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Solar flare electron acceleration is an efficient process, but its properties(mechanism, location) are not well constrained. Via hard X-ray (HXR) emission,we routinely observe energetic electrons at the Sun, and sometimes we detectenergetic electrons in interplanetary space. We examine if the plasmaproperties of an acceleration region (size, temperature, density) can beconstrained from in-situ observations, helping to locate the accelerationregion in the corona, and infer the relationship between electrons observedin-situ and at the Sun. We model the transport of energetic electrons,accounting for collisional and non-collisional effects, from the corona intothe heliosphere (to 1.0 AU). In the corona, electrons are transported through ahot, over-dense region. We test if the properties of this region can beextracted from electron spectra (fluence and peak flux) at differentheliospheric locations. We find that cold, dense coronal regions significantlyreduce the energy at which we see the peak flux and fluence for distributionsmeasured out to 1.0 AU, the degree of which correlates with the temperature anddensity of plasma in the region. Where instrument energy resolution isinsufficient to differentiate the corresponding peak values, the spectral ratioof [7-10) to [4-7) keV can be more readily identified and demonstrates the samerelationship. If flare electrons detected in-situ are produced in, and/ortransported through hot, over-dense regions close to HXR-emitting electrons,then this plasma signature should be present in their lower-energy spectra(1-20 keV), observable at varying heliospheric distances with missions such asSolar Orbiter.

Exploring the Origin of Solar Energetic Electrons I: Constraining the Properties of the Acceleration Region Plasma Environment