The X-ray puzzle of the L1551 IRS 5 jet

TL;DR

This study analyzes X-ray emissions from the L1551 IRS 5 protostellar jet over nearly a decade, revealing stable luminosity, proximity to the source, and temperature gradients, supporting shock-based models of jet emission.

Contribution

It provides the first spatially resolved spectral analysis of the jet's X-ray emission, demonstrating the stability and origin of the X-ray source near the protostar.

Findings

X-ray luminosity remains constant over almost a decade.

X-ray emission is localized near the driving source.

Plasma temperature decreases with distance from the source.

Abstract

Protostars are actively accreting matter and they drive spectacular, dynamic outflows, which evolve on timescales of years. X-ray emission from these jets has been detected only in a few cases and little is known about its time evolution. We present a new Chandra observation of L1551 IRS 5's jet in the context of all available X-ray data of this object. Specifically, we perform a spatially resolved spectral analysis of the X-ray emission and find that (a) the total X-ray luminosity is constant over almost one decade, (b) the majority of the X-rays appear to be always located close to the driving source, (c) there is a clear trend in the photon energy as a function of the distance to the driving source indicating that the plasma is cooler at larger distances and (d) the X-ray emission is located in a small volume which is unresolved perpendicular to the jet axis by Chandra. A comparison of our X-ray data of the L1551 IRS 5 jet both with models as well as X-ray observations of other protostellar jets shows that a base/standing shock is a likely and plausible explanation for the apparent constancy of the observed X-ray emission. Internal shocks are also consistent with the observed morphology if the supply of jet material by the ejection of new blobs is sufficiently constant. We conclude that the study of the X-ray emission of protostellar jet sources allows us to diagnose the innermost regions close to the acceleration region of the outflows.