## GravitationEdit

### Kepler's LawsEdit

- The orbit of each planet is an ellipse which has the sun at one of its foci.
- Each planet moves in such a way that the line joining it to the sun sweeps out equal areas in equal times.
- 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 lawEdit

*F* = |
The gravitational force between two bodies. |

*G* = |
Universal gravity constant, 6.67 x 10^{−11} N m^{2} kg^{−2} |

*m*_{1} = |
The mass of the first body. |

*m*_{2} = |
The mass of the second body. |

*r* = |
The distance between the centres of mass of two bodies. |

## Black body radiationEdit

temperature of the black body.

*w* = 2.90 × 10^{−3} m K

### Stefan's LawEdit

*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 MagnitudeEdit

### Apparent MagnitudeEdit

*m* = |
Apparent magnitude of star. |

*I* = |
Intensity of light received. |

*K* = |
a constant |

### Pogson's FormulaEdit

*m*_{1} = |
Apparent magnitude of first star. |

*m*_{2} = |
Apparent magnitude of second star. |

*I*_{1} = |
Intensity of light received from first star. |

*I*_{2} = |
Intensity of light received from second star. |

### Absolute MagnitudeEdit

*m* = |
Apparent magnitude of star. |

*M* = |
Absolute magnitude of star. |

*d* = |
Distance to star in parsecs. |