• Journal of Astronomy and Space Sciences
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• 제31권3호
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• pp.187-197
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• 2014

We have investigated the dynamical stability of the proposed companions orbiting the Algol type short-period eclipsing binary SW Lyncis (Kim et al. 2010). The two candidate companions are of stellar to substellar nature, and were inferred from timing measurements of the system's primary and secondary eclipses. We applied well-tested numerical techniques to accurately integrate the orbits of the two companions and to test for chaotic dynamical behavior. We carried out the stability analysis within a systematic parameter survey varying both the geometries and orientation of the orbits of the companions, as well as their masses. In all our numerical integrations we found that the proposed SW Lyn multi-body system is highly unstable on time-scales on the order of 1000 years. Our results cast doubt on the interpretation that the timing variations are caused by two companions. This work demonstrates that a straightforward dynamical analysis can help to test whether a best-fit companion-based model is a physically viable explanation for measured eclipse timing variations. We conclude that dynamical considerations reveal that the proposed SW Lyncis multi-body system most likely does not exist or the companions have significantly different orbital properties from those conjectured in Kim et al. (2010).

• Journal of Astronomy and Space Sciences
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• 제34권2호
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• pp.75-82
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• 2017

High-resolution spectroscopic observations of the eclipsing binary system RR Lyn were made using the 1.8 m telescope at the Bohuynsan Optical Astronomical Observatory in Korea. The spectral resolving power was R = 82,000, with a signal to noise ratio of S/N > 150. We found the effective temperatures and surface gravities of the primary and secondary components to be equal to $T_{eff}$ = 7,920 & 7,210 K and log(g) = 3.80 & 4.16, respectively. The abundances of 34 and 17 different chemical elements were found in the atmospheric components. Correlations between the derived abundances with condensation temperatures and the second ionization potentials of these elements are discussed. The primary component is a typical metallic line star with the abundances of light and iron group elements close to solar values, while elements with atomic numbers Z > 30 are overabundant by 0.5-1.5 dex with respect to solar values. The secondary component is a ${\lambda}$ Boo type star. In this type of stars, CNO abundances are close to solar values, while the abundance pattern shows a negative correlation with condensation temperatures.

• 천문학회지
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• 제42권6호
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• pp.135-144
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• 2009

We present JHK near-infrared photometric study for the old open cluster (OC) Trumpler 5 (Tr 5), based on the 2MASS data. From the color-magnitude diagrams of Tr 5, we have located the position of the red giant clump (RGC) stars, and used the mean magnitude of the RGC stars in K-band to estimate the distance to Tr 5, d = $3.1{\pm}0.1$ kpc ($(m-M)_0$ = $12.46{\pm}0.04$). From fitting the theoretical isochrones of Padova group, we have estimated the reddening, metallicity, and age : E(B-V) = $0.64{\pm}0:05$, [Fe/H] = $-0.4{\pm}0.1$ dex, and t = $2.8{\pm}0.2$ Gyr (log t = $9.45{\pm}0.04$), respectively. These parameters generally agree well with those obtained from the previous studies on Tr 5 and confirms that this cluster is an old OC with metallicity being metal-poorer than solar abundance, located in the anti-Galactic center region.

• 천문학회지
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• 제53권2호
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• pp.35-42
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• 2020

We analyze high dispersion emission lines of the symbiotic nova AG Pegasi, observed in 1998, 2001, and 2002. The Hα and Hβ lines show three components, two narrow and one underlying broad line components, but most other lines, such as H_I, He_I, and He_II lines, show two blue- and red-shifted components only. A recent study by Lee & Hyung (2018) suggested that the double Gaussian lines emitted from a bipolar conical shell are likely to form Raman scattering lines observed in 1998. In this study, we show that the bipolar cone with an opening angle of 74°, which expands at a velocity of 70 km s^-1 along the polar axis of the white dwarf, can accommodate the observed double line profiles in 1998, 2001, and 2002. We conclude that the emission zone of the bipolar conical shell, which formed along the bipolar axis of the white dwarf due to the collimation by the accretion disk, is responsible for the double Gaussian profiles.

• 천문학회지
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• 제28권2호
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• pp.255-264
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• 1995

The HII region S140 and the associated molecular cloud L1204 have been observed with 10 molecular transitions, CO (1-0), $^{13}CO$ (1-0), $C^{18}O$ (1-0), CS (2-1), $HCO^+$ (1-0), HCN (1-0), SO (${2_2}-{1_1}$), $SO_2(2_{20}-3_{13})$, OCS (8-7), and $HNCO\;(4_{04}-3_{03})$ with ${\sim}50"$ angular resolutions. More than 7,000 spectra were obtained in total. The morphology of this region shows a massive fragment (the S140 core) and the extended envelope to the northeast. Several gas condensations have been identified in the envelope, having masses of ${\sim}10^{3}M_{\odot}$ and gas number densities of ${\lesssim}10^{4}cm^{-3}$ to $3{\times}10^{5}cm^{-3}$ in their cores. The column densities of the observed molecular species toward the S140 core appear to be the typical warm clouds' abundances. It seems to be that the S140 core and L1204 have been swept up by an expanding shell called the Cepheus bubble. The large value of $L_{IR}$(embedded\;stars)/$M_{cloud}\;{\sim}\;5\;L_{\odot}$/$M_{\odot}$ of the S140 core may suggest that the star formation has been stimulated by the HII region, but the shock velocity and the pressure of the region seem to give a hint of the spontaneous star formation by the self gravity.

