Accelerating strangelets via Penrose process in non-BPS fuzzballs

Ultra High Energy Cosmic Rays may include strangelets, a form of Strange Quark Matter, among their components. We briefly review their properties and discuss how they can be accelerated via Penrose process taking place in singular rotating Kerr black holes or in their smooth, horizonless counterparts in string theory, according to the fuzzball proposal. We focus on non-BPS solutions of the JMaRT kind and compute the efficiency of Penrose process that turns out not to be bounded unlike for Kerr BHs.

In Section 2 we will briefly review the notion of Strange Quark Matter and strangelets, discuss how Penrose mechanism can have a role in accelerating UHECRs including strangelets and SQM and sketch the alternative acceleration mechanisms proposed so far. In Section 3 we will recall the JMaRT solution and its properties. We set the stage for the analysis of the Penrose process with the study of geodesics motion in JMaRT geometry. Thanks to the large amount of isometry it proves convenient to work in the Hamiltonian formulation. We focus on the geodesics in the θ = 0 hyperplane and compute the efficiency of the Penrose process for massive spin-less particles that in-fall in a counter-rotating way. We discuss the results in comparison with the analogous process for Kerr BHs, reviewed in an Appendix. Section 4 contains our conclusions and an outlook for future investigation in this subject. In particular we will comment on upper limits that MINI-EUSO can set on the flux of strangelets and on the Penrose mechanism for their acceleration derived in Section 3 for non-BPS fuzz-balls and reviewed in the Appendix. In the Appendix, for the sake of convenience and for comparison with our analysis for non-BPS fuzzballs, we briefly review the rotating BH solution, originally found by Kerr, and its properties and discuss the Penrose process for both massive particles decaying into a massless pair (photons).

Strangelets and their acceleration via Penrose process
Neutron stars (NS) are probably the most compact and dense form of 'ordinary' matter in the Universe [18,19]. When thermo-nuclear reactions have exhausted their fuel, protons tend to recombine with electrons and form neutrons via emission of neutrinos. Matter becomes so dense that in a radius of a few km one can package masses of the order of the Sun's. In fact modelling the system as a perfect fluid with spherical symmetry Tolman, Oppenheimer and Volkoff (TOV) wrote down relativistic equations that allow determining quantitative bounds on the masses of these compact stars [18,19]. Assuming very low temperatures so much so that NS be supported only by the pressure of the degenerate Fermi gas of neutrons, one can set an upper limit on the mass of NS around the mass of the Sun. Mutatis mutandis i.e. replacing electrons with neutrons and using a 'reasonable' equation of state (EoS), relating pressure and energy density, the result is strikingly similar to Chandrasekar bound on the mass of white dwarves [20,18,13]. More recently, stimulated by the observation of candidate NS's violating the bound through direct GW detection [21], more elaborate equations of states have been proposed that amount to slice NS radially with different layers satisfying different EoS's that are glued at the interface [18,19]. In particular it has been suggested that Strange Quark Matter (SQM) [22], composed of up u, down d and strange s quarks, may play a role in internal layers, whereby temperature can raise and deconfinement can take place thus giving rise to a quark-gluon plasma. In fact the concept of a Quark Star (QS) has been put forward [23].

