  We investigate the luminous star ELHC 10 located in the bar of the Large
Magellanic Cloud, concluding that it is a SB1 long-period eclipsing binary
where the main eclipse is produced by an opaque structure hiding the secondary
star. For the more luminous component we determine an effective temperature of
6500 $\pm$ 250 $K$, log\,g = 1.0 $\pm$ 0.5 and luminosity 5970 L$_{\sun}$. From
the radial velocities of their photospheric lines we calculate a mass function
of 7.37 $\pm$ 0.55 M$_{\sun}$. Besides Balmer and forbidden N II emission, we
find splitting of metallic lines, characterized by strong discrete absorption
components (DACs), alternatively seen at the blue and red side of the
photospheric spectrum. These observations hardly can be interpreted in terms of
an structured atmosphere but might reflect mass streams in an interacting
binary. The primary shows signatures of s-process nucleosynthesis and might be
a low-mass post-AGB star with a rare evolutionary past if the binary is
semi-detached. The peak separation and constancy of radial velocity in
H$\alpha$ suggest that most of the Balmer emission comes from a circumbinary
disc.
