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Multi-spacecraft observations are used to study the in-situ effects of alarge CME erupting from the farside of the Sun on 3 November 2011, withparticular emphasis on the associated solar energetic particle (SEP) event. Atthat time both Solar Terrestrial Relations Observatory (STEREO) spacecraft werelocated more than 90 degrees from Earth and could observe the CME eruptiondirectly, with the CME visible on-disk from STEREO-B and off the limb fromSTEREO-A. Signatures of pressure variations in the corona such as deflectedstreamers were seen, indicating the presence of a coronal shock associated withthis CME eruption. The evolution of the CME and an associated EUV wave werestudied using EUV and coronagraph images. It was found that the lateralexpansion of the CME low in the corona closely tracked the propagation of theEUV wave, with measured velocities of 240+/-19 km/s and 221+/-15 km/s for theCME and wave respectively. Solar energetic particles were observed arrivingfirst at STEREO-A, followed by electrons at the Wind spacecraft at L1, thenSTEREO-B, and finally protons arriving simultaneously at Wind and STEREO-B. Bycarrying out velocity-dispersion analysis on the particles arriving at eachlocation, it was found that energetic particles arriving at STEREO-A werereleased first and the release of particles arriving at STEREO-B was delayed byaround 50 minutes. Analysis of the expansion of the CME to a wider longitudeindicates that this delay is a result of the time taken for the edge of the CMEto reach the footpoints of the magnetic-field lines connected to STEREO-B. TheCME expansion is not seen to reach the magnetic footpoint of Wind at the timeof solar particle release for the particles detected here, suggesting thatthese particles may not be associated with this CME.

An Investigation of the CME of 3 November 2011 and its Associated Widespread Solar Energetic Particle Event