Disc wind in the HH 30 binary models

TL;DR

This study models low velocity disc winds in the HH 30 binary system to explain observed molecular outflows, finding that short orbital periods produce outflows consistent with observations.

Contribution

It introduces two binary models of disc winds for HH 30, demonstrating that short orbital periods yield outflow structures matching observations.

Findings

Short orbital periods produce symmetric outflows.

Long orbital periods result in spiral-like outflow structures.

Models with P ≤ 1 yr align with observed outflow symmetry.

Abstract

Recent interferometric observations of the young stellar object(YSO) HH 30 have revealed a low velocity outflow in the $^{12}$CO J=1-2 molecule line (Pety et al. 2006). We present here two models of the low velocity disc winds with the aim of investigating an origin of this molecular outflow. Following Andlada et al. (2006) we treated HH 30 as a binary system. Two cases have been considered: i) the orbital period $P$ = 53 yrs and ii) $P \le$ 1 yr. Calculations showed that in the first case the outflow cone had a spiral-like structure due to summing the velocities of the orbital motion and the disc wind. Such a structure contradicts the observations. In the second case, the outflow cone demonstrates a symmetry relatively to the system axis and agrees well with the observations.