  In this paper, we present a detailed morphological, kinematic, and thermal
analysis of two homologous magnetic flux ropes (MFRs) from NOAA 11515 on 2012
July 8--9. The study is based on multi-wavelength and dual-perspective imaging
observations from the Solar Dynamics Observatory and the Solar Terrestrial
Relations Observatory Ahead spacecraft, which can well reveal the structure and
evolution of the two MFRs. We find that both of the MFRs show up in multiple
passbands and their emissions mainly consist of a cold component peaking at a
temperature of $\sim$0.4--0.6 MK and a hot component peaking at $\sim$7--8 MK.
The two MFRs exhibit erupting, expanding, and untwisting motions that manifest
distinctive features from two different viewpoints. Their evolution can be
divided into two stages, a fast-eruption stage with speeds of about 105--125 km
s$^{-1}$ for MFR-1 and 50--65 km s$^{-1}$ for MFR-2 and a slow-expansion (or
untwisting) stage with speeds of about 10--35 km s$^{-1}$ for MFR-1 and 10--30
km s$^{-1}$ for MFR-2 in the plane of sky. We also find that during the
two-stage evolution, the high temperature features mainly appear in the
interface region between MFRs and ambient magnetic structures and also in the
center of MFRs, which suggests that some heating processes take place in such
places like magnetic reconnection and plasma compression. These observational
results indicate that the eruption and untwisting processes of MFRs are coupled
with the heating process, among which an energy conversion exists.
