Effects of Non-Solar Abundance Ratios on Star Spectra: Observations versus Models

被引：0

作者：

Sansom, Anne E. ^{[1
]}

Milone, Andre de Castro ^{[2
]}

Vazdekis, Alexandre ^{[3
]}

Sanchez-Blazquez, Patricia ^{[4
]}

机构：

[1] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

[2] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil

[3] Inst Astrofis Canarias, E-38200 Tenerife, Spain

[4] Univ Autonoma Madrid, Dept Fis Teor, Madrid 28409, Spain

来源：

SPECTRAL ENERGY DISTRIBUTION OF GALAXIES | 2012年 / 284期

关键词：

stars: atmospheres; stars: abundances; techniques: spectroscopic; LIBRARY;

D O I：

10.1017/S1743921312008617

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Element abundance ratios hold important clues to understanding the evolution of stellar populations, through the varying timescales of different nucleosynthetic contributors. Newly measured and compiled [Mg/Fe] ratios in the MILES stellar library are used to confront models of star spectra. Such models have been used in recent years to provide estimates of differential changes in spectral line strengths, due to enhancements in [alpha/Fe]. In this paper we test one widely used set of theoretical element response functions. Using magnesium as a proxy for all alpha elements we test the reliability of these theoretical response functions against empirical observations, and thus the reliability of current methods of measuring element abundance ratios in the stellar populations.

引用

页码：12 / +

页数：2

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