The excitation of 5-min oscillations in the solar corona

Abstract

We aim to study excitation of the observed 5-min oscillations in the solar corona by localized pulses that are launched in the photosphere. We solve the full set of nonlinear one-dimensional Euler equations numerically for the velocity pulse propagating in the solar atmosphere that is determined by the realistic temperature profile. Numerical simulations show that an initial velocity pulse quickly steepens into a leading shock, while the nonlinear wake in the chromosphere leads to the formation of consecutive pulses. The time interval between arrivals of two neighboring pulses to a detection point in the corona is approximately 5 min. Therefore, the consecutive pulses may result in the 5-min oscillations that are observed in the solar corona. The 5-min oscillations observed in the solar corona can be explained in terms of consecutive shocks that result from impulsive triggers launched within the solar photosphere by granulation and/or reconnection.

5 pages, 2 figures, accepted in A&A

References in corpus (3)

• Numerical simulations of spicule formation in the solar atmosphere
• Intensity oscillations observed with Hinode near the south pole of the Sun: leakage of low frequency magneto-acoustic waves into the solar corona
• Two-wave interaction in ideal magnetohydrodynamics

Cited by in corpus (6)

• Frequency drifts of 3-min oscillations in microwave and EUV emission above sunspots
• Magnetohydrodynamic waves driven by p-modes
• Oscillation of solar radio emission at coronal acoustic cut-off frequency
• Observation of kink waves and their reconnection-like origin in solar spicules
• Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade
• A Scenario for Origin of Global 4 mHz Oscillations in Solar Corona