Kroupa (1995a)

Abstract (paraphrased)¶

All stars are taken to form in binary systems; the observed Galactic-field population (~50–60% binaries) then emerges from the dynamical evolution of binary-rich embedded clusters. Kroupa derives the birth orbital-parameter distributions by inverse dynamical population synthesis: assume an initial period distribution flat in $\log_{10}P$ over $3 < \log_{10}P \le 7.5$ (P in days), an uncorrelated birth mass-ratio distribution, and the three-segment IMF; distribute $N_{\rm bin}=200$ binaries in clusters of half-mass radius ~0.08–2.5 pc (tightly clustered → isolated); and follow the subsequent evolution by direct $N$-body integration. The evolved population reproduces the observed field binaries (e.g. the $\log_{10}P > 4$ period distribution) for clusters of $R_{0.5}\approx 0.8$ pc.

Use in progenax¶

• progenax.imf.binary (imf.py) — cited as the IMF-consistent birth binary-population framework (period distribution flat in $\log_{10}P$), alongside Moe & Di Stefano (2017).