The age of cataclysmic variables: a kinematical study

TL;DR

This study analyzes the kinematical properties of cataclysmic variables using astrometric and radial velocity data, revealing their ages, evolutionary differences, and velocity dispersions, which support and refine existing theories of CV evolution.

Contribution

It provides a refined kinematical age estimate for CVs and their subgroups, and compares observed age differences with standard evolutionary models.

Findings

CVs have a mean age of 5±1 Gyr.

Non-magnetic CVs are younger, with an age of 4±1 Gyr.

CVs below the period gap are older than those above, consistent with evolution theory.

Abstract

Using available astrometric and radial velocity data, the space velocities of cataclysmic variables (CVs) with respect to Sun were computed and kinematical properties of various sub-groups of CVs were investigated. Although observational errors of systemic velocities ($\gamma$) are high, propagated errors are usually less than computed dispersions. According to the analysis of propagated uncertainties on the computed space velocities, available sample is refined by removing the systems with the largest propagated uncertainties so that the reliability of the space velocity dispersions was improved. Having a dispersion of $51\pm7$ km s$^{-1}$ for the space velocities, CVs in the current refined sample (159 systems) are found to have $5\pm1$ Gyr mean kinematical age. After removing magnetic systems from the sample, it is found that non-magnetic CVs (134 systems) have a mean kinematical age of $4\pm1$ Gyr. According to $5\pm1$ and $4\pm1$ Gyr kinematical ages implied by $52\pm8$ and $45\pm7$ km s$^{-1}$ dispersions for non-magnetic systems below and above the period gap, CVs below the period gap are older than systems above the gap, which is a result in agreement with the standard evolution theory of CVs. Age difference between the systems below and above the gap is smaller than that expected from the standard theory, indicating a similarity of the angular momentum loss time scales in systems with low-mass and high-mass secondary stars. Assuming an isotropic distribution, $\gamma$ velocity dispersions of non-magnetic CVs below and above the period gap are calculated $\sigma_\gamma=30\pm5$ km s$^{-1}$ and $\sigma_\gamma=26\pm4$ km s$^{-1}$.