Lab help! I did calculations, I need to check my work with something though, so

Question

Lab help! I did calculations, I need to check my work with something though, so please show all work or explain. Conclusions/Questions 1. The sun's almost continuous spectrum, a Fraunhofer lines). Why are these lines missing? few spectra lines are missing (called 2. JJ. Balmer, in 1885, found that the wavelengths of the hydrogen spectrum were related to one another by the formula: Where Rw is a constant called Rydberg constant, 1.10 x 107 m1. The variables ni and n are integers (n2> nl, these integers in fact correspond to the energy levels in a hydrogen atom. An electron transitions from a higher to lower energy level, releasing a photon of a specific energy: Where hcRy is equal to 2.179 x 10-18 J. The energy levels are referred to as n1-final energy state and n initial energy state, so n and n2 n. The Balmer Series represents the spectrum in the visible region where an electron transitions from a higher energy level n' = 3, 4, 5,-e to n 2. Calculate the energy for the first transition in the Balmer series (n-32). Show your work a. Calculate the wavelength for the first transition in the Balmer series (ne3->2). Show your work. b.

Explanation / Answer

1)

This lines are missing since the light is being absorbed by the elements present in sun:

He, O2, Mg, Na,Hg, Fe are some examples of the elements in the sun

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