tokens: site at a coronal location at or above the looptop. Having said that, we note that some spectral evolution of the electrons injected at the looptop along with the pitch-angle distribution can still affect the exact delay values, while the field inclination is taken into account within our 3D model. We checked that an SHS evolution of the injected nonthermal electron spectrum, where the spectral index varies by a few percent, while the electrons are beamed along the magnetic field can reduce the TOF distance by a factor of two as needed. However, such a model does not contain any population of nonthermal electrons reflected back to the coronal portion of the flaring loop(s) needed to account for the microwave emission. From this, we conclude that an electron beam with a modest angular scatter, rather than an ideal field-aligned beam, is responsible for the observed deviation of the loop half-length from the estimated TOF distance. Such an angular distribution is capable of reducing their “effective” speed along the magnetic field typically by a factor of 1.5–3. As we noted above, some angular spread is also required to supply a population of the upward-reflected electrons needed to interpret the microwave data. However, an isotropic angular distribution does not look likely given that it assumes a rather large pitch angle of the majority of streaming electrons and, thus, efficient trapping, which is not observed. Thus, the data favor an anisotropic beam-like distribution of the accelerated electrons with a modest opening angle of 30°–40°. The mirror ratio m = 3 in Loop II of our 3D model; thus, the electrons launched downward at the pitch-angle θ ≲ 35° will not be reflected at the footpoint and, thus, will not contribute to the trapping. The mean parallel velocity for the electrons launched at the looptop at θ = 35° is . Electrons with θ ≳ 35° will be reflected and will contribute to the brightness peaks observed at 5.7 GHz from the LF–loop. The observed delay of 70 ms between 5.7 GHz peaks and 102.2–293.5 keV emission peaks, both produced by presumably 400 keV electrons, places the 5.7 GHz source at a distance ∼5 Mm from the mirror points at the bases of loop II. Microwave emission at 17 and 34 GHz delayed by 120 ms requires an additional time for the electrons to be transported from Loop II to Loop I and, perhaps, additional time for trapping in Loop I. Thus, the time delays are naturally consistent with the identified magnetic configuration of the flare and the TPP model in which the particles are injected at the looptop of Loop II and then propagate to produce the observed variety of the HXR and microwave components. 3.2. Accelerated Electron Population In Section 2.4 we determined the HXR spectrum of subpeaks to be a single power-law with the indexes about 2.4. This spectrum is injected during a subpeak in addition to a preexisting population of nonthermal electrons responsible for a gradual (background) component of the burst.
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