Oscillations in the Solar Faculae. III. The Phase Relations between Chromospheric and Photospheric LOS Velocities

Abstract

An analysis of line-of-sight velocity oscillation in nine solar faculae was undertaken with the aim of studying of phase relations between chromosphere (He i 10830 A line) and photosphere (Si i 10827 A line) five-minute oscillations. We found that time lag of the chromospheric signal relative to photospheric one varies from -12 to 100 seconds and is about 50 seconds on average.We assume that the small observed lag can have three possible explanations: i) convergence of formation levels of He i 10830 A and Si i 10827 A in faculae; ii) significant increase of five-minute oscillation propagation velocity above faculae; iii) simultaneous presence of standing and travelling waves.

12 pages, 6 figures, accepted in Solar Physics

References in corpus (2)

• Channeling 5-min photospheric oscillations into the solar outer atmosphere through small-scale vertical magnetic flux tubes
• Features of spatial distribution of oscillations in faculae regions

Cited by in corpus (5)

• Multiwavelength studies of MHD waves in the solar chromosphere: An overview of recent results
• The Source of Three-minute Magneto-acoustic Oscillations in Coronal Fans
• Properties of local oscillations in the lower sunspot atmosphere
• Oscillations accompanying a He I 10830 Å negative flare in a solar facula
• Using Flare-Induced Modulation of Three- and Five-Minute Oscillations for Studying Wave Propagation in the Solar Atmosphere