interpreted Eq. (3.26), with n equal zero (4 dimensions) with a 10
2 plank mass
(in four dimensions) black hole, that we would have
T H / 1 TeV Á
1
1:22 Â 10
21
Á 2 Á
ffiffiffi
π
p
Á
1
4
ffiffiffi
π
p
ð3:28Þ
Noticeably we have a set of reality problems to attend to. Hawking radiation and
the Ng (2008) paradigm alter our process so that we obtain the following results as
given in Eq. (3.29) for Hawking blackbody style results.
Diosi (2019) and Calmet (n.d.) will add further refinement as to the physics of Eq.
(3.29) and hopefully alter them to reflect more of the known observational physics,
since Eq. (3.29) is a greatly over simplified version of the gravitational physics input
into observational gravitational astronomy. We hope in doing so we obtain data sets
as to confirm or falsify our hypothesis as given in this document.
T H normal À 4dim
ð
Þ ¼
ħc
3
8πGm bh k B
¼ 6:17 Â 10
À8 K À if m bh ¼ 1 À solar‐mass
T H normal À 4dim
ð
Þ ¼
ħc
3
8πGm bh k B
’ 6:17 Â 10
28 K À if m bh ¼ 10
2
 m planck 4 À dim
ð
Þ
T H normal À 4dim
ð
Þ ¼
6:17 Â 10
28
11, 604
eV À if m bh ¼ 10
2
 m planck 4 À dim
ð
Þ
T H normal À 4dim
ð
Þ ¼ 5:317 Â 10
12 TeV À if m bh ¼ 10
2
 m planck 4 À dim
ð
Þ
ð3:29Þ
The sun is 9.8 times 10
37 Planck masses, so this means that the Hawkings
temperature of a 10
2 times four-dimensional Planck mass black hole, as postulated
here would be then about 10
36 times higher, 1 eV in Kelvin is 11,604 K, hence if we
have only n ¼ 0 we really would prefer not to use Eq. (3.28). Hence, using
Eq. (3.29). we can then go to Hawking (1974) for entropy, i.e., we have then that
S bh ¼
1 þ n
2 þ n
Á
m bh
T bh
¼
1 þ n
2 þ n
Á
10
2
 m planck 4 À dim
ð
Þ
5:317 Â 10
12 TeV
%
1 þ n
2 þ n
Á
10
2
 1:22  10
16 TeV
5:317 Â 10
12 TeV
S bh %
1 þ n
4 þ 2n
Á 10
4
!
n!0
10
3
ð3:30Þ
That is, if we had 10
2 black holes, of mass about 10
2 times a four-dimensional black
hole, we probably would be looking at an initial entropy of about 10
5 . Then using
Kolb and Turner (1991), we would see
3 Using ”Enhanced Quantization“ to Bound the Cosmological Constant, (for a. . .
33
2 plank mass
(in four dimensions) black hole, that we would have
T H / 1 TeV Á
1
1:22 Â 10
21
Á 2 Á
ffiffiffi
π
p
Á
1
4
ffiffiffi
π
p
ð3:28Þ
Noticeably we have a set of reality problems to attend to. Hawking radiation and
the Ng (2008) paradigm alter our process so that we obtain the following results as
given in Eq. (3.29) for Hawking blackbody style results.
Diosi (2019) and Calmet (n.d.) will add further refinement as to the physics of Eq.
(3.29) and hopefully alter them to reflect more of the known observational physics,
since Eq. (3.29) is a greatly over simplified version of the gravitational physics input
into observational gravitational astronomy. We hope in doing so we obtain data sets
as to confirm or falsify our hypothesis as given in this document.
T H normal À 4dim
ð
Þ ¼
ħc
3
8πGm bh k B
¼ 6:17 Â 10
À8 K À if m bh ¼ 1 À solar‐mass
T H normal À 4dim
ð
Þ ¼
ħc
3
8πGm bh k B
’ 6:17 Â 10
28 K À if m bh ¼ 10
2
 m planck 4 À dim
ð
Þ
T H normal À 4dim
ð
Þ ¼
6:17 Â 10
28
11, 604
eV À if m bh ¼ 10
2
 m planck 4 À dim
ð
Þ
T H normal À 4dim
ð
Þ ¼ 5:317 Â 10
12 TeV À if m bh ¼ 10
2
 m planck 4 À dim
ð
Þ
ð3:29Þ
The sun is 9.8 times 10
37 Planck masses, so this means that the Hawkings
temperature of a 10
2 times four-dimensional Planck mass black hole, as postulated
here would be then about 10
36 times higher, 1 eV in Kelvin is 11,604 K, hence if we
have only n ¼ 0 we really would prefer not to use Eq. (3.28). Hence, using
Eq. (3.29). we can then go to Hawking (1974) for entropy, i.e., we have then that
S bh ¼
1 þ n
2 þ n
Á
m bh
T bh
¼
1 þ n
2 þ n
Á
10
2
 m planck 4 À dim
ð
Þ
5:317 Â 10
12 TeV
%
1 þ n
2 þ n
Á
10
2
 1:22  10
16 TeV
5:317 Â 10
12 TeV
S bh %
1 þ n
4 þ 2n
Á 10
4
!
n!0
10
3
ð3:30Þ
That is, if we had 10
2 black holes, of mass about 10
2 times a four-dimensional black
hole, we probably would be looking at an initial entropy of about 10
5 . Then using
Kolb and Turner (1991), we would see
3 Using ”Enhanced Quantization“ to Bound the Cosmological Constant, (for a. . .
33