Abstract
Our objective is to construct models of the velocity ellipsoid and the retrieved Solar motion for program stars with 4924 points within the Solar neighborhood (∼2 kpc). In which 1374 early types (B5, A0, A5, F0, and F5) and about 3550 late types (G0, G5, K0, and K5) with more recent data source with Gaia DR3. Based on space velocity vectors \((\bar {U},\bar {V},\bar {W};\;{\text{km }}{{{\text{s}}}^{{ - 1}}})\) , we have determined a velocity ellipsoid parameter for our program stars. We have derived the Solar velocity \(({{S}_{ \odot }})\) , which ranged from 13.39 ± 3.66 to 25.06 ± 5.06 km s–1, and other Solar elements \(({\text{i}}.{\text{e}}.,\;{{l}_{{\text{A}}}},\;{{b}_{{\text{A}}}},\;{{{{\alpha }}}_{{\text{A}}}},\;{{{{\delta }}}_{{\text{A}}}})\) , the velocity dispersion \(\left( \sigma \right)\) , ranging from 26.65 ± 5.16 to 57.29 ± 7.57 km s–1 for considered program stars, the projected distances \(({{X}_{ \odot }},{{Y}_{ \odot }},{{Z}_{ \odot }};\;{\text{kpc}})\) , ratio of \(\left( {{{\sigma }_{2}}{\text{/}}{{\sigma }_{1}}} \right)\) , ranging from 0.52 to 0.92, which relates to Oort’s constants \((A,B;\;{\text{km}}\;{{{\text{s}}}^{{ - 1}}}{\text{ kp}}{{{\text{c}}}^{{ - 1}}}),\) and finally the ratio of \(({{\sigma }_{3}}{\text{/}}{{\sigma }_{1}})\) , ranging from 0.41 to 0.61.
