We describe our procedure to determine effective temperatures , rotational velocities , microturbulent velocities , and chemical abundances in the atmospheres of Sun-like stars . We use independent determinations of iron abundances using the fits to the observed Fe I and Fe II atomic absorption lines . We choose the best solution from the fits to these spectral features for the model atmosphere that provides the best confidence in the determined log N ( Fe ) , V _ { t } , and v sin i .Computations were done in the framework of LTE . Blending effects were accounted for explicitly . First , we compute the abundance of iron for a set of adopted microturbulent velocities . In some cases , a few points of log N ( Fe I ) = log N ( Fe II ) can be found . To determine the most self-consistent effective temperature and microturbulent velocity in any star ’ s atmosphere , we used an additional constraint where we minimise the dependence of the derived abundances of Fe I and Fe II on the excitation potential of the corresponding lines . Using this procedure we analyse the spectra of the Sun and two well known solar type stars , HD1835 and HD10700 to determine their abundances , microturbulent velocity and rotational velocity . Our approach allows us to determine self-consistent values for the effective temperatures , abundances , V _ { t } and v sin i . For the Sun we obtain the best agreement for a model atmosphere of T _ { eff } /log g/ [ Fe/H ] = 5777/4.44/0.0 , iron abundances and microturbulent velocities of log N ( Fe ) =4.44 , V _ { t } = 0.75 km/s , for the Fe I lines , and log N ( Fe ) = -4.47 , V _ { t } = 1.5 km/s for the Fe II lines . Furthermore , abundances of other elements obtained from the fits of their absorption features agree well enough ( \pm 0.1 dex ) with the known values for the Sun . We determined a rotational velocity of v sin i = 1.6 \pm 0.3 km/s for the spectrum of the Sun as a star . For HD1835 the self-consistent solution for Fe I and Fe II lines log N ( Fe ) =+0.2 was obtained with a model atmosphere of 5807/4.47/+0.2 and microturbulent velocity V _ { t } = 0.75 km/s , and leads to v sin i = 7.2 \pm 0.5 km/s . For HD10700 the self-consistent solution log N ( Fe ) = -4.93 was obtained using a model atmosphere of 5383/4.59/-0.6 and microturbulent velocity V _ { t } = 0.5 km/s . The Fe I and Fe II lines give rise to a v sin i = 2.4 \pm 0.4 km/s . Using the T _ { eff } found from the ionisation equilibrium parameters for all three stars , we found abundances of a number of other elements : Ti , Ni , Ca , Si , Cr . We show that uncertainties in the adopted values of T _ { eff } of 100 K and V _ { t } of 0.5 km/s change the abundances of elements up to 0.1 and 0.2 dex respectively . Galactic abundances variations can generally be larger than this measurement precision and therefore we can study abundance variations throughout the Galaxy .