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Hot channels (HCs), high temperature erupting structures in the lower coronaof the Sun, have been proposed as a proxy of magnetic flux ropes (MFRs) sincetheir initial discovery. However, it is difficult to make definitive proofgiven the fact that there is no direct measurement of magnetic field in thecorona. An alternative way is to use the magnetic field measurement in thesolar wind from in-situ instruments. On 2012 July 12, an HC was observed priorto and during a coronal mass ejection (CME) by the AIA high-temperature images.The HC is invisible in the EUVI low-temperature images, which only show thecooler leading front (LF). However, both the LF and an ejecta can be observedin the coronagraphic images. These are consistent with the high temperature andhigh density of the HC and support that the ejecta is the erupted HC. In themeanwhile, the associated CME shock was identified ahead of the ejecta and thesheath through the COR2 images, and the corresponding ICME was detected by\textit{ACE}, showing the shock, sheath and magnetic cloud (MC) sequentially,which agrees with the coronagraphic observations. Further, the MC contained alow-ionization-state center and a high-ionization-state shell, consistent withthe pre-existing HC observation and its growth through magnetic reconnection.All of these observations support that the MC detected near the Earth is thecounterpart of the erupted HC in the corona for this event. Therefore, ourstudy provides strong observational evidence of the HC as an MFR.

Evidence of the Solar EUV hot channel as a magnetic flux rope from remote-sensing and in-situ observations