  WD0810-353 is a white dwarf within the 20pc volume around the Sun. Using Gaia
astrometric distance and proper motions, and a radial velocity derived from
Gaia spectroscopy, it has been predicted that this star will pass within 1pc of
the Solar System in about 30kyr. However, WD0810-353 has been also shown to
host a magnetic field with strength of the order of 30MG. Its spectrum is
therefore not like those of normal DA stars of similar effective temperature.
We have obtained and analysed new polarised spectra of the star around Halpha.
Our analysis suggests that the visible surface of the star shows two regions of
different field strength (~30 and ~45MG, respectively), and opposite polarity.
The spectra do not change over a 4 year time span, meaning that either the
stellar rotation period is no shorter than several decades, or that the field
is symmetric about the rotation axis. Taking into account magnetic shift and
splitting, we obtain an estimate of the radial velocity of the star (+83+/-
140km/s); we reject both the value an the claimed precision deduced from the
Gaia DR3 spectroscopy (-373.7+/- 8.2km/s), and we conclude that there will
probably be no close encounter between the Solar System and WD0810-353. We also
reject the suggestion that the star is a hypervelocity runaway star, a survivor
of a Type Ia Supernova explosion. It is just a stellar remnant in the Solar
neighborhood with a very strong and complex magnetic field.
