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The astrophysicist should look for the specific wavelength of light that corresponds to the energy difference between the initial and final states of the transition they are trying to detect. This is typically achieved through spectroscopy, which allows them to identify the exact wavelength of light emitted or absorbed during the transition.

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Related Questions

What wavelength lambda should the astrophysicist look for to detect a transition of an electron from the n equals 7 to the n equals 3 level?

1005 m


What wavelength should the astrophysicist look for to detect a transition of an electron from the n equals 7 to the n equals 3 level?

, Use Rydberg's Equation to solve for this problem, which is as follows: 1/wavelength = R((1/n2x )-(1/ny2 )) Where R is Rydberg's constant, 1.0974 * 107 m-1 And where nx is the lower energy state (n=1), and ny is the higher energy state (n=3). So, plugging in those values gives us the following calculations to be made: 1/(12)=1, and 1/(32)= 1/9, so (1) - (1/9) = 8/9. So, we get: 1/wavelength = (1.0974* 107 m-1)(8/9) = 1/wavelength = (.9754666667 m-1) = wavelength = 1/(.9754666667 m-1) = Wavelength = 1.025150355 * 10-7 m And, since wavelength is typically given in nanometers (1 nm = 1 * 10-9 m) when looking at hydrogren emission spectra, convert the 10-7to 10-9 by moving the decimal back two more places. So, The wavelength expected for light composed of photons produced by an n=3 to n=1 transition in a hydrogen atom is: 102.5150355 nm or, to three significant figures, 103 nm Hope I helped! I am an engineering student at the University of Arizona.


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