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stunner5000pt
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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
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 can't 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?
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 can't 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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