The Cosmic Microwave Background and the Light Elements
A hot dense start predicts both a cooled thermal glow filling the sky and fixed proportions of hydrogen, helium and lithium, and both are measured. Together they are the strongest evidence for the Big Bang.
What a learner can do afterwards
- Explains why the background radiation has a blackbody spectrum and why it is so cold now
- Relates the predicted helium fraction to conditions in the first minutes
- Says what the small temperature ripples in the background correspond to
1 · Read
The whole sky glows faintly in microwaves at just 2.7 degrees above absolute zero. This is the cooled afterlight of the hot early universe, released when atoms first formed about 380,000 years after the start. Expansion has stretched that original orange glare a thousandfold into microwaves.
Its spectrum is the most perfect blackbody ever measured, exactly what a hot dense origin predicts. No scattered starlight could fake both the spectrum and the uniformity. The glow is the strongest witness for the hot start.
In the first minutes the universe was a nuclear furnace, fusing protons and neutrons into helium before cooling stopped the reactions. About a quarter of ordinary mass ended up as helium. That fixed fraction is a firm prediction only a hot dense start can make.
Look at the tiny ripples, one part in a hundred thousand, marking the glow. Those faint patches are the seeds that gravity later grew into galaxies. Smooth overall, slightly lumpy in detail: that is the signature to remember.
A cold perfect glow plus a fixed helium share point to a hot dense start with lumpy seeds.
2 · Watch
Take it off screen
Where it sits
8 questions wait behind this lesson, each with its answer explained. Every answer feeds the sky: stars light as they are learned, and dim when it is time to come back.