Strange Quark Matter and strangelets
The existence of SQM as a different state of hadronic matter other than ordinary nuclear matter was proposed for the first time in 1984 [22]. SQM would be composed by roughly an equal number of u, d and s quarks, with the presence of a third quark lowering the nucleon Fermi level with respect to a system with only two quark flavours [?]. In this case SQM may constitute the true ground state of hadronic matter and be stable. Quarks would be lumped together and not separated in nucleons, resulting in quark matter being much denser than ordinary matter. SQM could have been produced in the Big Bang [?], be present in the core of neutron stars or in "Strange Quark Stars" (SQS) [23] and be a candidate for baryonic dark matter [24]. Portions of SQM could be ejected as a consequence of collisions of these stars in binary systems [25]. Such collisions can inject a small fraction of this matter (also called strangelets) in the galactic radiation where it could be identifiable with cosmic ray detectors or mass spectrometers. Various experiments have tried to produce or search for SQM in various environments, on the ground, on balloons and in satellites, both of active and passive nature. A review on strangelet search and models can be found in [26,27]. SQM should be neutral (uncharged), if an exactly equal number of u, d, and s quarks is dynamically favoured, however the neutrality condition may be approximate, allowing strangelets to have a small residual electrical charge. In the light mass range, these objects could be identified as having an anomalous A/Z >> 2 ratio. A search with the PAMELA space-borne magnetic spectrometer has yielded upper limits 2 · 10 3 p/(m 2 sr yr) in the mass range 2 < A < 10 5 [83]. In [28] it has been suggested that heavier objects could interact with the atmosphere through an adiabatic compression mechanism similar to that of meteors. The higher density of SQM would result in longer and more uniform tracks than in case of meteorites, which tend to break up and flash during atmospheric entry. Furthermore since SQM is expected to be of interstellar origin, the speed of the track would be around 220 km/s (galactic velocity), higher than that of meteors that have an average speed of 40 km/s (solar system velocity), although interstellar meteors have also been observed [29]. Strangelets [30] may represent a fraction of UHECR. The first 'evidence' of such form of SQM could be provided by Price's event (balloon) that was initially proposed as a magnetic monopole candidate and subsequently rebutted and interpreted instead as a strangelet, having penetrated the Earth atmosphere.

Penrose process
After gravitational collapse of a NS a (rotating) black hole (BH) can form that is the only astrophysical object that could carry out a tidal tearing of a Quark Star (QS) -thus providing a source of SQM to be scattered throughout the Universe 4 . Rotating (Kerr) BHs are special in that in addition to a horizon that hides the curvature singularity they are surrounded by an 'ergo-region' external to the horizon where a time-like Killing vector becomes space-like [31]. Although curvature is finite in the ergo-region, tidal forces are much stronger than outside the ergo-sphere and a compact object captured by the rotating BH may be torn into pieces with different energies and angular momenta. As a result Penrose process can take place in Kerr BHs. This will be reviewed in the Appendix for the reader's convenience and for comparison with the case of BPS fuzz balls. According to Penrose [6] a particle with positive energy (wrt to flat infinity) can enter the ergo-region and split into two (or more) particles one of which has negative energy (as seen from infinity) and crosses the horizon to finally fall into the singularity. The rest of the products can escape back to infinity carrying out more energy than their 'mother'. The extra energy is provided by the BH that loses energy and angular momentum, since the initial particle should be counter-rotating, ie have opposite angular momentum wrt to the BH, for the very process to take place. The efficiency of the process is defined as the energy gained wrt to the initial energy As we will see momentarily, the efficiency depends on the mass, energy and spin of the initial particle as well as of the products and of the BH and the place where the splitting takes place. In the simple case when the initial counter-rotating object with energy equal to its rest mass (E 0 = µ 0 ) decomposes into two massless products at the turning point of its geodesics in the equatorial plane (θ = π/2), it is simple to express η in terms of the 'radial' position r * where the process takes place. We have reproduced the text-book analysis in the Appendix for the interested reader and for comparison with the similar process in non-BPS fuzz balls. Though almost obvious η is positive -in fact with an upper bound η ≤ (1/2)( √ 2 − 1) -only when r * lies inside the ergo-region and the particle is massive and counter-rotating. The analogue process for massless particles or waves is called super-radiance [32].

