  TOI-849b is one of the few planets populating the hot-Neptune desert and it
is the densest Neptune-sized one discovered so far. Its extraordinary proximity
to the host star, together with the absence of a massive H/He envelope on top
of the $40.8 ~M_{\oplus}$ rocky core calls into question the role played by the
host star in the evolution of the system. We aim to study the impact of the
host star's rotational history on the evolution of TOI-849b, focussing on the
planetary migration due to dynamical tides dissipated in the stellar convective
envelope and on the high-energy emission. Rotating stellar models of TOI-849
are coupled to our orbital evolution code to study the evolution of the
planetary orbit. The evolution of the planetary atmosphere is studied by means
of the JADE code, which uses realistic XUV-fluxes provided by our rotating
stellar 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 surface
rotation 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 reproduce
the current position of the planet, given that for $\Omega_{\rm in}$ larger
than $5 \Omega_{\odot}$ its orbit is efficiently deflected by dynamical tides.
We tested the impact of increasing the initial mass of the planet on the
efficiency of tides, finding that a higher initial mass ($1~M_{\rm Jup}$) does
not change the results reported above. Based on these results we computed the
evolution of the planetary atmospheres with the JADE code for a large range of
initial masses above a core mass of $40.8~M_{\oplus}$, finding that the strong
XUV-flux received by the planet is able to remove the entirety of the envelope
within the first 50 Myr, even if it formed as a Jupiter-mass planet.
