• 제목/요약/키워드: stars: variables: other

검색결과 12건 처리시간 0.027초

Chemical composition of Am stars: RR Lyn and $\rho$ Pup

  • Yushchenko, A.V.;Lee, J.J.;Kang, Y.W.;Doikov, D.N.
    • 한국우주과학회:학술대회논문집(한국우주과학회보)
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    • 한국우주과학회 2008년도 한국우주과학회보 제17권2호
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    • pp.22.3-22.3
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    • 2008
  • We present the results of the investigations of high dispersion spectra of two stars. These are the eclipsing binary RR Lyn, and $\rho$ Pup - the prototype of the group of pulsating variables. The spectra were obtained at 1.8 m Bohyuunsan observatory telescope, and 8.2 m VLT. We found the chemical composition. The both components of RR Lyn are Am stars (metallic line stars), but the abundance patterns of the components are not similar - the iron abundance and the abundances of other elements are surely different. For few elements the differences exceeds 1 dex. We found the abundances of 56 chemical elements in the atmosphere of $\rho$ Pup. This is one of the best stellar abundance patterns. It permits to investigate the role of the charge-exchange reactions in stellar atmospheres. These reactions can produce the abundance anomalies in the atmospheres of B-F type stars. These reactions can be one of the sources of galactic cosmic rays, and the reason of the braked rotation of A-F type chemically peculiar stars.

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DISCOVERY OF NEW RR LYRAE STARS IN THE CENTER OF THE GLOBULAR CLUSTER M53

  • Sohn, Sang-Mo;Rey, Soo-Chang;Lee, Young-Wook;Byun, Yong-Ik;Chun, Mun-Suk
    • Journal of Astronomy and Space Sciences
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    • 제16권2호
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    • pp.115-130
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    • 1999
  • We report the discovery of 17 new RR Lyrae variables in the central region ($\rleq1'$) of the globular cluster M53. There candidates were identified by using the Welch & Stetson (1993) technique and confirmed by checking individual light curves in both B and V bands. The color-magnitude diagram of the horizontal-branch stars in the central region is compared with that for stars observed in the outer region by Rey et al. (1998). Including the new data from this study, we estimate the fraction of c typeRR Lyrae variables, n(c)/n(ab + c), to be 0.43 which agrees well with the valuse of other Oosterhoff group II clusters.

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The Search for Binaries in Post-Asymptotic Giant Branch Stars: Do Binary Companions Shape the Nebulae?

  • Hrivnak, Bruce J.
    • Journal of Astronomy and Space Sciences
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    • 제29권1호
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    • pp.57-61
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    • 2012
  • Binary companions are often invoked to explain the axial and point symmetry seen in the majority of planetary nebulae and proto-planetary nebulae (PPNs). To explore this hypothesis, we have undertaken a long-term (20 year) study of light and velocity variations in PPNs. From the photometric study of 24 PPNs, we find that all vary in brightness, and from a subset of 12 carbon-rich PPNs of F-G spectral type we find periods of 35-155 days, with the cooler having the longer periods. The variations are seen to be due to pulsation; no photometric evidence for binarity is seen. A radial velocity study of a sub-sample of seven of the brightest of these shows that they all vary with the pulsation periods. Only one shows evidence of a longer-term variation that we tentatively identify as being due to a binary companion. We conclude that the present evidence for the binary nature of these PPNs is meager and that any undetected companions of these PPNs must be of low mass (< 0.25 $M_{\odot}$) or long period (> 30 years).

Galactic Globular and Open Clusters in the Sloan Digital Sky Survey. III. Horizontal Branch Stars and Mass Loss in NGC 6791

  • Yu, Hyein;An, Deokkeun;Chung, Chul
    • 천문학회보
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    • 제39권1호
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    • pp.61.2-61.2
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    • 2014
  • We present a set of fiducial sequences of horizontal-branch stars in bright Galactic globular clusters, which have previously been observed in the Sloan Digital Sky Survey (SDSS). We derive fiducial lines on color-magnitude diagrams in multiple color indices (g - r, g - i, g - z, and u - g), after rejecting foreground and background objects as well as RR Lyrae variables utilizing these color indices. We compare our fiducial sequences with model predictions from Yonsei-Yale evolutionary tracks and BaSel spectral libraries, and find a satisfactory agreement between them in terms of their color-magnitude relations, except in u - g. We also compare theoretical models to color-magnitude diagrams of two open clusters (M67 and NGC 6791). Based on our best available cluster distance and reddening, we find that the mass of red clump (RC) stars in NGC 6791 is about a factor of two smaller than an earlier estimate from the application of asteroseismic scaling relations for solar-like oscillations. The smaller RC mass implies an enhanced mass loss along the red giant branch, which is in accordance with other compelling evidences found in this metal-rich system. Our estimated luminosity of RC stars in NGC 6791 is about 0.2 mag fainter than in earlier investigations based on solar-metallicity calibrations, and results in ~10% reduction in the RC-based distance estimation, when applied to metal-rich systems such as in the Galactic bulge.

