. However, the degree of cell killing was also investigated by measuring $^3H$-thymidine incorporation of PUVA treated cells. In cell survival test, the GPF showed higher cytotoxicity in L929 and B16 than in CHO cells. However, the degree of cell killing was not high enough to consider it as an antitumorigenic agent. Variable results were obtained in the effects on DNA repair capacity depending on the protectors and cell lines used. In pretreatment, the presence of GPF and MVOI brought about a sinificant increase in the capacity in both CHO and B16 cells. However, in L929, the enhancing effect was not shown. In all three cell lines, cysteamine showed lower repair capacity than control, suggesting the primary damage reduction in stronger enhancing effects in L929 and B16 cells, while it was weaker in CHO cells. Here also cystemine hsowed a very little or no increase in the capacity in all three cell lines. These results demonstrate that GPF has mild cytotoxicity in tumorignic cells and that GPF and MVQI enhance DNA repair capacity of UV damaged cells, whether they are tumorigenic or not. On the other hand, cysteamine shows only damage reduction effect. Celles of different genetic origin seem to give different responses to the modifier and different modifiers may possibly work by different mechanisms.

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광중합 개시제 첨가량의 변화에 따른 Bisphenol A diacrylate UV 경화 film의 역학적 거동 (Dynamic Behavior on the Bisphenol A diacrylate UV curing film according to change of photoinitiator concentration)

  • 노재호
    • 한국인쇄학회지
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    • 제12권1호
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    • pp.81.2-98
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    • 1994
  • This syudy analyzed the main bodies, marginal space, Position of the main bodies of current textbooks in high schools and "the eriteria of reading system for textbooks" which was suggested the Department of Education and Provided some suggestions for the improvement. The research methods used for the study were both literature review and survey rdsdarch with a questionaire. Inorder to research for the main body of textbook, space of margin, the optimum position of the main body, sizes of litters, spaces between letters, words, lines, length of lines, sizes of main body and margin, and margin and position of main body were checked through a related literature review. For the questionaire experiment, a questionaire based on data drawn from analysis of current textbooks, :criteria for reading system of textbook" suggested by the Department of Education, and some suggestions for improvement by the researcher was made and used for the test, targetting 384 body and girl student in high schools.n high schools.

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