Acceleration mechanisms for UHECR
Thanks to Penrose mechanism Kerr/rotating BHs can be used as cosmic slings thus allowing one to reach the peak (GZK cutoff) of the UHECRs mountain. Sling-shot by other small magnetized objects such as white dwarves, neutron stars and quark stars has been proposed by Blandford & Znajek, Berti, Brito & Cardoso, Banados and West. Contrary to BHs the efficiency η is not bounded from above. As we will momentarily see, this will turn out to be the case for non-BPS 'fuzz-balls', too. Before concluding this section, let us briefly recall the broad features of the two classes of acceleration mechanisms for CR proposed so far. According to the first "one-shot" mechanism, CR are accelerated by an extended/intense electric field directly to the ZeV scale [33]. The original idea put forward by Swann [34] has been elaborated on and the necessary electric field is usually related to the fast rotation of small, highly magnetized objects such as white dwarfs [35,36], neutron stars (pulsars) [37,38,39,40,41], or black holes [42,43,44]. While electric field acceleration has the advantage of being fast, it suffers from the drawback of occurring in astrophysical sites with extremely high energy density, where many energy-loss phenomena can take place at the same time. According to the second "stochastic" mechanism of acceleration, instead, particles gain energy gradually through multiple interactions with moving magnetized plasmas. The idea, pioneered by Fermi [45,46], can be realised in a variety of astrophysical environments, including the interplanetary medium [47,48], supernova remnants (SNRs) [49,50,51,52,53,54], the galactic disk and halo [55,56,57,58], AGN's [59,60,61], large-scale jets and lobes of giant radio-galaxies (RG) [62,63,64], blazars [65,66,67,68], gammaray bursts (GRBs) [69,70], starburst superwinds [71,72], galactic microquasar systems [73,74], and clusters of galaxies [75,76,77]. Contrary to the previous case, stochastic acceleration tends to be slow. Furthermore it poses the issue of how to keep relativistic particles confined within the Fermi 'engine'.

Penrose mechanism for smooth non-BPS fuzzballs
In this Section, we analyze the Penrose process for neutral massive scalar particles in smooth non-BPS geometries such as JMaRT. In order to set the stage for the computation we will first recall JMaRT soliton solution and its properties and then study the geodesics motion in this geometry. Thanks to the large amount of isometry the problem is integrable very much as for Kerr BHs 5 as well as for some BPS fuzz-balls [78]. To exploit this property it is convenient to work in the Hamiltonian formulation that requires the determination of the canonical momenta P µ , conjugate to the generalised velocitiesẋ µ . We will restrict our attention on the case where the conserved KK momentum P y of the infalling particle is zero. Moreover, we focus on geodesics in the hyperplane θ = 0 whereby an effective dimensional reduction takes place since the radius of one of the angular directions (φ) shrinks to zero and one has to set the corresponding conserved (angular) momentum P φ to zero. One ends up with only three variables t, r, ψ and the dynamics looks remarkably similar to the one in Kerr BHs 6 . Despite the relatively compact and elegant form of JMaRT, explicit formulae for the 'effective potentials' E ↑↑/↑↓ ± and for the efficiency η tend to become unwieldy. We will express the results in compact form in terms of the coefficient functions that appear as components of the inverse metric. We refrain from displaying cumbersome formulae that cannot illuminate the understanding. To illustrate the results for various values of the parameters we present different plots of E ↑↑/↑↓ ± and η as well as for other relevant coefficient functions.

