Yunnan-III models for evolutionary population synthesis

	Yunnan-III models for evolutionary population synthesis
	Zhang FH(张奉辉)1,2 ; Li LF(李立芳)1,2 ; Han ZW(韩占文)1,2 ; Zhuang YL(庄宇龙)1,2,3 ; Kang XY(康晓宇)1,2
刊名	MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
	2013-02
卷号	428 期号:4 页码:3390-3408
关键词	stars: AGB and post-AGB stars: evolution galaxies: evolution galaxies: fundamental parameters galaxies: stellar content
ISSN号	0035-8711
通讯作者	Zhang, F (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China.
产权排序	第一完成单位
英文摘要	We build the Yunnan-III evolutionary population synthesis (EPS) models by using the MESA stellar evolution code, BaSeL stellar spectra library and the initial mass functions (IMFs) of Kroupa and Salpeter, and present colours and integrated spectral energy distributions (ISEDs) of solar-metallicity stellar populations (SPs) in the range of 1 Myr to 15 Gyr. The main characteristic of the Yunnan-III EPS models is the usage of a set of self-consistent solar-metallicity stellar evolutionary tracks (the masses of stars are from 0.1 to 100 M-circle dot). This set of tracks is obtained by using the state-of-the-art MESA code. MESA code can evolve stellar models through thermally pulsing asymptotic giant branch (TP-AGB) phase for low-and intermediate-mass stars. By comparisons, we confirm that the inclusion of TP-AGB stars makes the V - K, V - J and V - R colours of SPs redder and the infrared flux larger at ages log(t/yr) greater than or similar to 7.6 [the differences reach the maximum at log(t/yr) similar to 8.6, similar to 0.5-0.2 mag for colours, approximately two times for K-band flux]. We also find that the colour-evolution trends of Model with-TPAGB at intermediate and large ages are similar to those from the STARBURST99 code, which employs the Padova-AGB stellar library, BaSeL spectral library and the Kroupa IMF. At last, we compare the colours with the other EPS models comprising TP-AGB stars (such as CB07, M05, V10 and POPSTAR), and find that the B - V colour agrees with each other but the V-K colour shows a larger discrepancy among these EPS models [similar to 1 mag when 8 less than or similar to log(t/yr) less than or similar to 9]. The stellar evolutionary tracks, isochrones, colours and ISEDs can be obtained on request from the first author or from our website (http://www1.ynao.ac.cn/similar to zhangfh/). Using the isochrones, you can build your EPS models. Now the format of stellar evolutionary tracks is the same as that in the STARBURST99 code; you can put them into the STARBURST99 code and get the SP's results. Moreover, the colours involving other passbands or on other systems (e. g. HST F439W - F555W colour on AB system) can also be obtained on request.
学科主题	Astronomy & Astrophysics
WOS标题词	Science & Technology ; Physical Sciences
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
关键词[WOS]	ASYMPTOTIC GIANT BRANCH ; INITIAL MASS FUNCTION ; STANDARD STELLAR LIBRARY ; HIGH-SPECTRAL-RESOLUTION ; TP-AGB MODELS ; M-CIRCLE-DOT ; RADIATIVE OPACITIES ; INTERMEDIATE-AGE ; LUMINOSITY FUNCTION ; CHEMICAL-YIELDS
收录类别	SCI
原文出处	http://mnras.oxfordjournals.org/content/428/4/3390
语种	英语
WOS记录号	WOS:000318232000046
内容类型	期刊论文
源URL	[http://ir.ynao.ac.cn/handle/114a53/4561]
专题	云南天文台_大样本恒星演化研究组云南天文台_中国科学院天体结构与演化重点实验室
作者单位	1.National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China 2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China 3.Graduate University of the Chinese Academy of Science, Beijing 100049, China
推荐引用方式 GB/T 7714	Zhang FH,Li LF,Han ZW,et al. Yunnan-III models for evolutionary population synthesis[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2013,428(4):3390-3408.
APA	Zhang FH,Li LF,Han ZW,Zhuang YL,&Kang XY.(2013).Yunnan-III models for evolutionary population synthesis.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,428(4),3390-3408.
MLA	Zhang FH,et al."Yunnan-III models for evolutionary population synthesis".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 428.4(2013):3390-3408.