On Sat, Sep 14, 2019 at 10:13:27PM -0700, Alan Grayson wrote:
> 
> 
> On Saturday, September 14, 2019 at 7:12:34 AM UTC-6, Alan Grayson wrote:
> 
>     If the early universe, say before the emergence of the CMBR, consisted of 
> a
>     random collection of electrons and photons, wouldn't this correspond to a
>     high, not low entropy? Wouldn't it be analogous to gas with many possible
>     states? Yet cosmologists seem hard pressed to explain an initial or early
>     state assuming the entropy is low. AG
> 
> 
> When I was an undergraduate I took a course in Classical Thermodynamics and
> recall being satisfied that entropy was well-defined. I never took a course in
> Classical Statistical Mechanics, but I've seen Boltzmann's equation for S and
> wonder how N, the number of possible states is defined. If we have a gas
> enclosed in a container, we can divide it into occupation cells of fixed 
> volume
> to calcuate S. But why can't we double the number of cells by reducing their
> volume by half? How then is S well defined in the case of Classical 
> Statistical
> Mechanics? TIA, AG

It actually isn't. The point bothered me too. The number of states is
basically V/h, where V is the volume of phase space occupied by the
system, and h a cell size. Therefore, entropy is

klog V  - klog h

For a large range of values of h, the second term is just a negligible
constant offset to the total entropy. However, as h→0, entropy blows
up. And that what classical statistical mechanics tells you.

Enter quantum mechanics. Heisenberg's uncertainty relation tells us
that ΔxΔp ≥ ℏ, so in the above entropy formula, h is constrained to be
larger than ℏ³. Quantum mechanics saves classical statistical physics'
bacon. Nothing blows up.

-- 

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Dr Russell Standish                    Phone 0425 253119 (mobile)
Principal, High Performance Coders
Visiting Senior Research Fellow        [email protected]
Economics, Kingston University         http://www.hpcoders.com.au
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