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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Context: A large sample of T Tauri stars exhibits optical jets, approximatelyhalf of which rotate slowly, only at ten per cent of their breakup velocity.The disk-locking mechanism has been shown to be inefficient to explain thisobservational fact.  Aims: We show that low mass accreting T Tauri stars may have a strong stellarjet component that can effectively brake the star to the observed rotationspeed.  Methods: By means of a nonlinear separation of the variables in the full setof the MHD equations we construct semi- analytical solutions describing thedynamics and topology of the stellar component of the jet that emerges from thecorona of the star.  Results: We analyze two typical solutions with the same mass loss rate butdifferent magnetic lever arms and jet radii. The first solution with a longlever arm and a wide jet radius effectively brakes the star and can be appliedto the visible jets of T Tauri stars, such as RY Tau. The second solution witha shorter lever arm and a very narrow jet radius may explain why similar stars,either Weak line T Tauri Stars (WTTS) or Classical T Tauri Stars (CTTS) do notall have visible jets. For instance, RY Tau itself seems to have differentphases that probably depend on the activity of the star.  Conclusions: First, stellar jets seem to be able to brake pre-main sequencestars with a low mass accreting rate. Second, jets may be visible only parttime owing to changes in their boundary conditions. We also suggest a possiblescenario for explaining the dichotomy between CTTS and WTTS, which rotatefaster and do not have visible jets.

Nonradial and nonpolytropic astrophysical outflows IX. Modeling T Tauri jets with a low mass-accretion rate