  We present chemical composition and fundamental parameters (the effective
temperature, surface gravity and radius) for four sharp-lined A-type stars
${\gamma}$ Gem (HD 41705), o Peg (HD 214994), ${\theta}$ Vir (HD 114330) and
${\nu}$ Cap (HD 193432). Our analysis is based on a self-consistent model
fitting of high-resolution spectra and spectrophotometric observations over a
wide wavelength range. We refined the fundamental parameters of the stars with
the SME package and verified their accuracy by comparing with the spectral
energy distribution and hydrogen line profiles. We found Teff/log g =
9190+/-130 K/3.56+/-0.08, 9600+/-50 K/3.81+/-0.04, 9600+/-140 K/3.61+/-0.12,
and 10200+/-220 K/3.88+/-0.08 for ${\gamma}$ Gem, o Peg, ${\theta}$ Vir and
${\nu}$ Cap, respectively. Our detailed abundance analysis employs a hybrid
technique for spectrum synthesis based on classical model atmospheres
calculated in local thermodynamic equilibrium (LTE) assumption together with
the non-LTE (NLTE) line formation for 18 of 26 investigated species. Comparison
of the abundance patterns observed in A stars of different types (normal A, Am,
Ap) with similar fundamental parameters reveals significant abundance diversity
that cannot be explained by the current mechanisms of abundance peculiarity
formation in stellar atmospheres. We found a rise of the heavy element (Zn, Sr,
Y, Zr, Ba) abundance excess up to +1 dex with Teff increasing from 7200 to
10000 K, with a further decrease down to solar value at Teff = 13000 K,
indicating that stars with solar element abundances can be found among late
B-type stars.
