T Tauri Jet Physics Resolved Near The Launching Region with the Hubble Space Telescope

TL;DR

This study uses high-resolution HST spectra to analyze the physical conditions of jets near their launching points in five T Tauri stars, revealing detailed gas dynamics, density structures, and jet parameters crucial for understanding star formation.

Contribution

It provides the first resolved PV maps of electron density, ionization, and temperature in the jet collimation region close to the star, with detailed measurements of mass and angular momentum outflows.

Findings

Identification of high-density regions and asymmetries in jets.

Mass ejection-to-accretion ratio between 0.01 and 0.07.

Higher velocity jet components dominate mass and angular momentum transport.

Abstract

We present an analysis of the gas physics at the base of jets from five T Tauri stars based on high angular resolution optical spectra, using the Hubble Space Telescope Imaging Spectrograph (HST/STIS). The spectra refer to a region within 100 AU of the star, i.e. where the collimation of the jet has just taken place. We form PV images of the line ratios to get a global picture of the flow excitation. We then apply a specialised diagnostic technique to find the electron density, ionisation fraction, electron temperature and total density. Our results are in the form of PV maps of the obtained quantities, in which the gas behaviour is resolved as a function of both radial velocity and distance from the jet axis. They highlight a number of interesting physical features of the jet collimation region, including regions of extremely high density, asymmetries with respect to the axis, and possible shock signatures. Finally, we estimate the jet mass and angular momentum outflow rates, both of which are fundamental parameters in constraining models of accretion/ejection structures, particularily if the parameters can be determined close to the jet footpoint. Comparing mass flow rates for cases where the latter is available in the literature (i.e. DG Tau, RW Aur and CW Tau) reveals a mass ejection-to-accretion ratio of 0.01 - 0.07. Finally, where possible (i.e. DG Tau and CW Tau), both mass and angular momentum outflow rates have been resolved into higher and lower velocity jet material. For the clearer case of DG Tau, this revealed that the more collimated higher velocity component plays a dominant role in mass and angular momentum transport.