Deriving photospheric parameters and elemental abundances for a sample of stars showing the FIP effect. (arXiv:1904.13103v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Seli_B/0/1/0/all/0/1">Bálint Seli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kriskovics_L/0/1/0/all/0/1">Levente Kriskovics</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vida_K/0/1/0/all/0/1">Krisztián Vida</a>
One puzzling question in solar physics is the difference between elemental
abundances in the photosphere and the corona. Elements with low first
ionization potential (FIP) can be overabundant in the corona compared to the
photosphere under certain circumstances. The same phenomenon has been observed
on a handful of stars, while a few of them show the inverse effect. But not all
the stars in the original sample had precise photospheric abundances derived
from optical spectra, so for some the solar values were adopted. In this work
we make homogeneous abundance measurements from optical spectroscopy.
We collected spectra of 16 stars showing the FIP effect with the 1-m RCC
telescope of Konkoly Observatory, with resolution of $lambda / Delta lambda
sim 21,000$. We determine the fundamental astrophysical parameters
($T_mathrm{eff}$, $log g$, $[M/H]$, $xi_mathrm{mic}$, $v sin i$) and
individual elemental abundances with the SME spectral synthesis code using
MARCS2012 model atmosphere and spectral line parameters from the Vienna Atomic
Line Database (VALD).
One puzzling question in solar physics is the difference between elemental
abundances in the photosphere and the corona. Elements with low first
ionization potential (FIP) can be overabundant in the corona compared to the
photosphere under certain circumstances. The same phenomenon has been observed
on a handful of stars, while a few of them show the inverse effect. But not all
the stars in the original sample had precise photospheric abundances derived
from optical spectra, so for some the solar values were adopted. In this work
we make homogeneous abundance measurements from optical spectroscopy.
We collected spectra of 16 stars showing the FIP effect with the 1-m RCC
telescope of Konkoly Observatory, with resolution of $lambda / Delta lambda
sim 21,000$. We determine the fundamental astrophysical parameters
($T_mathrm{eff}$, $log g$, $[M/H]$, $xi_mathrm{mic}$, $v sin i$) and
individual elemental abundances with the SME spectral synthesis code using
MARCS2012 model atmosphere and spectral line parameters from the Vienna Atomic
Line Database (VALD).
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