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The second flight of the SUNRISE balloon-borne solar observatory: overview of instrument updates, the flight, the data and first results | | S. K. Solanki
; T. L. Riethmüller
; P. Barthol
; S. Danilovic
; W. Deutsch
; H. P. Doerr
; A. Feller
; A. Gandorfer
; D. Germerott
; L. Gizon
; B. Grauf
; K. Heerlein
; J. Hirzberger
; M. Kolleck
; A. Lagg
; R. Meller
; G. Tomasch
; M. van Noort
; J. Blanco Rodríguez
; J. L. Gasent Blesa
; M. Balaguer Jiménez
; J. C. Del Toro Iniesta
; A. C. López Jiménez
; D. Orozco Suárez
; T. Berkefeld
; C. Halbgewachs
; W. Schmidt
; A. Álvarez-Herrero
; L. Sabau-Graziati
; I. Pérez Grande
; V. Martínez Pillet
; G. Card
; R. Centeno
; M. Knölker
; A. Lecinski
; | | Date: |
6 Jan 2017 | | Abstract: | The SUNRISE balloon-borne solar observatory, consisting of a 1~m aperture
telescope that provided a stabilized image to a UV filter imager and an imaging
vector polarimeter, carried out its second science flight in June 2013. It
provided observations of parts of active regions at high spatial resolution,
including the first high-resolution images in the Mg~{sc ii}~k line. The
obtained data are of very high quality, with the best UV images reaching the
diffraction limit of the telescope at 3000~AA after Multi-Frame Blind
Deconvolution reconstruction accounting for phase-diversity information. Here a
brief update is given of the instruments and the data reduction techniques,
which includes an inversion of the polarimetric data. Mainly those aspects that
evolved compared with the first flight are described. A tabular overview of the
observations is given. In addition, an example time series of a part of the
emerging active region NOAA AR~11768 observed relatively close to disk centre
is described and discussed in some detail. The observations cover the pores in
the trailing polarity of the active region, as well as the polarity inversion
line where flux emergence was ongoing and a small flare-like brightening
occurred in the course of the time series. The pores are found to contain
magnetic field strengths ranging up to 2500~G and, while large pores are
clearly darker and cooler than the quiet Sun in all layers of the photosphere,
the temperature and brightness of small pores approach or even exceed those of
the quiet Sun in the upper photosphere. | | Source: | arXiv, 1701.1555 | | Services: | Forum | Review | PDF | Favorites | |
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