We need to estimate the temperature at recombination from the figure below. (Estimate a temperature to the nearest 500 K.) Matter dominates Temperature (K) λ = 1010 109 108 107 10⁰ 10° 104 10³ 100 10 1 Formation of helium 1s H !K 1 min Radiation dominates X Electron-positron annihilation 1 hour 1 day 1 yr 100 yr 104 yr Time since Big Bang Energy density equals Recombination Re-ionization (first stars and galaxies) Dark age 10 yr 108 yr ℗ Then use that temperature in Wien's Law to determine the wavelength in nanometers. Round to one significant figure. 2.9 x 106 Now A = 407 x Use Wien's law and the temperature you estimated to calculate the wavelength. nm. 1010 yr
Stellar evolution
We may see thousands of stars in the dark sky. Our universe consists of billions of stars. Stars may appear tiny to us but they are huge balls of gasses. Sun is a star of average size. Some stars are even a thousand times larger than the sun. The stars do not exist forever they have a certain lifetime. The life span of the sun is about 10 billion years. The star undergoes various changes during its lifetime, this process is called stellar evolution. The structure of the sun-like star is shown below.
Red Shift
It is an astronomical phenomenon. In this phenomenon, increase in wavelength with corresponding decrease in photon energy and frequency of radiation of light. It is the displacement of spectrum of any kind of astronomical object to the longer wavelengths (red) side.
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