Helium
Helium is the second-lightest and second most abundant element in the universe, yet on Earth it's scarce — a colorless, odorless noble gas so chemically inert it forms essentially no compounds. It was actually spotted in the Sun's spectrum before anyone found it on Earth, a rare case of an element being discovered somewhere other than our own planet.
- Group · Period
- 18 · 1
- At room temp
- gas
- Melts at
- 0.95 K
- Density
- 0.0001785 g/cm³
- Discovered
- 1868
Uses
Liquid helium’s defining use is as a coolant for superconducting magnets, most notably in MRI scanners, where it chills the magnet coils to temperatures cold enough for superconductivity to work. That same extreme-cold capability makes it valuable in scientific research, including particle accelerators and low-temperature physics experiments. Because it’s inert and won’t react with molten or reactive metals, helium is also used as a protective shielding gas in some types of welding.
Its low density and non-flammability make it the standard gas for balloons and airships, and deep-sea divers sometimes breathe a helium-oxygen mixture called heliox, which reduces the risk of nitrogen-related problems at depth compared to ordinary compressed air.
History
Helium was first detected in 1868, not in a laboratory but in the Sun. During a solar eclipse, French astronomer Pierre Janssen observed a bright yellow line in the Sun’s spectrum that didn’t match any known element, and English astronomer Norman Lockyer, studying the same spectral feature separately, proposed it belonged to a new element and named it helium, after Helios, the Greek sun god. It wasn’t confirmed on Earth until 1895, when Scottish chemist William Ramsay isolated it from a uranium-bearing mineral, showing that this “solar” element existed here all along.
Fun facts
- Helium has the lowest boiling point of any element, staying liquid down to about −269°C, just a few degrees above absolute zero.
- Unlike almost every other substance, helium doesn't freeze into a solid at normal pressure no matter how cold it gets — it has to be squeezed under extra pressure to solidify.
- It's the second most abundant element in the universe after hydrogen, but makes up only a tiny trace of Earth's atmosphere because it's light enough to escape into space.
Frequently asked questions
Why does helium make your voice sound funny?
It's not about your vocal cords — helium is much less dense than air, so sound waves travel through it faster. That changes the resonant frequencies of your vocal tract, shifting the tone of your voice upward without actually changing its pitch at the source.
Why is helium used in balloons instead of hydrogen, if hydrogen is lighter?
Hydrogen is lighter and would lift a balloon slightly better, but it's also flammable and can ignite explosively. Helium is inert and non-flammable, so it's used almost everywhere balloons need to be safe around people, despite being more expensive and rarer to produce.
Is the world actually running out of helium?
In a practical sense, yes. Helium on Earth comes from the slow radioactive decay of uranium and thorium trapped underground, and it's captured mainly as a byproduct of natural gas extraction. Once helium is released into the atmosphere, it's light enough to drift up and escape into space permanently, so known reserves aren't replenished on any human timescale.
Isotopes
8 known isotopes
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| Isotope | Natural abundance | Half-life | Decay mode | Mass excess | Binding energy / nucleon | Decay width |
|---|---|---|---|---|---|---|
| He-3 stable | 0.0002% | Stable | — | 14,931.22 keV | 2,572.68 keV | — |
| He-4 stable | 99.9998% | Stable | — | 2,424.92 keV | 7,073.92 keV | — |
Show all 8 isotopes
| He-5 | — | 0.648 MeV | Neutron emission | 11,231.23 keV | 5,512.13 keV | 6.48 × 105 eV |
| He-6 | — | 806.7 ms | Beta-minus decay (100%) | 17,592.1 keV | 4,878.52 keV | 5.66 × 10-16 eV |
| He-7 | — | 150 keV | Neutron emission | 26,073.13 keV | 4,123.06 keV | 1.50 × 105 eV |
| He-8 | — | 119.1 ms | Beta-minus decay (100%), Beta-minus, neutron emission (16%) | 31,609.68 keV | 3,924.52 keV | 3.83 × 10-15 eV |
| He-9 | — | — | Neutron emission (100%) | 40,935.83 keV | 3,349.04 keV | — |
| He-10 | — | 300 keV | Neutron emission (100%) | 49,197.15 keV | 2,995.13 keV | 3.00 × 105 eV |