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Magellanic Clouds Cepheids: Thorium Abundances

  • Jeong, Yeuncheol;Yushchenko, Alexander V.;Gopka, Vira F.;Yushchenko, Volodymyr O.;Kovtyukh, Valery V.;Vasil'eva, Svetlana V.
    • Journal of Astronomy and Space Sciences
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    • 제35권1호
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    • pp.19-30
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    • 2018
  • The analysis of the high-resolution spectra of 31 Magellanic Clouds Cepheid variables enabled the identification of thorium lines. The abundances of thorium were found with spectrum synthesis method. The calculated thorium abundances exhibit correlations with the abundances of other chemical elements and atmospheric parameters of the program stars. These correlations are similar for both Clouds. The correlations of iron abundances of thorium, europium, neodymium, and yttrium relative to the pulsational periods are different in the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC), namely the correlations are negative for LMC and positive or close to zero for SMC. One of the possible explanations can be the higher activity of nucleosynthesis in SMC with respect to LMC in the recent several hundred million years.

Strong Attachment toward Human Brand and Its Implication for Life-Satisfaction and Self-efficacy: Hero versus Celebrity

  • Jun, Mina;Kim, Chung K.;Han, Jeongsoo;Kim, Miyea;Kim, Joshua Y.
    • Asia Marketing Journal
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    • 제16권1호
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    • pp.101-116
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    • 2014
  • In the year 2013, Warren Buffett was named one of the most influential people of the year by TIME magazine. When people are exposed to such news, they show strong interest in who the influential people are and how those people became so successful. Likewise, people show strong attachment to other prominent figures as well. This social phenomenon indicates that people perceive well-known persona like business leaders, TV stars or sports stars etc. as human brands of intangible assets. As the role of these human brands is becoming more important, people tend to develop stronger attachment toward them. Another notable modern social phenomenon is people's pursuit of life-satisfaction and social well-being. People desire to increase their quality of life by having quality time with family and friends, and also by building attachment towards celebrities, sports stars, and so on. The main objective of this study is to examine how attachment toward human brands affects quality of life. While existing studies on human brands examined antecedents of attachment, e.g., some needs fulfillment such as A-R-C needs (autonomy, relatedness and competence needs) fulfillment, this study focuses on the outcome variables of attachment, e.g., how attachment toward human brands affects stress relief and life satisfaction through self-efficacy. Based on previous research, we divided human brands into two types: heroes and celebrities. Heroes are defined as people who have considerable and lasting importance on both societal and individual levels, and celebrities are defined as people who are well-known but have little or no short-term impact on society and individual levels. This study focuses on how attachment toward each type of human brands, celebrities and heroes, affects the quality of life or well-being. This study focuses on three important outcome variables; stress relief, life satisfaction, and self-efficacy, (three variables) which have been recently gaining importance, especially in the domain of positive psychology. Major findings from the present study show that although celebrities draw attachment from people by providing fun and entertainment or providing stress relief, they have weak influences on the wellbeing or efficacy of individuals at a deeper level. In contrast, attachment toward heroes helps people live better by providing meaning and positively influencing life satisfaction through self-efficacy (Frankl 1997). These results are consistent with the main tenet of 'positive psychology' which seeks "to find and nurture genius and talent and to make normal life more fulfilling" (Seligman and Csikszentmihalyi 2000). Considering the fact that certain celebrities are perceived as heroes to some, we can conclude that celebrities can become heroes if they provide meaning and value to the lives of people. This study contributes to the research stream of human brands since the most current leading research (e.g., Thomson 2006) indicated the need to look at the resulting effect of attachment on life satisfaction through self-efficacy. Another important contribution is that we empirically documented the different effects of celebrities and heroes. As expected, this study shows that heroes more deeply influence the lives of individuals in the long term while celebrities do so rather shallowly in the short term. The issues of the influence of heroes on the individuals' lives need to be further investigated in relation with the perspective of positive psychology.

