# Observational constraints on dust disk sizes in tidally truncated protoplanetary disks in multiple systems in the Taurus region

## TL;DR

This study uses high-resolution ALMA observations to analyze dust disk sizes in multiple stellar systems in Taurus, revealing that such disks are smaller and more truncated than those around single stars, influenced by tidal interactions.

## Contribution

It provides the first detailed spatially resolved analysis of dust disks in multiple systems in Taurus, demonstrating the impact of tidal truncation and high binary eccentricities on disk sizes.

## Key findings

- Disks in multiple systems are smaller than in single stars.
- Disk outer edges show steeper millimeter emission decay.
- Dust radii are consistent with high binary eccentricities or smaller gas radii.

## Abstract

The impact of stellar multiplicity on the evolution of planet-forming disks is still the subject of debate. Here we present and analyze disk structures around ten multiple stellar systems that were included in an unbiased, high spatial resolution survey performed with ALMA of 32 protoplanetary disks in the Taurus star-forming region. At the unprecedented spatial resolution of ~0.12" we detect and spatially resolve the disks around all primary stars, and those around eight secondary and one tertiary star. The dust radii of disks around multiple stellar systems are smaller than those around single stars in the same stellar mass range and in the same region. The disks in multiple stellar systems also show a steeper decay of the millimeter continuum emission at the outer radius than disks around single stars, suggestive of the impact of tidal truncation on the shape of the disks in multiple systems. However, the observed ratio between the dust disk radii and the observed separation of the stars in the multiple systems is consistent with analytic predictions of the effect of tidal truncation only if the eccentricities of the binaries are rather high (typically >0.5), or if the observed dust radii are a factor of two smaller than the gas radii, as is typical for isolated systems. Similar high-resolution studies targeting the gaseous emission from disks in multiple stellar systems are required to resolve this question.