For wavelengths less than about 1 cm, the dispersion relation for waves on the surface of water is ω=(γ/p)k3, whereandare the surface tension and density of water. Givenγ=0.072N/mandp=103kg/m3, calculate the phase and group velocities for a wave of 5mm wavelength.

Short Answer

Expert verified

The phase velocity for a wave is 0.3 m/s

The group velocity for a wave is 0.45 m/s

Step by step solution

01

 Concept involved

Waves of different wavelengths travel at different phase speeds. Water waves on the surface propagate with gravity and surface tension as the restoring forces.

02

 Formulae used        

The dispersion relation for waves on the surface of water is

ω=γ/pk3

Where,γand p are the surface tension and density of water

The phase velocity is,

vphase=γ/pk3k

The group velocity is,

vgroup=dωdkk0

03

 Determining the wave number

The wave number, k is given by

k=2πλ

Where, λ= wavelength

k=2π5×10-3m=1.265×103m-1

04

 Calculating the angular frequency

Calculate the angular frequencyω, using the wave number k, surface tension of waterγ, and the density of water p

ω=γpk3

Substitute the values of γ, pand k to get ω

ω=0.072kg/s2103kg/m31.265×10-3m-13=377.99rad/s

05

 Calculating the phase velocity

vphase=γ/pk3kvphase=γpk

Substitute the values of γ, pand k

vphase=0.072kg/s2103kg/m31.265×10-3m-1=0.3m/s

06

 Calculating the group velocity

Group velocity is calculated by taking a derivation of the angular frequencyωwith respect to the wave number k

vgroup=dkk0=12γk3p-1/23γk2pk0=32γk0p

Use the wave number k as the median wave number k0

vgroup=32(0.072kg/s2)(1.265×10-3m-1)103kg/m3=0.45m/s

07

 Conclusion        

Therefore, phase velocity for a wave is 0.3 m/s

The group velocity for a wave is 0.45 m/s

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Most popular questions from this chapter

For wavelengths greater than about,20cm the dispersion relation for waves on the surface of water isω=gk

(a) Calculate the phase and group velocities for a wave ofwavelength.

(b) Will the wave spread as it travels? Justify your answer.

Given the situation of exercise 25, show that

(a) as Uo, reflection probability approaches 1 and

(b) as L0, the reflection probability approaches 0.

(c) Consider the limit in which the well becomes infinitely deep and infinitesimally narrow--- that is Uoand data-custom-editor="chemistry" L0but the product U0L is constant. (This delta well model approximates the effect of a narrow but strong attractive potential, such as that experienced by a free electron encountering a positive ion.) Show that reflection probability becomes:

R=[1+2h2EmUoL2]-1

Fusion in the Sun: Without tunnelling. our Sun would fail us. The source of its energy is nuclear fusion. and a crucial step is the fusion of a light-hydrogen nucleus, which is just a proton, and a heavy-hydrogen nucleus. which is of the same charge but twice the mass. When these nuclei get close enough. their short-range attraction via the strong force overcomes their Coulomb repulsion. This allows them to stick together, resulting in a reduced total mass/internal energy and a consequent release of kinetic energy. However, the Sun's temperature is simply too low to ensure that nuclei move fast enough to overcome their repulsion.

a) By equating the average thermal kinetic energy that the nuclei would have when distant,32KBT. and the Coulomb potential energy they would have when 2fm apart, roughly the separation at which they stick, show that a temperature of about 1019K would be needed.

b) The Sun's core is only about 10k. If nuclei can’t make it "over the top." they must tunnel. Consider the following model, illustrated in the figure: One nucleus is fixed at the origin, while the other approaches from far away with energyE. As rdecreases, the Coulomb potential energy increases, until the separation ris roughly the nuclear radius rnuc. Whereupon the potential energy is Umaxand then quickly drops down into a very deep "hole" as the strong-force attraction takes over. Given then EUmax, the point b, where tunnelling must begin. will be very large compared with rnuc, so we approximate the barrier's width Las simply b. Its height, U0, we approximate by the Coulomb potential evaluated at b2. Finally. for the energy Ewhich fixes b, let us use 4×32KBT. which is a reasonable limit, given the natural range of speeds in a thermodynamic system.Combining these approximations, show that the exponential factor in the wide-barrier tunnelling probability is

exp[-e24πε0h4m3kBT]

c)Using the proton mass for , evaluate this factor for a temperature of107K. Then evaluate it at3000K. about that of an incandescent filament or hot flame. and rather high by Earth standards. Discuss the consequences.

For the E>U0 potential barrier, the reflection, and transmission probabilities are the ratios:

R=B*BA*AT=F*FA*A

Where A, B, and F are multiplicative coefficients of the incident, reflected, and transmitted waves. From the four smoothness conditions, solve for B and F in terms of A, insert them in R and T ratios, and thus derive equations (6-12).

From equations (6-23) and (6-29) obtain the dispersion coefficient for matter waves (in vacuum), then show that probability density (6-35) follows from (6-28)

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