LBA observations for project V586 semester 2019OCTS

We are requesting LBA time at 8.4 GHz to observe the flare dwarf binary UV Ceti (M6.0) and BL Ceti (M5.5). The system's proximity (2.7 pc) and UV Ceti's known coronal radio emission make this system an excellent laboratory to study the enhanced magnetic activity in the M dwarf stellar class. Given that the latter are associated with the majority of exoplanets detected to date, how their associated 'space weather' impacts long term habitability remains an outstanding problem in modern astronomy. Prior VLBA observations at 8.4 GHz in 1996 resolved two extended lobe like structures extending 4 stellar radii around UV Ceti, consistent with radio emitting electrons trapped within large coronal loops. The inability to accurately register the radio data against the actual stellar position at the time limited rigorous physical interpretation of the local physical conditions associated with the emitting gyrosynchrotron populations. Using the latest GAIA DR2 catalogue the astrometry of this binary system's components is now known to ~ 0.2mas. Any LBA detected radio emitting sources can now be anchored to the underlying stellar photosphere, resolving these earlier uncertainties. Tracking fixed coronal structures over the timeframe of the observations could provide estimates of UV Ceti's rotation rate, and changes in coronal topology used to test changing magnetic cycles in this M dwarf since earlier observational epochs. A particular advantage of using the LBA is significantly enhanced astrometry given our proposed target's declination at -17 degrees.