  How structures, e.g., magnetic loops, in the upper atmosphere, i.e., the
transition region and corona, are heated and sustained is one of the major
unresolved issues in solar and stellar physics. Various theoretical and
observational studies on the heating of coronal loops have been undertaken. The
heating of quiescent loops caused by eruptions is, however, rarely observed. In
this study, employing data from the Solar Dynamics Observatory (SDO) and Solar
Upper Transition Region Imager (SUTRI), we report the heating of quiescent
loops associated with nearby eruptions. In active regions (ARs) 13092 and
13093, a long filament and a short filament, and their overlying loops are
observed on 2022 September 4. In AR 13093, a warm channel erupted toward the
northeast, whose material moved along its axis toward the northwest under the
long filament, turned to the west above the long filament, and divided into two
branches falling to the solar surface. Subsequently, the short filament erupted
toward the southeast. Associated with these two eruptions, the quiescent loops
overlying the long filament appeared in SDO/Atmospheric Imaging Assembly (AIA)
high-temperature images, indicating the heating of loops. During the heating,
signature of magnetic reconnection between loops is identified, including the
inflowing motions of loops, and the formation of X-type structures and newly
reconnected loops. The heated loops then cooled down. They appeared
sequentially in AIA and SUTRI lower-temperature images. All the results suggest
that the quiescent loops are heated by reconnection between loops caused by the
nearby warm channel and filament eruptions.
