A) What temperature will the energy per mole of a solid achieve one third its classical value of 3RT. Express in terms of einstein temperature(adsbygoogle = window.adsbygoogle || []).push({});

Einstein Temperature [tex] T_{e} = \frac {h \nu}{k} [/tex]

where h is plancks constant

k = boltzmann's constant

Not really sure on how to do this?

Do i use this formula

[tex] C_{v} = \frac{3 N_{a} h^2 \nu^2}{k T^2} \frac{e^\frac{h\nu}{kT}}{(e^\frac{h\nu}{kT} - 1)^2} [/tex]

i know that the term hv / kT must be the exponent of e but i cant get it to work. but that is beside the point

but how do i manipulate it to get what i need?

Now onto the Blackbody radiation topic

IIfyou have the wavelength and the temperature then which function would you use for finding the Total Radiancy?

R = Sigma T^4 or the big formula 2pi h c^2 / lambda ^5 ( 1 / e^ hc / lambda k T)

Which is the the Total radiancy function?

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# Homework Help: In terms of Einstein's theory of heat capacity

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