JMaRT solution and its properties
In string theory, the objects colloquially called black-holes (BHs) are bound states of strings and p-branes, i.e. p-dimensional extended solitons. This description allows reproducing the micro-states necessary to explain the origin of BH entropy that scales with the area of the event horizon, at least for charged BPS black-holes [9]. In the fuzzball proposal [10] classical BHs can be thought of as ensembles of smooth, horizon-less geometries with the same asymptotic behaviour as the would-be BH, i.e. same mass, charge and angular momenta. BPS systems with two charges give rise to small BHs with string-size horizon. In order to have a large BH with a finite (possibly large) area of the event horizon, one has to consider 5 We thank P. Fré for stressing this property. 6 The same happens for θ = π/2 after replacing ψ with φ and the parameters a1 and a2 with one another. systems with at least three charges in D = 5 or four charges in D = 4. One of the grand successes of string theory is the precise micro-state counting for charged BHs, mostly in a BPS context. Extension to non-BPS and un-charged BHs has proven much harder. For our purposes, as a toy model of the Penrose mechanism for non-BPS fuzz-balls, we will consider a non-BPS 3-charge solution in D = 5 originally found by Jejjalla, Madden, Ross and Titchener (JMaRT). JMaRT solutions 7 in Type IIB superstring theory depend on five parameters associated to charges: D1brane Q 1 and D5-brane Q 5 charge, the asymptotic radius R of the Kaluza-Klein circle and two additional integer parameters m and n. For m = n+1 the solutions turn out to be BPS. Imposing appropriate conditions on the parameters, that determine the mass and angular momenta, JMaRT has neither singularity nor event horizon and is free from CTC's. The reason why we are interested in JMaRT is the presence of an ergo-region, whereby particles with negative energy can propagate. It has been argued that an ergo-region that does not enclose a horizon and a singularity should lead to an instability: JMaRT should decay to an extremal BPS solution with the same charges. This ergo region or similar instabilities has been studied by various groups [16,17]. We will assume that the decay process would take a long time so much so that JMaRT could behave as a cosmic sling thanks to Penrose process, that in turn can also play a role in the relaxation of JMaRT to a stable BPS configuration. Having in mind SQM and strangelets, we focus on massive neutral scalar particles rather than on waves. The analogous process for waves is called 'super-radiance' and has been studied for JMaRT in [32]. Hawking process has also been considered for JMaRT in [79]. In order to construct JMaRT one starts fromType IIB supergravity in D = 10 and considers 3-charge micro-state geometries of the D1-D5-P system [80]. The D1-branes wrap a circle S 1 y , along which KKmomentum is added, while the D5-branes wrap a five-torus S 1 y × T 4 . The original solution depends on 8 parameters that determine the mass M ADM (related to M ), two independent angular momenta J φ and J ψ (parameterised in terms of a 1 and a 2 ), the three charges Q 1 , Q 5 and Q p (expressible in terms of the 'boost' parameters δ 1 , δ 5 and δ p ), the radius R of the S 1 y and the volume V 4 of the four-torus T 4 . Safely neglecting T 4 , whose volume can be taken to be very small, the six-dimensional geometry is parameterized in terms of t (time), r (radial coordinate), y (for S 1 y ) and three angular coordinates θ, φ and ψ and reads with c i = cosh δ i , s i = sinh δ i , for short henceforth, as well as c θ = cos θ, s θ = sin θ, c φ = cos φ, s φ = sin φ, c ψ = cos ψ, s ψ = sin ψ.
We have not displayed the profiles of the other Type IIB supergravity fields that are present in JMaRT since they play no role in our later analysis of the Penrose process. The 6-dimensional metric can be written in the form Henceforth we call it JMaRT for short. 8 Our Hi are denoted by Hi in JMaRT [14].
The ADM mass and angular momenta are given by where δ i ≥ 0, without loss of generality, and c i = cosh δ i and s i = sinh δ i , as before. Note that J φ and J ψ get exchanged under the exchange of a 1 and a 2 . Potential singularities appear when H 1 = 0 or H 5 = 0 (curvature singularities) and when det g = 0, where | det g| = r 2 H 1 H 5 cos θ 2 sin θ 2 (3.10) that is for r 2 = 0 (coordinate singularity) or for θ = 0, π or θ = π/2 (degeneration of the polar coordinates on the 'poles' of S 3 ). The vanishing of G(r) = (r 2 + a 2 1 )(r 2 + a 2 2 ) − M r 2 , the denominator of g rr , at require a detailed analysis. In order shows that r = 0 is a removable coordinate singularity it proves convenient to introduce the adimensional variable Moreover, if one could smoothly shrink a circle to zero at the origin (x = 0), the space is capped at x = 0 i.e. at r 2 = r 2 + > r 2 − and the 'true' curvature singularity at x = −1 i.e. at r 2 = r 2 − is excised. Absence of singularities, horizons and closed-time-like curves imposes conditions on the parameters that can be satisfied in the low mass (parameter) regime and fixes M and R to be given by As a result one gets Two quantization conditions (needed to have closed orbits for φ = φ + α(s i , c i )y and ψ = ψ + β(s i , c i )y as y → y + 2πR) constrain the remaining parameters in terms of two integers m and n where j = a 2 /a 1 ≤ 1 and s = s 1 s 5 s p /c 1 c 5 c p ≤ 1, indeed one can take a 1 ≥ a 2 ≥ 0 without loss of generality, thus getting m ≥ n+1 ≥ 1. In terms of j, s and a 1 the expression for M reads replacing j, s in terms of the integers m, n one finds The remaining five independent parameters correspond to Q 1 , Q 5 , R, m and n that determine the KK charge Q p and the angular momenta J φ , J ψ The Penrose process can take place in JMaRT thanks to the presence of an ergoregion, that can be identified as the region where the norm of the time-like Killing vector V t = ∂ t becomes positive. Using JMaRT one finds where f (r, θ) = r 2 +a 2 1 sin θ 2 +a 2 2 cos θ 2 and H i = f (r, θ)+M s 2 i . An ergo-sphere appears at f (r, θ) = M c 2 where V t becomes space-like. In the BPS limit the norm of V t is always negative: ||V t || 2 = −f / √ H 1 H 5 and no ergo-region appears.