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NGC 7790의 UBVI CCD 측광 (UBVI CCD Photometry of NGC 7790)

  • 최동열;김희수;임범두;성환경
    • 한국지구과학회지
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    • 제36권7호
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    • pp.661-673
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    • 2015
  • 우즈베키스탄 Maidanak 천문대 AZT-22 1.5 m 망원경(f/7.74)과 SITe $2000{\times}800$CCD를 사용하여 3개의 ${\delta}$ Cep 변광성 CEa Cas, CEb Cas 및 CF Cas가 있는 중년 산개성단 NGC 7790의 UBVI 측광 관측을 수행하였다. 관측자료는 IRAF/DAOPHOT를 이용하여 PSF 측광을 수행하였으며, V와 I 필터에서 모두 측광된 별의 수는 총 1008개이며, 측광의 한계등급은 $V{\approx}22$등급이다. 대기소광계수 및 측광영점을 결정하기 위하여 천구적도에 있는 여러 표준별과 청색 및 적색 표준별을 다양한 대기투과량에서 관측하였다. 표준별 측광을 통해 대기소광계수 및 측광영점을 결정하고, 성단의 측광자료는 Johnson-Cousins UBVI 표준계로 변환하였다. NGC 7790의 UBVI 색-등급도와 색-색도에서 이 성단의 B와 V 필터에서의 색초과량 [$E(B-V)=0.58{\pm}0.02$], B와 V 필터에서의 선택적 소광량 [$R_V{{\equiv}}A_V/E(B-V)=3.02{\pm}0.09$] 및 거리지수($V_0-M_V=12.65{\pm}0.10$)를 얻었다. H-R도에서 세페이드 변광성의 위치를 고려하여 나이를 결정하였다. 이 과정에서 Padova 연구집단(Bressan et al., 2012)의 등연령곡선(Z=0.019)과 Geneva 연구집단($Ekstr{\ddot{o}}m$ et al., 2012)의 등연령곡선(Z=0.014)을 모두 사용하였고, 그중에서 자전을 고려한 Geneva 연구집단의 진화모형이 관측자료와 잘 일치하여 NGC 7790의 나이로 log $age=8.05{\pm}0.05$ [yr]를 얻었다. 또 NGC 7790내 세페이드 변광성의 절대등급은 세페이드 변광성의 평균 주기-광도 관계에 비해 분산 범위 내에 있기는 하지만 주어진 주기에서 평균적으로 약 0.5등급 정도 밝음을 확인하였다.

Graphs Used in ASEAN Trading Link's Annual Reports: Evidence from Thailand, Malaysia, and Singapore

  • Kurusakdapong, Jitsama;Tanlamai, Uthai
    • Journal of Information Technology Applications and Management
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    • 제22권3호
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    • pp.65-81
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    • 2015
  • This study reports a preliminary finding of the types and numbers of graphs being presented in the annual reports of about thirty top listed companies trading publicly in the stock markets of three countries-Thailand (SET), Malaysia (BM), and Singapore (SGX)-that were chosen based on their inclusion in the ASEAN Stars Index under the ASEAN Trading Link project. A total of 6,753 graphs from nineteen sectors were extracted and examined. Banking, real estate, and telecommunications are ranked the three most condense sectors, accounting for 50.2% of the total number of graphs observed. The three most used graphs are the Conservative Bar, Donut graph and Stack Bar. Less than one percent of Infographic type graphs were used. The five most depicted graphed variables are Asset, Revenue, Net profit, Liability, and Dividend. Using rudimentary framework to detect distorted or misleading statistical graphs, the study found 60.6% of the graphs distorted across the three markets, SET, BM, and SGX. BM ranked first in percentages of graphs being distortedly presented (73%). The other two markets, SET and SGX, have about the same proportions, 53.88% and 53.03%, respectively. Likewise, the proportions of Well-designed versus Inappropriate-designed graphs of the latter two markets are a little over one time (SET = 1 : 1.17; SGX = 1 : 1.13), whereas the proportion is almost triple for the BM market (BM = 1 : 2.70). In addition, the trend of distorted graphs found is slightly increasing as the longevity of the ASEAN Stars Index increases. One possible explanation for the relatively equal proportion of inappropriate graphs found is that SET is the smallest market and SGX, though the largest, is the most regulated market. BM, on the other hand, may want to present their financial data in the most attractive manner to prospective investors, thus, regulatory constraints and governance structure are still lenient.

