Dynamics of the Fe II 396.94 nm emission line observed at solar disk center

Abstract

Aims. We have studied the structure and dynamics of the upper photosphere and lower chromosphere of the quiet Sun. Methods. We analyzed a sequence of scans of slit spectra of the Ca II H line at 396.8 nm, with a spectral resolution of 850 000, and a spatial resolution of about one arcsec, taken in the quiet Sun at disk center, with a duration of about 55 min and an area coverage of 185 × 3.5 . We used statistical methods to characterize size, lifetime, and dynamics of emission features of the Fe II line at 396.94 nm. Results. We have identified about 780 distinct features where the Fe II line shows emission stronger than 3% above the local continuum. Their lifetime is on the order of one minute, and the spatial extent is about or less than 2 . On average, Fe II emission features show a significant redshift of 1.3 km s −1 , with respect to the position of the absorption line. The redshift of the Fe II emission is absent close to the solar limb. The Fe II emission is coupled with a strongly enhanced intensity level of the Ca II wings. A time line analysis shows that other photospheric lines show significant redshift one minute before, and a blueshift after, the occurrence of an emission event. A redshift of the Ca II H line core precedes the redshift of the Fe II line by about 30 s. The occurrence of the H2v emissions is strongly reduced before and significantly increased after the Fe II emission events. Conclusions. The temporal behavior of the Fe II emission line and both the Ca II H line core and H2v emission suggest a connection between Fe II emission and chromospheric activity. The presence of a significant redshift during the Fe II emissions and the absence of this redshift near the limb suggest that the observed redshift is indeed caused by a downflow in the line-forming region. From our result concerning the intensity fluctuations in the core of the Fe II line, and from the magnitude of the downflow velocities we conclude that the Fe II emissions at 396.94 nm occur in the photosphere.

Spectroscopy at the Solar Limb: II. Are Spicules Heated to Coronal Temperatures?

“…The spectral line seen in emission between Ca ii H and Hǫ up to a height of nearly 2 Mm should pertain to singly ionized iron (cf. Engvold and Halvorsen 1973;Lites 1974;Rutten and Stencel 1980;Watanabe and Steenbock 1986;Schmidt and Fisher 2013). Figure 13 shows the FWHM of the laterally averaged profiles for He i at 1083 nm, Ca ii H and Hǫ.…”

Chromospheric impact of an exploding solar granule

“…According to Pereira et al (2015) this is a sign of heated material in the low chromosphere with cooler material above; a rare quiet Sun event (1% of pixels) also observed in simulations (see also Carlsson et al 2015). Schmidt & Fisher (2013) Panel (e) in Fig. 2 shows the Mg ii k spectra in time for the slit position marked with a red solid line in the previous panels.…”

“…According to Pereira et al (2015) this is a sign of heated material in the low chromosphere with cooler material above; a rare quiet Sun event (1% of pixels) also observed in simulations (see also Carlsson et al 2015). Schmidt & Fisher (2013) have observed similarly rare emission in the Fe i 3969 Å line out of phase with the simultaneously observed Ca ii H2v intensity as a marker of chromospheric dynamics. Panel (e) in Fig.…”