Association of calcium network bright points with underneath photospheric magnetic patches. (arXiv:1902.03764v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Narang_N/0/1/0/all/0/1">Nancy Narang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banerjee_D/0/1/0/all/0/1">Dipankar Banerjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chandrashekhar_K/0/1/0/all/0/1">Kalugodu Chandrashekhar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pant_V/0/1/0/all/0/1">Vaibhav Pant</a>
Recent dedicated Hinode polar region campaigns revealed the presence of
concentrated kilogauss patches of magnetic field in the polar regions of the
Sun which are also shown to be correlated with facular bright points at the
photospheric level. In this work, we demonstrate that this spatial
intermittency of the magnetic field persists even up to the chromospheric
heights. The small-scale bright elements visible in the bright network lanes of
solar network structure as seen in the Ca ii H images are termed as network
bright points. We use special Hinode campaigns devoted to observe polar regions
of the Sun to study the polar network bright points during the phase of last
extended solar minimum. We use Ca ii H images of chromosphere observed by Solar
Optical Telescope (SOT). For magnetic field information, level 2 data of
spectro-polarimeter (SP) is used. We observe a considerable association between
the polar network bright points and magnetic field concentrations. The
intensity of such bright points is found to be correlated well with the
photospheric magnetic field strength underneath with a linear relation existing
between them.
Recent dedicated Hinode polar region campaigns revealed the presence of
concentrated kilogauss patches of magnetic field in the polar regions of the
Sun which are also shown to be correlated with facular bright points at the
photospheric level. In this work, we demonstrate that this spatial
intermittency of the magnetic field persists even up to the chromospheric
heights. The small-scale bright elements visible in the bright network lanes of
solar network structure as seen in the Ca ii H images are termed as network
bright points. We use special Hinode campaigns devoted to observe polar regions
of the Sun to study the polar network bright points during the phase of last
extended solar minimum. We use Ca ii H images of chromosphere observed by Solar
Optical Telescope (SOT). For magnetic field information, level 2 data of
spectro-polarimeter (SP) is used. We observe a considerable association between
the polar network bright points and magnetic field concentrations. The
intensity of such bright points is found to be correlated well with the
photospheric magnetic field strength underneath with a linear relation existing
between them.
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