  We present radio [1.3 GHz MeerKAT, 4-8 GHz Karl G. Jansky Very Large Array
(VLA) and 15.5 GHz Arcminute Microkelvin Imager Large Array (AMI-LA)] and X-ray
(Swift and MAXI) data from the 2019 outburst of the candidate Black Hole X-ray
Binary (BHXB) EXO 1846-031. We compute a Hardness-Intensity diagram, which
shows the characteristic q-shaped hysteresis of BHXBs in outburst. EXO 1846-031
was monitored weekly with MeerKAT and approximately daily with AMI-LA. The VLA
observations provide sub-arcsecond-resolution images at key points in the
outburst, showing moving radio components. The radio and X-ray light curves
broadly follow each other, showing a peak on ~MJD 58702, followed by a short
decline before a second peak between ~MJD 58731-58739. We estimate the minimum
energy of these radio flares from equipartition, calculating values of $E_{\rm
min} \sim$ 4$\times$10$^{41}$ and 5$\times$10$^{42}$ erg, respectively. The
exact date of the return to `quiescence' is missed in the X-ray and radio
observations, but we suggest that it likely occurred between MJD 58887 and
58905. From the Swift X-ray flux on MJD 58905 and assuming the soft-to-hard
transition happened at 0.3-3 per cent Eddington, we calculate a distance range
of 2.4-7.5\,kpc. We computed the radio:X-ray plane for EXO 1846-031 in the
`hard' state, showing that it is most likely a `radio-quiet' BH, preferentially
at 4.5 kpc. Using this distance and a jet inclination angle of
$\theta$=73$^{\circ}$, the VLA data place limits on the intrinsic jet speed of
$\beta_{\rm int} = 0.29c$, indicating sub-luminal jet motion.

High Energy Astrophysical Phenomena