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

Hot Jupiters are subject to strong irradiation from the host stars and, as aconsequence, they do evaporate. They can also interact with the parent stars bymeans of tides and magnetic fields. Both phenomena have strong implications forthe evolution of these systems. Here we present time resolved spectroscopy ofHD~189733 observed with the Cosmic Origin Spectrograph (COS) on board to HST.The star has been observed during five consecutive HST orbits, starting at asecondary transit of the planet ($\phi$ ~0.50-0.63). Two main episodes ofvariability of ion lines of Si, C, N and O are detected, with an increase ofline fluxes. Si IV lines show the highest degree of variability. The FUVvariability is a signature of enhanced activity in phase with the planetmotion, occurring after the planet egress, as already observed three times inX-rays. With the support of MHD simulations, we propose the followinginterpretation: a stream of gas evaporating from the planet is actively andalmost steadily accreting onto the stellar surface, impacting at $70-90\deg$ahead of the sub-planetary point.

FUV variability of HD 189733. Is the star accreting material from its hot Jupiter?