Initial Mass Function and Star Formation History in the Small Magellanic Cloud
(주)코리아스칼라
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- 2016.04.02
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- 2014.09
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서지정보
ㆍ발행기관 : 한국지구과학회
ㆍ수록지정보 : 한국지구과학회지 / 35권 / 5호
ㆍ저자명 : Lee, Ki-Won
목차
Abstract
Introduction
Population Synthesis Method
Stellar evolution model
Initial Mass Function
Star formation history
Selection effects
Transformation into observable parameters
Bayesian Statistics
Bayesian inference
Likelihood method
Results
Continuous model
Single burst models
Double bursts models
Complex models
Summary
Acknowledgment
References
영어 초록
This study investigated the initial mass function (IMF) and star formation history of high-mass stars in the Small Magellanic Cloud (SMC) using a population synthesis technique. We used the photometric survey catalog of Lee (2013) as the observable quantities and compare them with those of synthetic populations based on Bayesian inference. For the IMF slope (γ) range of -1.1 to -3.5 with steps of 0.1, five types of star formation models were tested: 1) continuous; 2) single burst at 10 Myr; 3) single burst at 60 Myr; 4) double bursts at those epochs; and 5) a complex hybrid model. In this study, a total of 125 models were tested. Based on the model calculations, it was found that the continuous model could simulate the high-mass stars of the SMC and that its IMF slope was -1.6 which is slightly steeper than Salpeter's IMF, i.e., γ=-1.35.
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