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Ch 36: Diffraction
Young & Freedman Calc - University Physics 14th Edition
Young & Freedman Calc14th EditionUniversity PhysicsISBN: 9780321973610당신이 사용하는 게 아니라요?교과서 변경
36장, 문제 41

The VLBA (Very Long Baseline Array) uses a number of individual radio telescopes to make one unit having an equivalent diameter of about 8000 km. When this radio telescope is focusing radio waves of wavelength 2.0 cm, what would have to be the diameter of the mirror of a visible-light telescope focusing light of wavelength 550 nm so that the visible-light telescope has the same resolution as the radio telescope?

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The resolution of a telescope is determined by the formula for angular resolution: θ = 1.22 * (λ / D), where θ is the angular resolution, λ is the wavelength of the light or radio waves, and D is the diameter of the telescope's aperture.
To ensure the visible-light telescope has the same resolution as the radio telescope, the angular resolution θ must be the same for both. Therefore, we can set up the equation: 1.22 * (λ_radio / D_radio) = 1.22 * (λ_visible / D_visible).
Simplify the equation by canceling out the common factor 1.22: (λ_radio / D_radio) = (λ_visible / D_visible).
Rearrange the equation to solve for D_visible: D_visible = (λ_visible * D_radio) / λ_radio.
Substitute the given values into the equation: λ_radio = 2.0 cm = 0.02 m, D_radio = 8000 km = 8,000,000 m, and λ_visible = 550 nm = 550 * 10^(-9) m. Perform the substitution and simplify to find the required diameter of the visible-light telescope's mirror.

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Resolution in Telescopes

Resolution refers to the ability of a telescope to distinguish between two closely spaced objects. It is determined by the diameter of the telescope's aperture and the wavelength of light being observed. A larger aperture allows for better resolution, enabling the telescope to resolve finer details in the observed objects.
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Diffraction Limit

The diffraction limit is a fundamental limit to the resolution of optical systems, including telescopes, caused by the wave nature of light. It can be quantified using the formula θ = 1.22(λ/D), where θ is the angular resolution in radians, λ is the wavelength of light, and D is the diameter of the aperture. This principle explains why longer wavelengths result in poorer resolution.
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Wavelength Comparison

Wavelength is a key factor in determining the resolution of telescopes. In this context, the VLBA operates at a wavelength of 2.0 cm (20,000 nm), while the visible-light telescope operates at 550 nm. To achieve the same resolution, the diameter of the visible-light telescope must be calculated based on the ratio of these wavelengths, highlighting the relationship between wavelength and aperture size.
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