Fundamental Properties of Young Binary Stars

TL;DR

This paper reviews the current state of resolving young binary star orbits using interferometry, highlighting the potential for improved measurements to test stellar evolution models.

Contribution

It compiles known pre-main-sequence spectroscopic binaries and discusses how enhanced interferometry can significantly improve mass measurements.

Findings

Few low-mass pre-main-sequence binaries have been resolved so far.

Modest improvements in interferometer sensitivity can increase the sample of well-measured young stars.

Enhanced measurements will help validate stellar evolution theories.

Abstract

Spatially resolving the orbits of double-lined spectroscopic binaries provides a way to measure the dynamical masses of the component stars. At the distances to the nearest star forming regions, high angular resolution techniques are required to resolve these short period systems. In this paper, I provide an overview of the few low-mass pre-main-sequence spectroscopic binaries that have been resolved thus far using long-baseline optical/infrared interferometers. I also compiled a list of known spectroscopic binaries in nearby star forming regions (Taurus, Orion, Ophiuchus, Scorpius-Centaurus, etc.) and show that with modest improvements in the sensitivity of interferometers with 200-300 meter baselines, we can build a significant set of pre-main sequence stars with precise mass determinations. This is important for validating and distinguishing among the theoretical calculations of evolution for young stars.