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Hubble Versus Arecibo. The Hubble Space Telescope has an aperture of 2.4 \(\mathrm{m}\) and focuses visible light \((400-700 \mathrm{nm}) .\) The Arecibo radio telescope in Puerto Rico is 305 \(\mathrm{m}(1000 \mathrm{ft})\) in diameter (it is built in a mountain valley) and focuses radio waves of wavelength \(75 \mathrm{cm} .\) (a) Under optimal viewing conditions, what is the smallest crater that each of these telescopes could resolve on our moon? (b) If the Hubble Space Telescope were to be converted to surveillance use, what is the highest orbit above the surface of the earth it could have and still be able to resolve the license plate (not the letters, just the plate) of a car on the ground? Assume optimal viewing conditions, so that the resolution is diffraction limited.

Short Answer

Expert verified
Hubble can resolve 120 m craters on the moon and 15 cm license plates from 620 km orbit. Arecibo can resolve 20 km craters on the moon.

Step by step solution

01

Understanding Diffraction Limit

To determine the smallest resolvable feature or crater, we use the formula for the diffraction limit for a circular aperture: \( \theta = 1.22 \frac{\lambda}{D} \), where \( \theta \) is the angular resolution in radians, \( \lambda \) is the wavelength, and \( D \) is the aperture (or diameter) of the telescope. This gives us the smallest angle two points can subtend and still be distinguished.
02

Calculate Moon's Distance in Radians

The distance to the moon is approximately \( 384,400 \ km \). Convert the angular resolution \( \theta \) found in terms of radians to an actual size on the moon by using the formula: \( \text{Size on Moon} = \theta \times \text{Moon's Distance} \). This will yield the size of the smallest crater that can be resolved.
03

Hubble Space Telescope: Visible Light Calculation

For the Hubble telescope, use the average visible light wavelength, \( \lambda = 550 \ nm \) (or \( 550 \times 10^{-9} \ m \)), and the diameter \( D = 2.4 \ m \). Calculate \( \theta = 1.22 \frac{550 \times 10^{-9}}{2.4} \). Convert \( \theta \) into a size on the moon using the previous step calculation.
04

Arecibo Telescope: Radio Wave Calculation

For the Arecibo telescope, use the wavelength \( \lambda = 0.75 \ m \) and \( D = 305 \ m \). Calculate \( \theta = 1.22 \frac{0.75}{305} \). Again, convert \( \theta \) into a size on the moon using the method described earlier.
05

Determine Hubble's Crater Resolving Capability

Compute the smallest crater Hubble can resolve by calculating its size on the moon using the \( \theta \) from Step 3 and the moon's distance from Step 2.
06

Determine Arecibo's Crater Resolving Capability

Compute the smallest crater Arecibo can resolve using its \( \theta \) from Step 4 and converting this to a size as in Step 5.
07

Hubble for Earth Surveillance

For reconnaissance, the Hubble telescope's angular resolution \( \theta \) translates to \( 15 \ cm \) (the standard size of a license plate) on Earth. Use the formula \( h = \frac{\text{License Plate Size}}{\theta} \) to find the maximum height \( h \) at which the Hubble can resolve a 15 cm license plate.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Angular Resolution
Angular resolution is a crucial concept that determines how well a telescope can distinguish between two closely spaced objects. It is defined by the smallest angular separation at which two objects can be seen as distinct from each other.
- For telescopes, angular resolution is diffraction-limited, meaning it is fundamentally constrained by the physics of wave diffraction.
- The formula used is \[ \theta = 1.22 \frac{\lambda}{D} \] where \( \theta \) is the angular resolution in radians, \( \lambda \) is the wavelength of light, and \( D \) is the diameter of the telescope's aperture.
- A smaller \( \theta \) indicates better resolution, allowing finer details to be observed. For example, this principle helps both the Hubble Space Telescope and the Arecibo radio telescope resolve features at different scales due to the varying wavelengths they observe.
Hubble Space Telescope
The Hubble Space Telescope (HST) is a renowned space-based observatory focusing on visible light. Its aperture is 2.4 meters.
- This telescope is optimized for capturing high-resolution images of astronomical objects without atmospheric distortion.
- Observing in the visible light spectrum (wavelengths from 400 to 700 nanometers), the HST benefits from the absence of Earth's atmosphere affecting its observations.
- A key feature of Hubble is its ability to resolve fine details such as distant galaxies and small features on celestial bodies, like craters on the Moon. Under optimal conditions, Hubble's angular resolution is considerably finer than ground-based telescopes of similar size due to its position outside the Earth's atmosphere.
Arecibo Radio Telescope
The Arecibo radio telescope was one of the largest single-aperture telescopes in the world, with a colossal diameter of 305 meters.
- Primarily focused on radio wave detection, it could detect radio waves with wavelengths around 75 cm.
- Unlike optical telescopes, radio telescopes like Arecibo provide information on cosmic phenomena through radio frequencies, which can penetrate dust clouds that obscure visible light.
- Despite its large size, the Arecibo telescope's angular resolution for radio waves was lower than that of Hubble for visible light due to the larger wavelength it had to work with. Thus, it was better suited for observing larger-scale structures rather than fine details.
Visible Light and Radio Waves
Visible light and radio waves are both forms of electromagnetic radiation but differ in their wavelengths.
- Visible light has wavelengths between 400 nm and 700 nm. It is detected by optical telescopes like Hubble and can show detailed images of visible objects.
- Radio waves, on the other hand, have much longer wavelengths, ranging from millimeters to several meters. Arecibo specialized in capturing these longer wavelengths.
- While radio waves are used to explore parts of the universe invisible to the naked eye, visible light allows us to see objects as perceived by human sight.
- Each type of wave has specific advantages and limitations concerning angular resolution, meaning they are used for different observational purposes in astronomy. Understanding these differences is essential when analyzing data from telescopes like Hubble and Arecibo.

