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Probing the Temperature Structure of the Solar Chromosphere with ALMA by C. Alissandrakis et al.*

1 Aug 2017, 11:06 UTC
Probing the Temperature Structure of the Solar Chromosphere with ALMA  by C. Alissandrakis et al.*
(200 words excerpt, click title or image to see full post)

Determining the detailed temperature structure of the solar atmosphere from observations is a basic means of constructing and testing atmospheric models. One avenue to address this problem is based on measuring the center-to-limb variation of the intensity in various spectral regions. Observations in the radio domain are particularly suited for such a task since they don’t suffer from a set of complications (e.g., departures from the ionization and local thermodynamic equilibrium, elemental abundances) which may be relevant to the diagnostics in other wavelength domains. Another convenient aspect is that the quiet Sun radio emission is due to the free-free process (e.g., Shibasaki et al. 2011; Wedemeyer et al. 2016). We have recently performed such a study (Alissandrakis et al. 2017), using the Atacama Large Millimeter/submillimeter Array (ALMA).
Observations and Analysis
We analyzed ALMA observations at 100 and 239 GHz taken from the 16-20th of December 2015, a period of solar commissioning activities. Full disk (FD) images were constructed by scanning the solar disk with twenty 12-m antennas, using the compact configuration of ALMA. The full width at half maximum of the single dish beam is ~27” and 60” at 239 GHz and 100 GHz, respectively. The pipeline of solar ...

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