On the detection of shocks in the solar granulation.

Details On the detection of shocks in the solar granulation. On the detection of shocks in the solar granulation.

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...308..623s&link_type=abstract

Astronomy and Astrophysics, v.308, p.623-630

Astronomy and Astrophysics

Astrophysics

34

Convection, Sun: Granulation, Line: Profiles, Hydrodynamics, Shocks

Scientific paper

We investigate the spectral signature of a hydrodynamic simulation of solar granulation and compare it with high resolution observations. The model gives the correct qualitative trend of increasing line width with decreasing continuum intensity seen by Nesis et al. (1992) and interpreted by them as a sign of post-shock turbulence. We find, however, that the profiles in the dark downflow lanes are broader even when there is no horizontal transonic flow or shock in the vicinity. We conclude that the observations of Nesis et al. do not provide any firm evidence for the presence of granular transonic flows. Nevertheless, the simulation predicts a promising diagnostic of shocked horizontal flows. We find that at the locations of the shocks the line profiles are particularly broad, especially near the solar limb. We present observations of quiet solar regions that show this specific signature of shocks and thus support the theoretical prediction of transonic granular flows.

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