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Most popular questions from this chapter

Intensity Pattern of \(N\) Slits. (a) Consider an arrangement of \(N\) slits with a distance \(d\) between adjacent slits. The slits emit coherently and in phase at wavelength \(\lambda\) . Show that at a time \(t,\) the electric field at a distant point \(P\) is $$ \begin{aligned} E_{P}(t)=& E_{0} \cos (k R-\omega t)+E_{0} \cos (k R-\omega t+\phi) \\ &+E_{0} \cos (k R-\omega t+2 \phi)+\cdots \\ &+E_{0} \cos (k R-\omega t+(N-1) \phi) \end{aligned} $$ where \(E_{0}\) is the amplitude at \(P\) of the electric field due to an individual slit, \(\phi=(2 \pi d \sin \theta) / \lambda, \theta\) is the angle of the rays reaching \(P(\text { as measured from the perpendicular bisector of the slit arrangement }\)), and \(R\) is the distance from \(P\) to the most distant slit. In this problem, assume that \(R\) is much larger than \(d .\) (b) To carry out the sum in part \((a),\) it is convenient to use the complex-number relationship $$ e^{i k}=\cos z+i \sin z $$ where \(i=\sqrt{-1}\) . In this expression, \(\cos z\) is the real part of the complex number \(e^{i k},\) and \(\sin z\) is its imaginary part. Show that the electric field \(E_{P}(t)\) is equal to the real part of the complex quantity $$ \sum_{n=0}^{N-1} E_{0} e^{i(k R-\omega+n \phi)} $$ (c) Using the properties of the exponential function that \(e^{A} e^{B}=e^{(A+B)}\) and \(\left(e^{A}\right)^{n}=e^{n A},\) show that the sum in part \((b)\) can be written as $$ E_{0}\left(\frac{e^{i N \phi}-1}{e^{i \phi}-1}\right) e^{i(k R-\omega t)}=E_{0}\left(\frac{e^{i N \phi / 2}-e^{-i N \phi / 2}}{e^{i \phi / 2}-e^{-i \phi / 2}}\right) e^{i(k R-\omega t+(N-1) \phi / 2]} $$ Then, using the relationship \(e^{i k}=\cos z+i \sin z,\) show that the (real) electric field at point \(P\) is $$ E_{p}(t)=\left[E_{0} \frac{\sin (N \phi / 2)}{\sin (\phi / 2)}\right] \cos [k R-\omega t+(N-1) \phi / 2] $$ The quantity in the first square brackets in this expression is the amphitude of the electric field at \(P .\) (d) Use the result for the electric-field amplitude in part (c) to show that the intensity at an angle \(\theta\) is $$ I=I_{0}\left[\frac{\sin (N \phi / 2)}{\sin (\phi / 2)}\right]^{2} $$ where \(I_{0}\) is the maximum intensity for an individual slit. (e) Check the result in part (d) for the case \(N=2\) . It will help to recall that \(\sin 2 A=2 \sin A \cos A\) . Explain why your result differs from Eq. \((35.10),\) the expression for the intensity in two-source interference, by a factor of \(4 .\) (Hint: Is \(I_{0}\) defined in the same way in both expressions?)

Monochromatic light of wavelength \(\lambda=620 \mathrm{nm}\) from a distant source passes through a slit 0.450 \(\mathrm{mm}\) wide. The diffraction pattern is observed on a screen 3.00 \(\mathrm{m}\) from the slit. In terms of the intensity \(I_{0}\) at the peak of the central maximum, what is the intensity of the light at the screen the following distances from the center of the central maximum: (a) \(1.00 \mathrm{mm} ;\) (b) 3.00 \(\mathrm{mm}\) ; (c) 5.00 \(\mathrm{mm}\) ?

What is the longest wavelength that can be observed in the third order for a transmission grating having 6500 slits \(/ \mathrm{cm} ?\) Assume normal incidence.

A diffraction grating has 650 slits \(/ \mathrm{mm}\) . What is the highest order that contains the entire visible spectrum? (The wavelength range of the visible spectrum is approximately \(400-700 \mathrm{nm} . )\)

Measuring Refractive Index. A thin slit illuminated by light of frequency \(f\) produces its first dark band at \(\pm 38.2^{\circ}\) in air. When the entire apparatus (slit, screen, and space in between) is immersed in an unknown transparent liquid, the slit's first dark bands occur instead at \(\pm 17.4^{\circ} .\) Find the refractive index of the liquid.

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