What is the dynamic method?

The dynamic method is the approach used in astrophysics to try to find out what the asteroid weight is, depending on how its space is affected by the gravitational thrust of another asteroid that passes close. The process is also referred to as failure theory and has led to determination of estimates for masses of 24 prominent asteroids. The use of a dynamic method to determine the asteroid mass is the most successful method with the exception of direct flying spacecraft since 2011, but is susceptible to problems due to two significant restrictions. Because asteroids are usually extremely small bodies, gravitational effects that have each other from a distance are often so small that they cannot be measured by contemporary technology. Secondly, the dynamic method only works with two isolated bodies in space coming closely, because the problem with the N-floors arises with the complex effects of the heavenly mechanics, if other asteroids or planets are simultaneously affected by the movement of both bodies directly studied.

The narrow group of conditions in astronomy must be present in order to determine the mass of asteroids using a dynamic method where the contribution to an error is not more than 10% of the actual matter of the object. These conditions include factors such as a measured asteroid with repeated, one per meeting with another asteroid to make more measurement, and compare with the past asteroid movement for many years. Determination of the mass of the first 19 asteroids using the dynamic method since 2003 has relied on historical records for orbit of objects from 1900 to 2002 to ensure the best possible accuracy in the calculations.

Since 2011, the mass of 24 asteroids has been determined in the solar system of the field of heavenly mechanics in astronomy for 200 years. Most of these Objects are relatively large according to asteroid standards, such as Asteroid Ceres, which in itself represents 30% to 40% of the whole mass of the asteroid belt itself. However, Ceres is only 1% of the mass of the earthMoon, which made it a difficult task to determine its mass. Some asteroids have their own natural satellites such as 1998 WW 31 and 2001 Qt _{297 , allowing more frequent calculations of gravitational disorders. Asteroids were also visited by a spacecraft such as 433 EROS and 253 Mathilde, which visited the Asteroid Rendezvous-Shoemaker (near Shoemaker) in 2000, and their gravitational effect on the craft was used to determine their mass.}

other large asteroids that have been determined by their masses designed by the dynamic method include 2 Pallas and 4 vest, which also included disorders caused by Mars when they went through the gravitational field in 2001. The vest also had a spacecraft observation as a part of its mass calculations. Asteroids, such as 45 Eugenia, 87 Sylvia and 90 anti -ope, have calculated dynamic methods of their weight based solely on their own satellite orbit.