The outflow history of two Herbig-Haro jets in RCW 36: HH 1042 and HH 1043

TL;DR

This study analyzes the outflow history of two Herbig-Haro jets in RCW 36, revealing variable outflow rates, jet launching asymmetries, and physical conditions, thereby providing insights into star formation processes across different stellar masses.

Contribution

It presents the first detailed spectral analysis of HH 1042 and HH 1043 jets in RCW 36, demonstrating variable outflow rates and jet launching asymmetries in intermediate-mass YSOs.

Findings

Measured mass outflow rates ~ 10^-7 Msun/yr

High accretion rate ~ 10^-6 Msun/yr for HH 1042

Outflow velocity varies on ~100-year timescales

Abstract

Jets around low- and intermediate-mass young stellar objects (YSOs) contain a fossil record of the recent accretion and outflow activity of their parent star-forming systems. We aim to understand whether the accretion/ejection process is similar across the entire stellar mass range of the parent YSOs. To this end we have obtained VLT/X-shooter spectra of HH 1042 and HH 1043, two newly discovered jets in the massive star-forming region RCW 36. HH 1042 is associated with the intermediate-mass YSO 08576nr292. Over 90 emission lines are detected in the spectra. High-velocity (up to 220 km/s) blue- and redshifted emission from a bipolar flow is observed in typical shock tracers. Low-velocity emission from the background cloud is detected in nebular tracers, including lines from high ionization species. We applied combined optical and infrared spectral diagnostic tools in order to derive the physical conditions (density, temperature, and ionization) in the jets. The measured mass outflow rates are Mjet ~ 10^-7 Msun/yr. We measure a high accretion rate for HH 1042 (Macc ~ 10^-6 Msun/yr) and Mjet/Macc ~ 0.1, comparable to low-mass sources and consistent with models for magneto-centrifugal jet launching. The knotted structure and velocity spread in both jets are interpreted as fossil signatures of a variable outflow rate. The mean velocities in both lobes of the jets are comparable, but the variations in Mjet and velocity in the two lobes are not symmetric, suggesting that the launching mechanism on either side of the accretion disk is not synchronized. For HH 1042, we have constructed an interpretative physical model with a stochastic or periodic outflow rate and a description of a ballistic flow as its constituents. The knotted structure and velocity spread can be reproduced qualitatively with the model, indicating that the outflow velocity varies on timescales on the order of 100 yr.