486
R. MacKenzie et al.
substance. Further, due to the demand of neutrality, the heavier gas Y cannot expand
either, although it has no condensation effects. Let us denote the number density of
the magninos trapped in the walls to be n X
walls and the remainder residing in the
enclosed domains by n X
bulk . Averaged (coarse grained) over a volume much larger
than the L 3 , this gives the average number density of the magninos to be
X
=
ω
L
n
X
walls +
1 −
ω
L
n
X
bulk
(6)
And from the neutrality condition we have
X
= =n
Y
(7)
Then we can demand that PAAI in this phase acts as the DE, so that assuming Y to
be non-relativistic, and ignoring other contributions,
ρ
Y
≈ m Y
Y
= ρ DE = 2.81 × 10
−11 (eV)
4
(8)
We can express the number density of Y as a ratio of the number density n γ =
3.12 × 10 −12 (eV) 3 of photons, and set η Y = =n Y /n γ . Then we can obtain
conditions that determine the ratio
m M
m Y
=
β Y
β
≈ (η
Y )
4/3
× 10
−6 λ1
( 9 )
These are the essential constraints determining the key parameters of our model.
Then we find that m M ranges over 10 −4 to 10 −6 eV corresponding to η Y ranging
from 10 −4 to 10 −8 eV; and m Y , respectively, ranges from 1 keV to 1 GeV. Further,
we can also develop a corresponding multi-flavour dark sector so that Dark Matter
can also be accommodated as neutral atoms of this sector. The details can be found
in [11].
5 Origin of Cosmic Magnetic Fields
The origin and evolution of galactic scale magnetic fields is an open question
[18, 31]. In particular the extent of seed magnetic field as against that generated
by subsequent motion is probably experimentally distinguishable [19, 20]. In the
present case, we can estimate the field strength of the X-magnetism in each domain,
and is found to be
B dom ≈
m M
eV
2
e
e
β
0.1
3
× 2.2 × 10
−8 T
(10)
R. MacKenzie et al.
substance. Further, due to the demand of neutrality, the heavier gas Y cannot expand
either, although it has no condensation effects. Let us denote the number density of
the magninos trapped in the walls to be n X
walls and the remainder residing in the
enclosed domains by n X
bulk . Averaged (coarse grained) over a volume much larger
than the L 3 , this gives the average number density of the magninos to be
X
=
ω
L
n
X
walls +
1 −
ω
L
n
X
bulk
(6)
And from the neutrality condition we have
X
= =n
Y
(7)
Then we can demand that PAAI in this phase acts as the DE, so that assuming Y to
be non-relativistic, and ignoring other contributions,
ρ
Y
≈ m Y
Y
= ρ DE = 2.81 × 10
−11 (eV)
4
(8)
We can express the number density of Y as a ratio of the number density n γ =
3.12 × 10 −12 (eV) 3 of photons, and set η Y = =n Y /n γ . Then we can obtain
conditions that determine the ratio
m M
m Y
=
β Y
β
≈ (η
Y )
4/3
× 10
−6 λ1
( 9 )
These are the essential constraints determining the key parameters of our model.
Then we find that m M ranges over 10 −4 to 10 −6 eV corresponding to η Y ranging
from 10 −4 to 10 −8 eV; and m Y , respectively, ranges from 1 keV to 1 GeV. Further,
we can also develop a corresponding multi-flavour dark sector so that Dark Matter
can also be accommodated as neutral atoms of this sector. The details can be found
in [11].
5 Origin of Cosmic Magnetic Fields
The origin and evolution of galactic scale magnetic fields is an open question
[18, 31]. In particular the extent of seed magnetic field as against that generated
by subsequent motion is probably experimentally distinguishable [19, 20]. In the
present case, we can estimate the field strength of the X-magnetism in each domain,
and is found to be
B dom ≈
m M
eV
2
e
e
β
0.1
3
× 2.2 × 10
−8 T
(10)