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

TOI-849b is one of the few planets populating the hot-Neptune desert and itis the densest Neptune-sized one discovered so far. Its extraordinary proximityto the host star, together with the absence of a massive H/He envelope on topof the $40.8 ~M_{\oplus}$ rocky core calls into question the role played by thehost star in the evolution of the system. We aim to study the impact of thehost star's rotational history on the evolution of TOI-849b, focussing on theplanetary migration due to dynamical tides dissipated in the stellar convectiveenvelope and on the high-energy emission. Rotating stellar models of TOI-849are coupled to our orbital evolution code to study the evolution of theplanetary orbit. The evolution of the planetary atmosphere is studied by meansof the JADE code, which uses realistic XUV-fluxes provided by our rotatingstellar models. Assuming that the planet was at its present day position($a=0.01598 \rm AU$) at the protoplanetary disc dispersal, with mass $40.8~M_{\oplus}$, and considering a broad range of host star initial surfacerotation rates ($\Omega_{\rm in}$) in the range $ [3.2, 18]~ \Omega_{\odot}$,we find that only for $\Omega_{\rm in} \leq 5 \Omega_{\odot}$ do we reproducethe current position of the planet, given that for $\Omega_{\rm in}$ largerthan $5 \Omega_{\odot}$ its orbit is efficiently deflected by dynamical tides.We tested the impact of increasing the initial mass of the planet on theefficiency of tides, finding that a higher initial mass ($1~M_{\rm Jup}$) doesnot change the results reported above. Based on these results we computed theevolution of the planetary atmospheres with the JADE code for a large range ofinitial masses above a core mass of $40.8~M_{\oplus}$, finding that the strongXUV-flux received by the planet is able to remove the entirety of the envelopewithin the first 50 Myr, even if it formed as a Jupiter-mass planet.

The key impact of the host star's rotational history on the evolution of TOI-849b