Introduction to Astrophysics/Laws and Formulae

From Wikibooks, open books for an open world
Jump to navigation Jump to search

Gravitation[edit | edit source]

Kepler's Laws[edit | edit source]

  1. The orbit of each planet is an ellipse which has the sun at one of its foci.
  2. Each planet moves in such a way that the line joining it to the sun sweeps out equal areas in equal times.
  3. The squares of the periods of revolution of the planets about the Sun are proportional to the cubes of their mean distance from it.

Newton's gravitational law[edit | edit source]

F = The gravitational force between two bodies.
G = Universal gravity constant, 6.67 x 10−11 N m2 kg−2
m1 = The mass of the first body.
m2 = The mass of the second body.
r = The distance between the centres of mass of two bodies.

Black body radiation[edit | edit source]

Wein’s displacement law(only for black bodies)

λmax = W/T

Wein’s constant(W)= 2.90 × 10−3 m K

T= temperature of the black body

Stefan's Law[edit | edit source]

E = Rate of energy radiated from the surface of a black body per unit area.
σ = Stefan's constant, 5.67 × 10−8 W m−2 K−4
T = Surface temperature of the black body.

Stellar Magnitude[edit | edit source]

Apparent Magnitude[edit | edit source]

m = Apparent magnitude of star.
I = Intensity of light received.
K = a constant

Pogson's Formula[edit | edit source]

m1 = Apparent magnitude of first star.
m2 = Apparent magnitude of second star.
I1 = Intensity of light received from first star.
I2 = Intensity of light received from second star.

Absolute Magnitude[edit | edit source]

m = Apparent magnitude of star.
M = Absolute magnitude of star.
d = Distance to star in parsecs.