Further calculations are based on the third Kepler law, according to which (T1 / T2) ^ 2 * (M1 + Mc) / (M2 + Mc) = (L1 / L2) ^ 3, where T is the period of revolution of the celestial body around Of the Sun, L is the distance to the last, M1, M2 and Mc-masses of two celestial bodies and stars, respectively.
Further calculations are based on the third Kepler law, according to which (T1 / T2) ^ 2 * (M1 + Mc) / (M2 + Mc) = (L1 / L2) ^ 3, where T is the period of revolution of the celestial body around Of the Sun, L is the distance to the last, M1, M2 and Mc-masses of two celestial bodies and stars, respectively.
user
Подальші обчислення спираються на 3-ій закон Кепплера, згідно з яким (T1 / T2) ^ 2 * (M1 + Mc) / (M2 + Mc) = (L1 / L2) ^ 3, де T - період обертання небесного тіла навколо сонця, L - відстань до останнього, M1, M2 і Mc -маси двох небесних тіл і зірки, відповідно.
assistant