Emission in EUV: The coronal loops are observed in specific EUV wavelengths emitted by highly ionised atoms in the solar corona, such as iron (Fe) and neon (Ne). These emissions are characteristic of the temperatures and densities found in coronal loops.
Morphology: The coronal loops exhibit distinct shapes and structures, including arcades, fan loops, and helmet streamers. These structures are consistent with the magnetic field configurations and plasma dynamics in the corona.
Time evolution: Coronal loops show dynamic behaviour, evolving over time scales ranging from minutes to hours. This evolution is associated with changes in the underlying magnetic field and plasma conditions.
Consistency with models: Theoretical models of coronal heating and magnetic field configurations predict the existence of coronal loops. Observations of coronal loops are consistent with these models, providing empirical support for our understanding of the solar atmosphere.
Overall, the coronal loops observed in EUV images are real physical structures in the Sun's atmosphere, supported by multiple lines of evidence from observations and theoretical models.