• 천문학논총
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• 제30권2호
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• pp.189-191
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• 2015

The calibration of the period luminosity relation (PLR) for Galactic Mira variables is one of the principle aims of the VERA project. We observe $H_2O$ maser emission at 22 GHz associated with Mira variables in order to determine their distances based on annual parallaxes. We conduct multi-epoch VLBI observations over 1-2 years with a typical interval of one month using VERA in order to obtain annual parallaxes with an accuracy of better than than 10%. Recently, the annnual parallax of T Lep was determined to be $3.06{\pm}0.04$ mas corresponding to a distance of $327{\pm}4pc$ (Nakagawa et al., 2014). The circumstellar distribution and kinematics of $H_2O$ masers was also revealed. With accurate distances to the sources, calibrations of K-band absolute magnitudes ($M_K$) can be improved compared to conventional studies. By compiling Mira variables whose distances were determined with astrometric VLBI, we obtained a PLR of $M_K=3.51logP+1.37{\pm}0.07$.

• 천문학회보
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• 제43권2호
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• pp.59.2-59.2
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• 2018

We introduce a new project of constructing a large spectro-photometric samples of metal-poor (i.e. [Fe/H] < -1.0) subdwarfs in the Galactic halo. The sample is collected from a compilation of the stellar objects that are cross-identified both in the Sloan Digital Sky Survey (SDSS) and recently published data from GAIA mission. The color range of the selected stars covers 0.0 < (g-r) < 2.0; thus the spectral types of our sample span from early F- through late K-type stars on the metal-poor main sequence (i.e. the local subdwarf sequence). We scrutinized the physical, chemical, and kinematical properties of our samples using their SDSS medium-resolution (R ~ 2000) spectra, combined with accurately measured proper motions from GAIA satellite. Our study will provide useful information on the global trend in the various properties (e.g. abundance pattern as a function of the galactocentric distance; rotational velocity vs [Fe/H] ${\cdots}$ etc) of the metal-poor subdwarf populations in the Galactic halo, which is ultimately important to better understand metal-poor stellar evolutionary models and chemical evolution of the Milky Way halo in the early phase of its formation. Further our comprehensive catalog of the Galactic field halo subdwarfs collected in this study will serve a solid groundwork for future follow-up high resolution spectroscopic observations on many interesting individual targets.

• 천문학회보
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• 제39권2호
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• pp.84.1-84.1
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• 2014

This research is to study the effects of individual element(C, N, O, Na, Mg, Al, Si, and Fe) on the standard stellar models. Our work is different from previous works in two aspects. Firstly, we have chosen to maintain helium abundance and other metal elements as target elements were changed. This is to see the effects more clearly, without further complication. Secondly, the amount of enhancement or reduction in each element has been based on the recent observation of stars in globular clusters. For comparison study with observation of the globular clusters, the mass and metallicity grids of the standard stellar models have been constructed in range $0.7{\sim}1.0M{\odot}$ and 0.0002~0.007, respectively. The opacity as a function of depth in stellar models at equal evolutionary point, as well as the evolutionary tracks, have been analyzed. The quantified shifts of the evolutionary tracks for the stellar models which have changed abundance of individual element and the astronomical meaning with physical reasons which produce the results, are going to be presented in this talk.

• 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.

• 유통과학연구
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• 제15권7호
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• pp.19-24
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• 2017

Purpose - There are several problems that organizations face to make a better team-based system such as free-rider issue, assigned difficult jobs unfairly and bickering between high performers and average performers. The purpose of this study is to provide solutions for practitioners through past academic studies on how organizations can resolve several issues in team management. Ultimately, it would lead to employees as better performers for organization's profitability and customers' satisfaction. Research design, data, and methodology - Solution 1 - put employees who have a similar performance ability together into a same team and apply 'growth' approach for low performance team. Solution 2 - make a new evaluation system which is balanced between individual's performance and team's performance. Solution 3 - monitor thoroughly to diffuse difficult works equally among teams and develop management practice system that may prevent or resolve difficult work-loads for a team or an individual performer. Result - Investigation suggests that organizations may resolve three conflicts which come from team base system. Moreover, the implications of results show that the most important criteria in team management depend on whether performers have a similar ability in the same team and management handles issue of justice and the performance of each employee is evaluated by total team performance evaluation simultaneously. Conclusions - All in all, our recommendation concludes that if three issues are resolved, the lack of trust in team-based system among team members will be missed.