Astrophysics Unit 13

1.1.1 The source of the Suns energy is nuclear fusion in the interior of the star. Inside the Sun, nuclei of hydrogen fuse together to form helium, releasing energy in the process. Beucase high pressures, the nuclei are suffciciently close to each other for collisions to occur. Owing to temperatures in excess of 10^8 K, the electrostatic repulsion hydrogen nuclei can be overcome and fuse together.

1.1.2 As Kinetic energy of the particles inside the Sun increase, the radiation pressure increases. Radiation pressure is the force exerted by solar radiation on the surroundings. It acts to stabilize the Sun against gravitational collapse, creating a kind of equilibrium.

1.2.1 The luminosity of a star is defined as the energy emitted per unit time.

1.2.2 b= L/(4πd^2 )

1.2.3 Apparent brightness of a star is defined as the power incident on Earth perpendicular to unit area. To measure apparent brightness, the light reaching the Earth is collected with a telescope and detected using a charge-coupled device (CCD). The data is processed by a computer and the apparent brightness can then be worked out accurately.

1.3.1 Max. Wavelength = 2.9 x 10^-3 / T

1.3.2 If the energy emitted from a star is analyzed over a range of wavelengths and the peak wavelength is determined, then the surface temp. of the star can be determined.

1.4.1