# Excitation of flare-induced waves in coronal loops and the effects of radiative cooling

## TL;DR

This study investigates how hot plasma injections in coronal loops excite slow magnetoacoustic waves and examines the impact of radiative cooling on wave damping, using advanced 3D MHD models with realistic energy considerations.

## Contribution

It extends previous isothermal models by incorporating full energy equations with radiative losses, providing more realistic simulations of wave excitation and damping in coronal loops.

## Key findings

- Hot jets excite slow magnetoacoustic waves propagating along loops.
- Radiative cooling has a small effect on wave damping in 1-6 MK loops.
- Simulations support that observed disturbances are primarily wave phenomena.

## Abstract

EUV imaging observations from several space missions (SOHO/EIT, TRACE, and SDO/AIA) have revealed a presence of propagating intensity disturbances in solar coronal loops. These disturbances are typically interpreted as slow magnetoacoustic waves. Recent spectroscopic observations with Hinode/EIS of active region loops, however, revealed that the propagating intensity disturbances are associated with intermittent plasma upflows (or jets) at the footpoints which are presumably generated by magnetic reconnection. For this reason, whether these disturbances are waves or periodic flows is still being studied. This study is aimed at understanding the physical properties of observed disturbances by investigating the excitation of waves by hot plasma injections from below and the evolution of flows and wave propagation along the loop. We expand our previous studies based on isothermal 3D MHD models of active region to a more realistic model that includes full energy equation accounting for effects of radiative losses. Computations are initialized with an equilibrium state of a model active region using potential (dipole) magnetic field, gravitationally stratified density and temperature obtained from polytropic equation of state. We model an impulsive injection of hot plasma into the steady plasma outflow along the loops of different temperature, warm ($\sim$1 MK) and hot ($\sim$6 MK). The simulations show that hot jets launched at the coronal base excite slow magnetoacoustic waves that propagate along the loops to the high corona, while the injected hot flows decelerates rapidly with heights. The simulated results support that the observed coronal disturbances are mainly the wave features. We also find that the effect of radiative cooling on the damping of slow-mode waves in 1-6 MK coronal loops is small, in agreement with the previous conclusion based on 1D MHD models.