  Accreting neutron stars in low-mass X-ray binaries show outflows -- and
sometimes jets -- in the general manner of accreting black holes. However, the
quantitative link between the accretion flow (traced by X-rays) and outflows
and/or jets (traced by radio emission) is much less well-understood for neutron
stars than for black holes, other than the general observation that neutron
stars are fainter in the radio at a given X-ray luminosity. We use data from
the deep MAVERIC radio continuum survey of Galactic globular clusters for a
systematic radio and X-ray study of six luminous (L_X > 10^34 erg/s) persistent
neutron star X-ray binaries in our survey, as well as two other transient
systems also captured by our data. We find that these neutron star X-ray
binaries show an even larger range in radio luminosity than previously
observed. In particular, in quiescence at L_X ~ 3x10^34 erg/s, the confirmed
neutron star binary GRS 1747--312 in Terzan 6 sits near the upper envelope of
the black hole radio/X-ray correlation, and the persistently accreting neutron
star systems AC 211 (in M15) and X1850--087 (in NGC 6712) show unusual radio
variability and luminous radio emission. We interpret AC 211 as an obscured "Z
source" that is accreting at close to the Eddington limit, while the properties
of X1850--087 are difficult to explain, and motivate future coordinated radio
and X-ray observations. Overall, our results show that neutron stars do not
follow a single relation between inflow and outflow, and confirm that their
accretion dynamics are more complex than for black holes.
