On 7/23/2020 4:41 AM, Lawrence Crowell wrote:
On Thursday, July 23, 2020 at 5:56:32 AM UTC-5 [email protected] wrote:
On Saturday, July 18, 2020 at 6:31:23 AM UTC-6, Alan Grayson wrote:
On Saturday, July 18, 2020 at 6:18:28 AM UTC-6, Lawrence
Crowell wrote:
The tortoise coordinates is found from the Schwarzschild
metric
ds^2 = (1 - 2m/r)dt^2 - (1 - 2m/r)^{-1}dr^2 - r^2dΩ^2
where for a signal leaving a point near the black hole
with ds = 0 (null path) and propagating radially out, dΩ =
0, we have dt = dr/(1 - 2m/r) which then leads to
T = t - t0 - 2m ln|r - 2m|.
That is the tortoise coordinate. Please look this up to
read further. I can't spend beaucoup time going over this
for weeks to come.
LC
You don't have to. We're done. But you should IMO address
Brent's objection, maybe on another thread. AG
I don't know what objection you're referring to. LC is just showing why
it takes a distant observer forever to see an infalling object reach the
event horizon of a black hole.
Brent
When it comes to GR, you're a genius; no question about it. I
wouldn't want to waste your valuable time. But consider this; the
Schwartzschild metric applies to NON-ROTATING masses. Do you
really think a massive contracting star which forms a BH will be
non-rotating? Obviously, it will be RAPIDLY rotating, like an ice
skater who contracts her arms. Brent also had some substantive
questions about your model. But I see you prefer your illusions
than to address his objections. AG
The result is similar, but more complex. The same calculation can be
done for the Kerr solution. It is just a lot more complicated
mathematically.
LC
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