Sagittarius Aβ is a compact radio source at the center of the Milky Way
that has not conclusively shown evidence for the presence of a relativistic
jet. Nevertheless, indirect methods at radio frequencies do indicate consistent
outflow signatures. Brinkerink et al. (2015) found temporal shifts between
frequency bands, called time-lags, which are associated with flares and/or
outflows of the accretion system. It is possible to gain information on the
emission and potential outflow mechanics by interpreting these time-lags. By
means of combined general-relativistic magnetrohydrodynamical and radiative
transfer modeling, we study the origin of the time-lags for magnetically
arrested disc models at three black hole spins (aββ = 0.9375, 0, -0.9375).
The study also includes a targeted `slow light' study for one of the
best-fitting `fast light' windows. We were able to recover the time-lags found
by Brinkerink et al. (2015) in various windows of our simulated lightcurves.
The theoretical interpretation of these most-promising time-lag windows is
threefold; i) a magnetic flux eruption perturbs the jet-disc boundary and
creates a flux tube, ii) the flux tube orbits and creates a clear emission
feature, and iii) the flux tube interacts with the jet-disc boundary. The
best-fitting windows have an intermediate (i=30β/50β) inclination
and zero-BH-spin. The targeted `slow light' study did not yield better-fitting
time-lag results, which indicates that the fast vs. slow light paradign is
often not intuitively understood and is likely influential in timing-sensitive
studies.Comment: 17 pages, 11 figure