• 천문학회보
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• 제35권2호
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• pp.83.1-83.1
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• 2010

Recent observations of Sloan Digital Sky Survey (SDSS) for the ugriz filters have provided the largest and the most homogeneous photometric database. Especially, the ugriz systems have been used in many telescopes, such as SDSS, CFHT, and Gemini, and will be applied next generation large telescopes. In addition, many stellar evolution models, like as PADOVA, BaSTI and DSEP, have introduced theoretical isochrones in ugriz system, to apply the isochrones into the photometry of stars in globular clusters. In this study, we transformed Yonsei-Yale($Y^2$) isochrones to ugriz photometric system and fit the isochrones to the (g-r, r), (g-i, r), and (r-i, r) CMDs of 13 globular clusters (Chun et al. 2009, Clem et al. 2008, An et al. 2008). We found that the derived ages from $Y^2$-isochrones are 1~3Gyr younger and the estimated distance moduli are 0.3mag larger than the values inferred from the other isochrones in r-band. Also, the E(B-V) are 0.02~0.04mag less than those estimated from the other models. The ages of each globular cluster estimated from $Y^2$-isochrones are 12~14Gyr and distance moduli show good agreement with previous studies. From this result, we confirmed the availability of the $Y^2$-isochrones in gri filters. However, it is a problem which will improve that E(B-V) values obtained from $Y^2$-isochrones are too small. Finally, the result of this study is expected to be used research of globular cluster in ugirz photometric system.

• 천문학회보
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• 제43권1호
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• pp.63.3-63.3
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• 2018

A comparison study between two low temperature opacity tables has been conducted. The opacity is the one of the major input physics in stellar model construction. Opacity is generally provided in a tabular form and as a function of 3 parameters, ie, density, temperature and chemical composition. Among available opacity tables, it has been common practice to utilize OPAL opacity table (Iglesias & Rogers, 1996) augmented with Ferguson opacity table (Ferguson et al. 2005) for the low temperature domain. For low temperature domain, another table, AESOPUS (Marigo & Aringer, 2009), has been announced in 2007. Reportedly, this opacity covers even lower temperature region, and is compatible with that of Ferguson in the overlapping temperature domain. To test the compatibility, stellar models and isochrones for various ranges in mass, metallicity and chemical composition, have been constructed. It is confirmed that there is no significant difference in the stellar models and isochrones constructed with the two different low temperature opacities. Therefore, in the construction of stellar models and isochrones, Ferguson low temperature opacity can be replaced with the AESOPUS opacity. The wider range in the temperature and chemical mixtures, and the easier accessibility make AESOPUS favorable in practical purpose.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2004년도 한국우주과학회보 제13권2호
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• pp.243-246
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• 2004

We calculate theoretical isochrones in a consistent way for five filters near the K-band, K, K', $K_s$, F205W, and F222M. Even when displayed in the same Vega magnitude system, the near-infrared colors of the same isochrone can differ by up to 0.18 mag at its bright end, depending on the filter. We analyze isochrones for several different extinction values, and find that a care is needed when comparing extinction values that are estimated by different filter sets, in particular when comparing those between atmospheric and space filter sets. To alleviate this problem, we present an 'effective extinction law' for each filter set and isochrone model, which describes extinction behaviour of isochrones in the observed color-magnitude diagram.

• 천문학회지
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• 제29권spc1호
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• pp.135-136
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• 1996

We present a new photometric study of the globular cluster NGC288 in Stromgren u, v, b, y, and H$\beta$ system. This cluster is known to have an intermediate metallicity but its color-magnitude diagram has a pure blue horizontal branch, which is a signature of metal poor stellar population. We compare our dataset with Bergbusch's (1993) in both field size and CMD to see whether different photometry system would determine the same physical parameters of a cluster. Demarque and Yi's isochrones (1996, private communication) were applied to Bergbusch's dataset, and we obtained distance modulus of (m - M) = 14.9 $\pm$ 0.2, color excess of E(B - V) = 0.03, and age of 1.5$\pm$3 Gyr. Vandenberg's (1985) isochrones for Stromgren system were also applied to Bergbusch's and our data. We find that the isochrone fits to different photometric systems give rather in consist ant solutions. The source of this discrepancy may become clear when the Demarque and Yi's isochrones for Johnson system are converted to those of Stromgren system. We note that Kurucz model atmospheres provide a useful ground for this conversion work as well as theoretical study of Stromgren characteristics of globular cluster stars.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 1994년도 한국우주과학회보 제3권2호
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• pp.67-72
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• 1994

• 천문학회보
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• 제29권2호
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• pp.67.1-67.1
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• 2004

• 천문학회보
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• 제27권2호
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• pp.62-62
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• 2002

• 한국수자원학회:학술대회논문집
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• 한국수자원학회 2002년도 학술발표회 논문집(II)
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• pp.861-866
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• 2002

• 천문학회보
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• 제40권1호
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• pp.70.4-70.4
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• 2015

Although the theory of stellar structure and evolution is considered one of the most successful developments in astrophysics, there still remains a significant mismatch between theoretical stellar models and the observed main sequence of the best studied nearby open clusters. To ease the tension, empirical corrections to the color-temperature transformations are used as a simple, but practical way of overcoming the difficulty than directly examining stellar atmosphere models that have large theoretical complexities and uncertainties. I will describe our continuing effort to calibrate stellar isochrones using cool main-sequence stars in Praesepe, complementing our previous work based on the Hyades and the Pleiades, and provide an extensive test of our models using photometry of cool and metal-rich main-sequence stars in NGC 6791. Finally, I will discuss the implication of our results on the mass loss in NGC 6791.

• 천문학회보
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• 제40권1호
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• pp.89.2-89.2
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• 2015

This research is to study the effects of individual metal elements(C, N, O, Na, Mg, Al, Si, and Fe) on the standard stellar models. The mixtures of the stellar models have been constructed to analyze the stars, extremely changed in the abundance of these elements. Therefore the mixture are based on the recent observation of stars in globular clusters. And the mass and metallicity grids have been decided in range $0.7{\sim}1.0M_{\odot}$ and 0.0002 ~ 0.007, respectively. The evolutionary tracks and isochrones, as well as the physical changes at each evolutionary phase, have been analyzed. Consequently, we present the mechanisms of the physical changes at each phase, and the quantified effects of the individual elements.