Coronal Electron Densities derived with Images acquired during the 21 August 2017 Total Solar Eclipse. (arXiv:2010.15005v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Bemporad_A/0/1/0/all/0/1">Alessandro Bemporad</a>
The total solar eclipse of August 21st, 2017 was observed with a Digital
Single Lens Reflex (DSLR) camera equipped with a linear polarizing filter. A
method was developed to combine images acquired with 15 different exposure
times (from 1/4000 sec to 4 sec), identifying in each pixel the best interval
of detector linearity. The resulting mosaic image of the solar corona extends
up to more than 5 solar radii, with a projected pixel size by 3.7 arcsec/pixel,
and an effective image resolution by 10.2 arcsecs, as determined with visible
$alpha-$Leo and $nu-$Leo stars. Image analysis shows that in the inner corona
the intensity gradients are so steep, that nearby pixels shows a relative
intensity difference by up to $sim 10 %$; this implies that careful must be
taken when analyzing single exposures acquired with polarization cameras.
Images acquired with two different orientations of the polarizer have been
analyzed to derive the degree of linear polarization, and the polarized
brightness $pB$ in the solar corona. After inter-calibration with $pB$
measurements by the K-Cor instrument on Mauna Loa Solar Observatory (MLSO),
data analysis provided the 2D coronal electron density distribution from 1.1 up
to $sim 3$ solar radii. The absolute radiometric calibration was also
performed, with the full sun image, and with magnitudes of visible stars. The
resulting absolute calibrations show a disagreement by a factor $sim 2$ with
respect to MLSO; interestingly, this is the same disagreement recently found
with eclipse predictions provided by MHD numerical simulations.
The total solar eclipse of August 21st, 2017 was observed with a Digital
Single Lens Reflex (DSLR) camera equipped with a linear polarizing filter. A
method was developed to combine images acquired with 15 different exposure
times (from 1/4000 sec to 4 sec), identifying in each pixel the best interval
of detector linearity. The resulting mosaic image of the solar corona extends
up to more than 5 solar radii, with a projected pixel size by 3.7 arcsec/pixel,
and an effective image resolution by 10.2 arcsecs, as determined with visible
$alpha-$Leo and $nu-$Leo stars. Image analysis shows that in the inner corona
the intensity gradients are so steep, that nearby pixels shows a relative
intensity difference by up to $sim 10 %$; this implies that careful must be
taken when analyzing single exposures acquired with polarization cameras.
Images acquired with two different orientations of the polarizer have been
analyzed to derive the degree of linear polarization, and the polarized
brightness $pB$ in the solar corona. After inter-calibration with $pB$
measurements by the K-Cor instrument on Mauna Loa Solar Observatory (MLSO),
data analysis provided the 2D coronal electron density distribution from 1.1 up
to $sim 3$ solar radii. The absolute radiometric calibration was also
performed, with the full sun image, and with magnitudes of visible stars. The
resulting absolute calibrations show a disagreement by a factor $sim 2$ with
respect to MLSO; interestingly, this is the same disagreement recently found
with eclipse predictions provided by MHD numerical simulations.
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