The fine structure of a chromospheric rosette

Details The fine structure of a chromospheric rosette The fine structure of a chromospheric rosette

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...271..574t&link_type=abstract

Astronomy and Astrophysics, Vol. 271, p. 574 (1993)

Astronomy and Astrophysics

Astrophysics

27

Lines: Profile, Sun: Chromosphere

Scientific paper

We have studied the spatial behaviour of the physical properties of dark mottles forming a well-defined rosette. The observations were obtained with the Multichannel Subtractive Double Pass (MSDP) spectrograph, operating in Hα at the Pic du Midi Observatory. From these observations, intensity fluctuations and Doppler shift velocities at different wavelengths were derived over a two dimensional field of view. The observed contrast profiles were matched with theoretical contrast profiles using Beckers' cloud model and 4 parameters were derived for the dark mottles: the source function, the line-of-sight velocity, the Doppler width and the optical depth. From these parameters a range for the temperature and electron density can be derived using Vernazza's et al. (1981) model D. We detected strong downflows at the roots of the mottles, while their upper part is ascending with velocities sometimes greater than 10 km s-1. The values of the cloud parameters are consistent with values given by other authors for this kind of features. Consistency was also found between cloud parameters and the values given for spicules, leading to the conclusion for the identity of these structures.

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