THEORETICAL STUDY ON OBSERVED COLOR-MAGNITUDE DIAGRAMS

  • Lee, See-Woo
    • 천문학회지
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    • 제12권1호
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    • pp.41-70
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    • 1979
  • From $B\ddot{o}hm$-Vitense's atmospheric model calculations, the relations, [$T_e$, (B-V)] and [B.C, (B-V)] with respect to heavy element abundance were obtained. Using these relations and evolutionary model calculations of Rood, and Sweigart and Gross, analytic expressions for some physical parameters relating to the C-M diagrams of globular clusters were derived, and they were applied to 21 globular clusters with observed transition periods of RR Lyrae variables. More than 20 different parameters were examined for each globular cluster. The derived ranges of some basic parameters are as follows; $Y=0.21{\sim}0.33,\;Z=1.5{\times}10^{-4}{\sim}4.5{\times}10^{-3},\;age,\;t=9.5{\sim}19{\times}10^9$ years, mass for red giants, $m_{RG}=0.74m_{\odot}{\sim}0.91m_{\odot}$, mass for RR Lyrae stars, $m_{RR}=0.59m_{\odot}{\sim}0.75m_{\odot}$, the visual magnitude difference between the turnoff point and the horizontal branch (HB), ${\Delta}V_{to}=3.1{\sim}3.4(<{\Delta}V_{to}>=3.32)$, the color of the blue edge of RR Lyrae gap, $(B-V)_{BE}=0.17{\sim}0.21=(<(B-V)_{BE}>=0.18),\;[\frac{m}{L}]_{RR}=-1.7{\sim}-1.9$, mass difference of $m_{RR}$ relative to $m_{RG},(m_{RG}-m_{RR})/m_{RG}=0.0{\sim}0.39$. It was found that the ranges of derived parameters agree reasonably well with the observed ones and those estimated by others. Some important results obtained herein can be summarized as follows; (i) There are considerable variations in the initial helium abundance and in age of globular clusters. (ii) The radial gradient of heavy element abundance does exist for globular clusters as shown by Janes for field stars and open clusters. (iii) The helium abundance seems to have been increased with age by massive star evolution after a considerable amount (Y>0.2) of helium had been attained by the Big-Bang nucleosynthesis, but there is not seen a radial gradient of helium abundance. (iv) A considerable amount of heavy elements ($Z{\sim}10{-3}$) might have been formed in the inner halo ($r_{GC}$<10 kpc) from the earliest galactic co1lapse, and then the heavy element abundance has been slowly enriched towards the galactic center and disk, establishing the radial gradient of heavy element abundance. (v) The final galactic disk formation might have taken much longer by about a half of the galactic age than the halo formation, supporting a slow, inhomogeneous co1lapse model of Larson. (vi) Of the three principal parameters controlling the morphology of C-M diagrams, it was found that the first parameter is heavy clement abundance, the second age and the third helium abundance. (vii) The globular clusters can be divided into three different groups, AI, BI and CII according to Z, Y an d age as well as Dickens' HB types. BI group clusters of HB types 4 and 5 like M 3 and NGC 7006 are the oldest and have the lowest helium abundance of the three groups. And also they appear in the inner halo. On the other hand, the youngest AI clusters have the highest Z and Y, and appear in the innermost halo region and in the disk. (viii) From the result of the clean separations of the clusters into three groups, a three dimensional classification with three parameters, Z, Y and age is prsented. (ix) The anomalous C-M diagrams can be expalined in terms of the three principal parameters. That is, the anomaly of NGC 362 and NGC 7006 is accounted for by the smaller age of the order of $1{\sim}2{\times}10^9$ years rather than by the helium abundance difference, compared with M 3. (x) The difference in two Oosterhoff types I and II can be explained in terms of the mean mass difference of RR Lyrae variables rather than in terms of the helium abundance difference as suggested by Stobie. The mean mass of the variables in Oosterhoff type I clusters is smaller by $0.074m_{\odot}$ which is exactly consistent with Rood's estimate. Since it was found that the mean mass of RR Lyrae stars increases with decreasing Z, the two Oosterhoff types can be explained substantially by the metal abundance difference; the type II has Z<$3.4{\times}10^{-4}$, and the type I has higher Z than the type II.

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팬덤활동의 유형에 따른 효과크기 비교 연구: 메타분석 기반 (A Comparison Study on the Effect Size According to the Type of Fandom Activities : Based on Meta-analysis)

  • 김종윤;김은비
    • 한국융합학회논문지
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    • 제11권6호
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    • pp.259-268
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    • 2020
  • 본 연구는 팬덤활동에 연구들을 총체적·계량적으로 분석한 후 팬덤활동의 구성 유형과 효과를 검증하는 데 목적이 있다. 연구결과는 다음과 같다. 효과크기 비교 시 사회경제분야 관련 변인이 가장 큰 효과크기를 보였고, 다음은 개인 행동, 개인심리로 효과크기가 나타났다. 다음으로 팬덤활동의 영향요인에서 긍정적 변인의 효과크기가 중간 수준의 효과크기를 나타내고 부정적 변인의 효과크기가 낮은 수준의 효과크기를 보이는 것으로 나타났다. 또한 팬덤 형태 내 분석에서는 팬덤이 아이돌 팬덤일 때 가장 효과크기가 크고, 그다음은 스포츠스타, 배우 순이었다. 연구 대상자 중 효과크기는 대학생, 전체, 성인, 중고등학생, 중학생 순으로 나타났다. 한편 나라별 구분에 따른 분석을 실시한 결과 중국이 가장 효과크기가 높고, 유사하게 미국의 경우도 높은 수준의 효과크기가 있었다. 반면 대한민국의 경우 효과크기가 나타나 낮은 수준의 효과크기를 보였다.