  The enigmatic and intriguing phenomenon of the "soft excess" observed in the
X-ray spectra of luminous quasars continues to be a subject of considerable
interest and debate in the field of high-energy astrophysics. This study
focuses on the quasar HE 1029-1401 ($z=0.086$,
$\log(L_{\rm{bol}}/[\rm{erg\,s^{-1}}])= 46.0 \pm 0.2$), with a particular
emphasis on investigating the properties of the hot corona and the physical
origin of the soft excess. In this study, we present the results of a joint
\textit{XMM-Newton}/\textit{NuSTAR} monitoring campaign of this quasar
conducted in May 2022. The source exhibits a cold and narrow Fe $\rm{K}\alpha$
emission line at 6.4 keV, in addition to the detection of a broad component.
Our findings suggest that the soft excess observed in HE 1029-1401 can be
adequately explained by Comptonized emission originating from a warm corona.
Specifically, fitting the spectra with two \nthcomp\, component we found that
the warm corona is characterized by a photon index ($\Gamma^{w}$) of
$2.75\pm0.05$ and by an electron temperature ($kT_{e}^{w}$) of
$0.39^{+0.06}_{-0.04}$ keV, while the optical depth ($\tau^{w}$) is found to be
$23\pm3$. We also test more physical models for the warm corona, corresponding
to two scenarios: pure Comptonization and Comptonization plus reflection. Both
models provide a good fit to the data, and are in agreement with a radially
extended warm corona having a size of a few tens of gravitational radii.
