Radiative damping of standing acoustic waves in solar coronal loops

Details Radiative damping of standing acoustic waves in solar coronal loops Radiative damping of standing acoustic waves in solar coronal loops

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...483..301b&link_type=abstract

Astronomy and Astrophysics, Volume 483, Issue 1, 2008, pp.301-309

Astronomy and Astrophysics

Astrophysics

5

Sun: Transition Region, Sun: Corona, Sun: Uv Radiation, Atomic Processes, Hydrodynamics

Scientific paper

Context: A detailed understanding of the physical processes that determine the damping timescales of magneto-acoustic waves is essential to interpret diagnostic results from the application of solar magneto-seismology. Aims: The influence of the transition region and the importance of radiative emission, arising from equilibrium and non-equilibrium ionisation balances, for the damping timescale of the fundamental mode standing acoustic wave is investigated. Methods: An extensive numerical study, in the framework of the field-aligned hydrodynamic approximation, is carried out of the damping of the fundamental mode standing wave in a solar coronal loop, for a wide range of loop lengths and apex temperatures. Results: It was found that the radiative emission arising from a non-equilibrium ionisation balance will always act to reduce the damping timescale (in comparison to the equilibrium case) and may do so by up to ~10%. The physics of the transition region is most crucial in determining the magnitude of the reduction of the damping timescale when a non-equilibrium ionisation balance is properly accounted for. Conclusions: The methods of solar magneto-seismology, in particular the tools of coronal seismology, may be used to estimate loop lengths to a reasonable degree of accuracy, although estimates of the apex temperature are significantly less reliable, and one should use alternative (e.g. spectroscopic) diagnostics instead.

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