Collective Properties of X-ray Binary Populations of Galaxies II. Pre-Low-mass X-ray Binary Properties, Formation Rates, and Constraints

TL;DR

This paper investigates the formation and properties of pre-low-mass X-ray binaries (pre-LMXBs), focusing on their evolutionary pathways, constraints on their formation, and their collective properties to better understand LMXB populations in galaxies.

Contribution

It provides a detailed analysis of the formation rates and parameter distributions of pre-LMXBs, enhancing understanding of their evolution and role in galaxy X-ray binary populations.

Findings

Calculated the formation rate of pre-LMXBs.

Analyzed the evolution of binary parameters through key phases.

Identified constraints affecting pre-LMXB formation.

Abstract

We continue exploring our understanding of the collective properties of X-ray binaries in the stellar fields (i.e., outside globular clusters) of normal galaxies, introduced in Paper I of this series, where we considered high-mass X-ray binaries (HMXBs). In this paper (Paper II of the series) and the companion paper (Paper III of the series), we consider low-mass X-ray binaries (LMXBs), whose evolutionary scenario is very different from that of HMXBs. In this paper, we consider the evolution of primordial binaries upto the stage where the neutron star just formed in the supernova explosion of the primary is in a binary with its low-mass unevolved companion, and this binary has circularized tidally, producing what we call a pre-low-mass X-ray binary (pre-LMXB). We study the constraints on the formation of such pre-LMXBs in detail (since these are low probability events), and calculate their collective properties and formation rate. To this end, we first consider the changes in the binary parameters in the various steps involved, viz., the common-envelope (CE) phase, the supernova, and the tidal evolution. This naturally leads to a clarification of the constraints. We then describe our calculation of the evolution of the distributions of primordial binary parameters into those of the pre-LMXB parameters, following the standard evolutionary scenario for individual binaries. We display the latter as both bivariate and monovariate distributions, discuss their essential properties, and indicate the influence of some essential factors on these. Finally, we calculate the formation rate of pre-LMXBs. The results of this paper are used in the next one (Paper III) to compute the expected X-ray luminosity function (XLF) of LMXBs, which is compared with observation.