Elementary introduction to the physics of Newtonian gravity
From Micasim
According to Newton's Law of Universal Gravitation - stated in Proposition VII, Book III, of his Philosophiae Naturalis Principia Mathematica, 1687 - two point-like bodies attract each other with a force whose strength is given by the formula
where m1 and m2 are the masses of the bodies and r is the distance between them.
In stellar dynamics, star sizes are in most cases much less than their mutual distances and thus it is justified to consider them as point-like bodies. Newton proved also that the same formula applies to spherical bodies, provided r is the distance between their centers - Proposition VIII, Book III.
G is a proportionality constant, whose value in the International System of units ( SI ) is about
.
Often the International System is not the most convenient choice for stellar dynamics.
In astronomy it is more convenient to measure distances in parsecs ( pc ), masses in units of one solar mass (
kg ), and speeds in kilometers per second ( km/s ).
Then the time unit is 0.9778 My and the gravitational constant is given as
.
Another system of units ( sometimes named N-body units ) is used in numerical calculations, that is what we are mostly interested in.
Masses are given in units of M, the total mass of the physical system under consideration ; G is taken to be one, and length units are adapted so that E, the total energy of the ( supposedly bound ) system, is -1/4.
In this system then the length unit ( called virial radius ) is
; the mass unit is M ; the time unit is
; and the speed unit is
.

