1Bitterroot Basic Research, Hamilton, MT, USA
2Heliospheric Physics Laboratory, Code 672, NASA Goddard Space Flight
Center, Greenbelt, MD, USA
Received: 17 Jun 2016 – Revised: 28 Nov 2016 – Accepted: 12 Dec 2016 – Published: 05 Jan 2017
Abstract. It is not uncommon during periods when the solar wind speed is less than 425 km s−1 to observe near 1 AU no evidence of a strahl population in either the electron solar wind or within the foreshock. Estimating the fluid flow within each energy step returned from the Plasma Electron And Current Experiment (PEACE) on board Cluster-2 often finds that in slow wind the GSE spherical flow angles in energies above where there is a clear core/halo signature are often close to radial with no evidence of a field-aligned flow. This signifies the lack of a strahl presence in the electron velocity distribution function (eVDF). When there is no obvious strahl signature in the data, the electrons above the core/halo in energy appear to be unstructured and smeared in angle. This can either be interpreted as due to statistical noise in low counting rate situations or the result of intense scattering. Regions where the strahl is seen and not seen are often separated by a very thin boundary layer. These transitions in the spacecraft frame of reference can be quite rapid, generally occurring within one to two spins (4–8 s).
Gurgiolo, C. and Goldstein, M. L.: Absence of the strahl during times of slow wind, Ann. Geophys., 35, 71-85, doi:10.5194/angeo-35-71-2017, 2017.