Hot channel ( HC ) is a high temperature ( \sim 10 MK ) structure in the inner corona revealed first by Atmospheric Imaging Assembly ( AIA ) on board Solar Dynamics Observatory .
Eruption of HC is often associated with flare and coronal mass ejection .
Previous studies suggest that HC is a good proxy of magnetic flux rope ( MFR ) in the inner corona , in addition to another well-known MFR candidate , the prominence-cavity structure that is with a normal coronal temperature ( \sim 1-2 MK ) .
In this paper , we report a high temperature structure ( HTS , \sim 1.5 MK ) contained in an interplanetary coronal mass ejection induced by an HC eruption .
According to the observations of bidirectional electrons , high temperature and density , strong magnetic field , and its association with the shock , sheath , and plasma pile-up region , we suggest that the HTS is the interplanetary counterpart of the HC . The scale of the measured HTS is around 14 R _ { \odot } , and it maintained a much higher temperature than the background solar wind even at 1 AU .
It is significantly different from the typical magnetic clouds ( MCs ) , which usually have a much lower temperature . Our study suggests that the existence of a corotating interaction region ahead of the HC formed a magnetic container to inhibit the HC expansion and cooling down to a low temperature .