The Imaging Vector Magnetograph at Haleakalā IV: Stokes Polarization Spectra in the Sodium D1 589.6 nm Spectral Line

Details The Imaging Vector Magnetograph at Haleakalā IV: Stokes Polarization Spectra in the Sodium D1 589.6 nm Spectral Line The Imaging Vector Magnetograph at Haleakalā IV: Stokes Polarization Spectra in the Sodium D1 589.6 nm Spectral Line

Mar 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012soph..tmp...57l&link_type=abstract

Solar Physics, Online First

Physics

Sun: Chromosphere, Observations, Polarimetry, Data Analysis

Scientific paper

The Imaging Vector Magnetograph (IVM) at the Mees Solar Observatory, Haleakalā, Maui, Hawai'i, obtained many years of vector magnetic-field data in the photospheric Fe uc(i) 630.25 nm line. In the latter period of its operation, the IVM was modified to allow routine observations in the chromospheric Na uc(i) D1 line, as well as the Fe uc(i) line. We describe the sodium observational data in detail, including the data-reduction steps that differ from those employed for the Fe uc(i) 630.25 nm line, to obtain calibrated Stokes polarization spectra. We have performed a systematic comparison between the observational data and synthetic NLTE Na uc(i) D1 Stokes spectra derived for a variety of solar-appropriate atmospheric and magnetic configurations. While the Na uc(i) D1 Stokes polarization signals from the solar atmosphere are expected to be weak, they should generally be within the IVM capability. A comparison between synthetic spectra and observational data indicates that this is indeed the case.

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