Editing Exoplanets (section)

== <span style="color: #FFFFFF;">Understanding</span> ==
The search for life is a search for '''Water''', '''Energy''', and '''Stability'''.

'''1. How we find them''':
* '''Transit (Kepler/TESS)''': This is how we've found most planets. If a star's light drops by 1% every 365 days, we know there's a planet there.
* '''Radial Velocity''': As a planet orbits, its gravity pulls the star back and forth. We see this as a "shift" in the star's light color (Doppler Effect).

'''2. The Habitable Zone''':
Life (as we know it) needs liquid water.
* If a planet is too close to its star, the water boils away (Venus).
* If it's too far, the water freezes (Mars).
The "Goldilocks Zone" is the sweet spot in between. For a small, cool star (Red Dwarf), this zone is very close to the star. For a hot, blue star, it is very far away.

'''3. Searching for 'The Fingerprint'''':
When a planet transits its star, a tiny bit of starlight passes through the planet's atmosphere. By analyzing that light, we can see "dips" that correspond to specific molecules. If we see '''Oxygen''' and '''Methane''' together, it's a huge sign of life, because those two gases normally destroy each other. Only life (like plants and cows) keeps producing them both.
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