Forward Modeling of Simulated Transverse Oscillations in Coronal Loops and the Influence of Background Emission

Abstract We simulate transverse oscillations in radiatively cooling coronal loops and forward-model their spectroscopic imaging signatures, paying attention to the influence of background emission. The are driven at one footpoint by a periodic velocity driver. A standing kink wave is subsequently formed loop cross section deformed due Kelvin–Helmholtz instability, resulting energy dissipation heating small scales. Besides motions, long-period longitudinal flow also generated ponderomotive force induced slow wave. then transform simulated straight semi-torus spectrometer emissions, mimicking observations Hinode/EIS SDO/AIA. find that oscillation amplitudes intensity different slit positions, but roughly same spectral lines or channels. X-t diagrams both Doppler width show signals. emission dramatically decreases velocity, making estimated kinetic two orders magnitude smaller than real value. Our results subtraction can help recover velocity. These helpful for further understanding observational signatures. However, they cast doubt on spectroscopically content waves using