English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Protostellar jets are tightly connected to the accretion process and regulatethe angular momentum balance of accreting star-disk systems. The DG Tau jet isone of the best-studied protostellar jets and contains plasma with temperaturesranging over three orders of magnitude within the innermost 50 AU of the jet.We present new Hubble Space Telescope (HST) far ultraviolet (FUV) long-slitspectra spatially resolving the C IV emission (T~1e5 K) from the jet for thefirst time, and quasi-simultaneous HST observations of optical forbiddenemission lines ([O I], [N II], [S II] and [O III]) and fluorescent H2 lines.The C IV emission peaks at 42 AU from the stellar position and has a FWHM of 52AU along the jet. Its deprojected velocity of around 200 km/s decreasesmonotonically away from the driving source. In addition, we compare our HSTdata with the X-ray emission from the DG Tau jet. We investigate therequirements to explain the data by an initially hot jet compared to localheating. Both scenarios indicate a mass loss by the T~1e5 K jet of ~1e-9Msun/year, i.e., between the values for the lower temperature jet (T~1e4 K) andthe hotter X-ray emitting part (T>1e6 K). However, a simple initially hot windrequires a large launching region (~1 AU), and we therefore favor localheating.

HST FUV C IV observations of the hot DG Tauri jet