Evolutionary population synthesis for binary stellar populations

Abstract

Abstract. We present integrated colours, integrated spectral energy distributions, and absorption-line indices, for instantaneous burst solar-metallicity binary stellar populations with ages in the range 1−15 Gyr. By comparing the results for populations with and without binary interactions we show that the inclusion of binary interactions makes the appearance of the population substantially bluer -this is the case for each of the quantities we have considered. This effect raises the derived age and metallicity of the population. Therefore it is necessary to consider binary interactions in order to draw accurate conclusions from evolutionary population synthesis work.

Population synthesis in astrophysics

“…Only in late 90s several groups of authors started to include binaries in their models (see [129] and references therein). Among recent papers we want to mention [130] and a review in [131].…”

Star clusters and single stellar populations

“…Just like the synthetic ISED of a star cluster, the ISED of a binary population is enhanced at shorter wavelengths compared with the conventional SSP model, as shown in Figure 3 (left). This enhancement is systematic in the model grid (see Zhang et al 2004).…”

“…There are two channels of BS formation related to interactions in close binaries, mass exchange between the components (Zhang et al 2004(Zhang et al , 2005Tian et al 2006;Lu et al 2009) and coalescence (Chen & Han 2009), which will eventually happen in some close binary systems. Thanks to recent advances in studies of binary evolution, population synthesis involving binaries ('binary synthesis') can be done.…”

Explanation of a Special Color–magnitude Diagram of Star Cluster NGC 1651 From Different Models

“…We construct synthetic CMDs following previously cited works (e.g., Zhang et al 2004;Li & Han 2008a, 2008bLi et al 2012a). Simple and composite stellar populations (SSPs and CSPs) are built by taking the initial mass function (IMF) of Salpeter (1955) with lower and upper mass limits of 0.1 and 100  M , respectively.…”