PARSEC：用Padova和TRieste恒星演化代码进行恒星轨迹和等时线
PARSEC: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code
摘要：
我们提出了更新版本的代码用于计算恒星在帕多瓦的进化轨迹。这是对主要输入物理进行彻底修订的结果，同时包含了前主序星阶段，这在我们以前发布的恒星模型中是不存在的。另一个创新方面是通过将高温下的OPAL不透明度数据与我们的AESOPUS代码计算的分子不透明度相结合，可以迅速生成与任何选定的初始化学成分完全一致的准确不透明度表（Marigo & Aringer 2009）。在这项工作中，我们提出了各种初始化学成分的恒星演化模型的扩展集，而其他集不同的金属丰度和/或不同的重元素分布正在计算。对于目前发布的模型，我们采用了Caffau等人（2011）最近修订的重元素太阳分布，对应于太阳的金属丰度Z=0.0152。从所有计算的恒星轨迹集，我们也得到在几个光度系统的等时线。其目的是为社区提供基本工具，通过人口合成技术模拟星团和星系。
英文摘要：
We present the updated version of the code used to compute stellar evolutionary tracks in Padova. It is the result of a thorough revision of the major input physics, together with the inclusion of the pre-main sequence phase, not present in our previous releases of stellar models. Another innovative aspect is the possibility of promptly generating accurate opacity tables fully consistent with any selected initial chemical composition, by coupling the OPAL opacity data at high temperatures to the molecular opacities computed with our AESOPUS code (Marigo & Aringer 2009). In this work we present extended sets of stellar evolutionary models for various initial chemical compositions, while other sets with different metallicities and/or different distributions of heavy elements are being computed. For the present release of models we adopt the solar distribution of heavy elements from the recent revision by Caffau et al. (2011), corresponding to a Sun's metallicity Z=0.0152. From all computed sets of stellar tracks, we also derive isochrones in several photometric systems. The aim is to provide the community with the basic tools to model star clusters and galaxies by means of population synthesis techniques.
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