Eur. Phys. J. C (2019) 79 :693 Page 5 of 26 693
2.3.2 Kerr Black Holes
For Kerr BHs, a new phenomenon arises. The rotation of
the BH enhances the emission of particles with high angular
momentum, and with a projection m of that angular momen-
tum aligned with the BH spin, thus effectively extracting
angular momentum from the BH [42]. The equation for the
Page factor f (M, a
∗
) becomes [24,43,44]
f (M, a
∗
) ≡−M
2
dM
dt
= M
2
+∞
0
E
2π
dof
Γ
s
(E, M, a
∗
)
e
E
/T
± 1
dE, (21)
and the differential equation describing the angular momen-
tum J is [24,43,44]
3
g(M, a
∗
) ≡−
M
a
∗
dJ
dt
=−
M
a
∗
+∞
0
dof
m
2π
Γ
s
(E, M, a
∗
)
e
E
/T
± 1
dE. (22)
Once the f (M, a
∗
) and g(M, a
∗
) Page factors are obtained,
the evolution of a
∗
is straightforwardly obtained through
da
∗
dt
=
d( J/M
2
)
dt
=
1
M
2
dJ
dt
− 2
J
M
3
dM
dt
= a
∗
2 f (M, a
∗
) − g(M, a
∗
)
M
3
. (23)
The computation of the f (M, a
∗
) and g(M, a
∗
) Page fac-
tors in BlackHawk is described in Appendix B.2.
2.3.3 Exotic Black Holes
Exotic BHs listed in Sect. 2.2.3 can have a modified evolu-
tion as compared to the Schwarzschild and Kerrcases,fortwo
main reasons. First, since their greybody factors and temper-
ature are different, the f and g parameters are expected to be
different as well and the master Eq. (18) will give a different
emission rate. Second, these BHs can possess other scalar
degrees of freedom, such as a U (1) charge (e.g. the electric
charge in Reissner–Nordström BHs [25]), which experience
a specific evolution. Evolution equations for these additional
charges have to be derived, and would be similar to Eqs. (21)
and (22). The implementation of beyond-standard BHs in
BlackHawk is described in Sect. 9.5.
3
Same remark as above, we have in our conventions an opposite sign
for g.
2.4 Hadronization
The elementary particles emitted by BHs are not the final
products of the HR. Some of them are unstable, others only
exist in hadrons. A particle physics code has to be used in
order to evolve the elementary particles into final products.
We used HERWIG [45] and PYTHIA [46] for this purpose.
The final particles, hereby denoted as “secondary Hawk-
ing particles” (the elementary being the “primary Hawking
particles”), depend on the cosmological context in which they
are emitted. For Big-Bang Nucleosynthesis (BBN) studies,
an estimation of the reaction rates imposes to keep the parti-
cles with a lifetimelonger than ∼ 10
−8
s[47]. These particles
are listed in the Table 2 of Appendix C.
The time-dependent comoving density of Hawking sec-
ondary particle j emitted by a distribution of BHs per units
of time and energy is computed with the integral
d
2
n
j
dtdE
=
i
d
2
n
i
dtdE
·
dN
i
j
dE
dE
, (24)
where the sum is taken over Hawking primary particles i,
and Sect. Appendix B.3 describes how hadronization tables
dN
i
j
(E
, E) have been computed to transform the primary
spectra into secondary spectra in BlackHawk.
3 Content and compilation
This section describes the structure and file content of the
code and explains its usage. BlackHawk is written in C
and has been tested under Linux, Mac and Windows (using
Cygwin64). It can be obtained from
blackhawk.hepforge.org
3.1 Main directory
The main directory contains:
– the source codes BlackHawk_*.c containing the
main routines,
– a pre-built parameter file parameters.txt,
– a compilation file Makefile,
–aREADME.txt file containing general information
about the code,
– four folders src/, results/, manual/ and
scripts/ that are described in the following.
3.2 src/ sub-folder
This folder contains:
123