  Sudden jets of collimated plasma arise from many locations on the Sun,
including active regions. The magnetic field along which a jet emerges is often
open to interplanetary space, offering a clear "escape route" for any
flare-accelerated electrons and making jets lucrative targets for studying
particle acceleration and the solar sources of transient heliospheric events.
Bremsstrahlung hard X-rays (HXRs) could, in principle, trace the accelerated
electrons that escape along the paths of the jets, but measurements of the
escaping electron beams are customarily difficult due to the low densities of
the corona. In this work, we augment HXR observations with gyrosynchrotron
emission observed in microwaves, as well as extreme ultraviolet (EUV) emission
and modeling to investigate flare-accelerated electrons in a coronal jet. HXR
and microwave data from RHESSI and OVSA, respectively, give complementary
insight into electron spectra and locations, including the presence of
accelerated electrons in the jet itself. High-time-resolution HXR data from the
Konus-Wind instrument suggest electron acceleration timescales on the order of
1 second or shorter. We model the energetic electron distributions in the GX
Simulator framework using SoHO/MDI, RHESSI, TRACE, and OVSA data as
constraints. The result is a modeled distribution, informed and constrained by
measurements, of accelerated electrons as they escape the Sun. Combining the
detection of microwave gyrosynchrotron emission from an open, rather than
closed, magnetic configuration, with realistic 3D modeling constrained by
magnetograms, EUV, and X-ray emission, we obtain the most stringent constraints
to date on the accelerated electrons within a solar jet.
