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What is the longest wavelength that can be observed in the third order for a transmission grating having 9200 slits/cm? Assume normal incidence.

Short Answer

Expert verified
The longest wavelength that can be observed in the third order for a transmission grating having 9200 slits/cm is approximately \(3623\) nm.

Step by step solution

01

Calculate the grating spacing

First, determine the spacing between the slits \(d\). We are given the number of slits per cm, so we take its reciprocal to get the distance between two adjacent slits in cm, and then convert it to meter. Here, grating spacing \(d = \frac{1}{9200}\) cm = \(1.0869565 \times 10^{-5}\) m.
02

Identify the order

The order \(m\) is given as 3.
03

Calculate the wavelength

From the grating equation \(mλ = d\), we can rearrange it for the wavelength \(λ\), it becomes \(λ = \frac{d}{m}\). Substituting the values for \(d\) and \(m\) into the equation gives \(λ = \frac{1.0869565 \times 10^{-5}}{3}\), resulting in λ = \(3.623188833 \times 10^{-6}\) m or approx. \(3623\) nm.

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Key Concepts

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

Transmission Grating
A transmission grating, a key tool in optical physics, is essentially a thin sheet of material that has a large number of parallel lines or slits etched into it at regular intervals. When light passes through the grating, it spreads out or 'diffracts' into its component colors or wavelengths. This phenomenon occurs because light waves interfere with each other constructively and destructively based on the spacing between the slits (referred to as the grating spacing) and the wavelength of the light.

Transmission gratings are used in various applications, including spectroscopy, where they help to analyze the spectral composition of light. They differ from reflection gratings, which reflect light, in that they allow light to pass through them, making them useful in situations where transmitting light is preferable or more practical.
Grating Equation
The grating equation is fundamental in understanding how diffraction gratings work. It relates the angle at which light of a particular wavelength is diffracted to the spacing of the grating and the order of the diffracted light. Mathematically, the grating equation is expressed as \( m\lambda = d\sin(\theta) \), where \( m \) is the order of the diffraction pattern, \( \lambda \) is the wavelength of the light, \( d \) is the grating spacing, and \( \theta \) is the diffraction angle.

The equation allows us to calculate the wavelength of light if the other variables are known, or conversely, to determine the grating constant or the diffraction angle when other parameters are given. It is a powerful tool in the field of optics to analyze light behavior and the properties of materials that interact with light.
Wavelength Order
In optics physics, 'wavelength order,' or simply 'order,' refers to the term \( m \) in the grating equation and signifies the series of spectra produced by diffraction. Each order corresponds to a multiple of the wavelength that constructively interferes to form visible patterns. The first order \( (m=1) \) is the principal order, but higher orders \( (m=2, 3, 4,...) \) can also be observed, each being less intense than the previous one.

The concept of order is critical in understanding the diffracted patterns and the resolution of a grating. A higher order often provides greater resolution but can lead to complications like overlapping of the spectra from different orders, which is something to account for in detailed spectral analysis.
Optics Physics
Optics physics is the area of physics that focuses on the study of light and its interactions with matter. It encompasses a range of phenomena, including reflection, refraction, diffraction, and interference. Diffraction grating falls into the category of diffraction, which examines how waves spread out as they pass through an aperture or around an obstacle that disrupts their path.

The study of optics is essential in many technological advances and practical applications. It underlies the tools and instruments used in areas such as astronomy, telecommunications, medical imaging, and even everyday objects like cameras and eyeglasses. Grasping the concepts in optics, such as how a diffraction grating functions, enables a deep understanding of the behavior of light and its manipulation for various technological applications.

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Most popular questions from this chapter

(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 \(P\) (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 \(e^{i z}=\cos z+i \sin z,\) where \(i=\sqrt{-1} .\) In this expression, \(\cos z\) is the real part of the complex number \(e^{i z}\), 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 $$ \sum_{n=0}^{N-1} E_{0} e^{i(k R-\omega t+n \phi)} $$ (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 $$ \begin{aligned} E_{0} &\left(\frac{e^{i N \phi}-1}{e^{i \phi}-1}\right) e^{i(k R-\omega t)} \\\ &=E_{0}\left(\frac{e^{i N \phi / 2}-e^{-i N \phi / 2}}{e^{i \phi / 2}-e^{-i \phi / 2}}\right) e^{j[k R-\omega t+(N-1) \phi / 2]} \end{aligned} $$ Then, using the relationship \(e^{i z}=\cos z+i \sin z,\) 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 amplitude 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 \(580 \mathrm{nm}\) passes through a single slit and the diffraction pattern is observed on a screen. Both the source and screen are far enough from the slit for Fraunhofer diffraction to apply. (a) If the first diffraction minima are at \(\pm 90.0^{\circ},\) so the central maximum completely fills the screen, what is the width of the slit? (b) For the width of the slit as calculated in part (a), what is the ratio of the intensity at \(\theta=45.0^{\circ}\) to the intensity at \(\theta=0 ?\)

Quasars, an abbreviation for quasi-stellar radio sources, are distant objects that look like stars through a telescope but that emit far more electromagnetic radiation than an entire normal galaxy of stars. An example is the bright object below and to the left of center in Fig. \(\mathrm{P} 36.58 ;\) the other elongated objects in this image are normal galaxies. The leading model for the structure of a quasar is a galaxy with a supermassive black hole at its center. In this model, the radiation is emitted by interstellar gas and dust within the galaxy as this material falls toward the black hole. The radiation is thought to emanate from a region just a few light-years in diameter. (The diffuse glow surrounding the bright quasar shown in Fig. \(\mathrm{P} 36.58\) is thought to be this quasar's host galaxy.) To investigate this model of quasars and to study other exotic astronomical objects, the Russian Space Agency has placed a radio telescope in a large orbit around the earth. When this telescope is \(77,000 \mathrm{~km}\) from earth and the signals it receives are combined with signals from the ground-based telescopes of the VLBA, the resolution is that of a single radio telescope \(77,000 \mathrm{~km}\) in diameter. What is the size of the smallest detail that this arrangement can resolve in quasar \(3 \mathrm{C} 405,\) which is \(7.2 \times 10^{8}\) light-years from earth, using radio waves at a frequency of \(1665 \mathrm{MHz}\) ? (Hint: Use Rayleigh's criterion.) Give your answer in lightyears and in kilometers.

A series of parallel linear water wave fronts are traveling directly toward the shore at \(15.0 \mathrm{~cm} / \mathrm{s}\) on an otherwise placid lake. A long concrete barrier that runs parallel to the shore at a distance of \(3.20 \mathrm{~m}\) away has a hole in it. You count the wave crests and observe that 75.0 of them pass by each minute, and you also observe that no waves reach the shore at \(\pm 61.3 \mathrm{~cm}\) from the point directly opposite the hole, but waves do reach the shore everywhere within this distance. (a) How wide is the hole in the barrier? (b) At what other angles do you find no waves hitting the shore?

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