On Friday, May 8, 2020 at 4:50:55 PM UTC-6, Lawrence Crowell wrote:
>
> There is no global meaning to energy conservation. There is the 
> Hamiltonian constraint Nℌ = 0, which just says that for a local region 
> where the lapse function can be parallel translated to the energy is zero. 
> This is for Petrov type O solutions 
>
> Nℌ = 0 = ½(da/dt)^2 - 4πGρa^2/3c^3 - k
>
> Which leads to the FLRW constraint
>
> (a’/a)^2 = 8πGρ/3c^3 – k/a^2 a’ = da/dt
>
> Where the Hubble parameter H = 70km/s-Mpc  is (a’/a)^2 = H^2. This means 
> that in a local region we have energy conservation FAPP. The difficulty is 
> this is not a property of the symmetries of the system so we have no way to 
> extend this globally.
>
> What this ultimately means is that all physics is local. It does not mean 
> we have mass-energy locally vanishing. The apparent increase in the kinetic 
> energy due to expansion is well enough compensated for by a decease in 
> gravitational potential energy.
>

This is the claim, but I haven't seen any proof of it. Do you have one? 
Take a planet. Can you show that Mc^2, where M is the planet's mass, is 
equal to its negative gravitational potential energy? AG
 

> There is nothing mysterious going on here. All this means is there is a 
> limitation or horizon to our ability to know if there are global symmetries 
> to the universe. As such there is no meaning to conservation principles.
>

We can estimate the volume of the observable universe and its average 
mass-energy density. So it seems we can estimate its total energy. Does 
that energy remain constant or not as the universe expands? This seems like 
a reasonable question to ask. AG 

>
> LC
>
>
> On Friday, May 8, 2020 at 3:00:18 AM UTC-5, Alan Grayson wrote:
>
>> If it's not conserved, as seems implied by the red shift due to 
>> expansion, where does it go? TIA, AG
>>
>

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