English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Conference Paper

Flows along arch filaments observed in the GRIS ‘very fast spectroscopic mode’

MPS-Authors

Hoch,  S.
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons104044

Lagg,  Andreas
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

/persons/resource/persons104218

Solanki,  Sami K.
Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society;

External Resource
No external resources are shared
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

González Manrique, S. J., Denker, C., Kuckein, C., Pastor Yabar, A., Collados, M., Verma, M., et al. (2017). Flows along arch filaments observed in the GRIS ‘very fast spectroscopic mode’. In Proceedings of the International Astronomical Union: Fine Structure and Dynamics of the Solar Atmosphere; Symposium S327 (pp. 28-33).


Cite as: http://hdl.handle.net/21.11116/0000-0003-A2F4-2
Abstract
A new generation of solar instruments provides improved spectral, spatial, and temporal resolution, thus facilitating a better understanding of dynamic processes on the Sun. High-resolution observations often reveal multiple-component spectral line profiles, e.g., in the near-infrared He i 10830 Å triplet, which provides information about the chromospheric velocity and magnetic fine structure. We observed an emerging flux region, including two small pores and an arch filament system, on 2015 April 17 with the ‘very fast spectroscopic mode’ of the GREGOR Infrared Spectrograph (GRIS) situated at the 1.5-meter GREGOR solar telescope at Observatorio del Teide, Tenerife, Spain. We discuss this method of obtaining fast (one per minute) spectral scans of the solar surface and its potential to follow dynamic processes on the Sun. We demonstrate the performance of the ‘very fast spectroscopic mode’ by tracking chromospheric high-velocity features in the arch filament system.