Direct Methods for Finding Exoplanets

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Presentation transcript:

Direct Methods for Finding Exoplanets 21 October 2016

What is a planet? Does not shine by its own light Too small to burn hydrogen (or even deuterium) by nuclear fusion Forms from a disk around a star, not a multiple star

How to detect a planet Directly Indirectly Reflected light from the star Emitted light from the planet Indirectly Absorbs or blocks light Refracts (bends) light Changes the motion of nearby objects by gravity

Reflected light Like Moon, Venus, Jupiter: even visible in daylight on Earth, if you know where to look Necessary Enough reflected light: decreases as square of distance Separation of star and planet: angular separation of a distant object Telescope resolution: capability to see two nearby objects: increases with telescope size Sensitivity to see dim object near bright star: biggest problem

Emitted vs reflected light Brightness increases with temperature But wavelength of brightest emission decreases with temperature: hotter stars are more blue, cooler objects are redder Go long! (look for planets at longer wavelengths)

4 planets

Sunshade idea is under development at CU

Summary: Direct Methods In principle, it is possible to see exoplanets by the light they reflect, but the brightness difference is too large: like a moth in a searchlight. Only a few cases found… Infra-red light (IR) is more promising, because the planets are only a million times dimmer Shades, coronagraphs, adaptive optics, interferometry improve this Next time: indirect methods

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