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Some of local sources of the slow solar wind can be associated withspectroscopically detected plasma outflows at edges of active regionsaccompanied with specific signatures in the inner corona. The EUV telescopes(e.g. SPIRIT/CORONAS-F, TESIS/CORONAS-Photon and SWAP/PROBA2) sometimesobserved extended ray-like structures seen at the limb above active regions in1MK iron emission lines and described as "coronal rays". To verify therelationship between coronal rays and plasma outflows, we analyze an isolatedactive region (AR) adjacent to small coronal hole (CH) observed by differentEUV instruments in the end of July - beginning of August 2009. On August 1 EISrevealed in the AR two compact outflows with the Doppler velocities V =10-30km/s accompanied with fan loops diverging from their regions. At the limb theARCH interface region produced coronal rays observed by EUVI/STEREO-A on July31 as well as by TESIS on August 7. The rays were co-aligned with open magneticfield lines expanded to the streamer stalks. Using the DEM analysis, it wasfound that the fan loops diverged from the outflow regions had the dominanttemperature of ~1 MK, which is similar to that of the outgoing plasma streams.Parameters of the solar wind measured by STEREO-B, ACE, WIND, STEREO-A wereconformed with identification of the ARCH as a source region at theWang-Sheeley-Arge map of derived coronal holes for CR 2086. The results of thestudy support the suggestion that coronal rays can represent signatures ofoutflows from ARs propagating in the inner corona along open field lines intothe heliosphere.

Signatures of the slow solar wind streams from active regions in the inner corona