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One puzzling question in solar physics is the difference between elementalabundances in the photosphere and the corona. Elements with low firstionization potential (FIP) can be overabundant in the corona compared to thephotosphere under certain circumstances. The same phenomenon has been observedon a handful of stars, while a few of them show the inverse effect. But not allthe stars in the original sample had precise photospheric abundances derivedfrom optical spectra, so for some the solar values were adopted. In this workwe make homogeneous abundance measurements from optical spectroscopy.  We collected spectra of 16 stars showing the FIP effect with the 1-m RCCtelescope of Konkoly Observatory, with resolution of $\lambda / \Delta \lambda\sim 21\,000$. We determine the fundamental astrophysical parameters($T_\mathrm{eff}$, $\log g$, $[M/H]$, $\xi_\mathrm{mic}$, $v \sin i$) andindividual elemental abundances with the SME spectral synthesis code usingMARCS2012 model atmosphere and spectral line parameters from the Vienna AtomicLine Database (VALD).

Deriving photospheric parameters and elemental abundances for a sample of stars showing the FIP effect