Because a charged BS may be relevant for a variety of scenarios, we detail the resulting equations. For example, cosmic strings are also constructed from a charged, complex scalar field and obeys these same equations. It is only when we choose the harmonic time dependence of the scalar field that we distinguish from the harmonic azimuth of the cosmic string . The evolution equations for the scalar field and for the Maxwell tensor areharmonic gauge condition, which casts the Einstein equations as a system of non-linear, wave equations .
Either from Noether’s theorem or by taking an additional covariant derivative of Eq. (63), one obtains that the electric current follows a conservation law. The spatial integral of the time component of this current, which can be identified with the total charge , is conserved. This charge is proportional to the number of particles, . The mass and the total charge can be calculated by associating the asymptotic behavior of the metric with that of Reissner–Nordström metric,
We look for a time independent metric by first assuming a harmonically varying scalar field as in Eq. (33). We work in spherical coordinates and assume spherical symmetry. With a proper gauge choice, the vector potential takes a particularly simple form with only a single, non-trivial component . This choice implies an everywhere vanishing magnetic field so that the electromagnetic field is purely electric. The boundary conditions for the vector potential are obtained by requiring the electric field to vanish at the origin because of regularity, . Because the electromagnetic field depends only on derivatives of the potential, we can use this freedom to set .
With these conditions, it is possible to find numerical solutions in equilibrium as described in Ref. . Solutions are found for . For the repulsive Coulomb force is bigger than the gravitational attraction and no solutions are found. This bound on the BS charge in terms of its mass ensures that one cannot construct an overcharged BS, in analogy to the overcharged monopoles of Ref. . An overcharged monopole is one with more charge than mass and is, therefore, susceptible to gravitational collapse by accreting sufficient (neutral) mass. However, because its charge is higher than its mass, such collapse might lead to an extremal Reissner–Nordström BH, but BSs do not appear to allow for this possibility. Interestingly, Ref.  finds that if one removes gravity, the obtained Q-balls may have no limit on their charge.
The mass and the number of particles are plotted as a function of for different values of in Figure 5. Trivially, for the mini-boson stars of Section (2.4) are recovered. Excited solutions with nodes are qualitatively similar . The stability of these objects has been studied in , showing that the equilibrium configurations with a mass larger than the critical mass are dynamically unstable, similar to uncharged BSs.
Recent work with charged BSs includes the publication of Maple  routines to study boson nebulae charge [63, 169, 168]
Other work generalizes the Q-balls and Q-shells found with a certain potential, which leads to the signum-Gordon equation for the scalar field [131, 132]. In particular, shell solutions can be found with a black hole in its interior, which has implications for black hole scalar hair (for a review of black hole uniqueness see ).
One can also consider Q-balls coupled to an electromagnetic field, a regime appropriate for particle physics. Within such a context, Ref.  studies the chiral magnetic effect arising from a Q-ball. Other work in Ref.  studies charged, spinning Q-balls.
Living Rev. Relativity 15, (2012), 6
This work is licensed under a Creative Commons License.