Geodetic motion in JMaRT
As a preliminary step to investigate the Penrose process in JMaRT, we study the geodesics for massive or massless neutral particles. Probes of this kind only feel the presence of the curved metric but are unaffected by the other Type IIB fields present in JMaRT. The Lagrangian that governs geodetic motion is given by where g µν denotes the six-dimensional metric tensor 9 . Recall that dr and dθ appear diagonally in ds 2 , while dt, dy, dφ, dψ form a four-dimensional block. As in Kerr BH or in BPS fuzz balls, in order to take advantage of all the symmetries, i.e. time translation, KK shifts U (1) y and rotations U (1) φ × U (1) ψ , it is better to switch to the Hamiltonian formalism. The generalized momenta are given by whereẋ ν = dx µ /dτ and the Hamiltonian reads where g µν is the inverse six-dimensional metric. For JMaRT the explicit expressions for the generalized momenta read P r =ṙ r 2 √ H 1 H 5 (a 1 2 + r 2 ) (a 2 2 + r 2 ) − M r 2 (3.25) 9 The extra four directions compactified on T 4 play no role in our analysis.
and the Hamiltonian for JMaRT can be written as where the coefficient functions A, B, U , C φ , C ψ , F , Ω φ , Ω ψ , Γ, K, Λ φ , Λ ψ are the non-zero components of the inverse metric g µν , whose explicit expressions are quite cumbersome and will not be displayed, except for the special case of θ = 0. The generalized velocities can be expressed in terms of the momenta using the above functionṡ t = −P t A + P y K + P ψ Ω ψ + P φ Ω φ (3.32) Very much as for Kerr BH and for BPS fuzz-balls, the system is integrable in that the dynamics in the r and θ coordinates can be separated in principle. In practice the geodesics are non-planar and their explicit form is not very illuminating for our purposes. Following similar analysis in BPS fuzz-balls [78] and without losing any significant feature of the result, one can focus on the hyper-planes θ = 0 and θ = π/2. Indeed it is consistent to setθ = 0 and P θ = 0 in these two cases since dP θ dτ = − ∂H ∂θ = 0 for θ = 0 and θ = π/2 (3.38) For both choices an effective dimensional reduction takes place. For θ = 0 all terms in dφ drop, being proportional to sin θ 2 , and one can safely set P φ = 0; while for θ = π/2 all terms in dψ drop, being proportional to cos θ 2 , and one can safely set P ψ = 0. The two cases are perfectly equivalent and one can get one from the other by simply exchanging a 1 and a 2 in any relevant formula. For definiteness we will focus on the θ = 0 hyperplane in the following.
Moreover, we are not interested in the motion along the compact y direction. In order to simplify the analysis, one can set P y = 0. This is consistent since P y = 0 is conserved:Ṗ y = 0. As a consequenceẏ is completely determined by the other velocities and conserved momenta, so much so that we will not consider it later on. If we fix θ = 0 and consequently P θ = 0, all the terms in dφ drop and the metric becomes which takes the form Recall that a 1 and a 2 switch their role under a change of θ from 0 to π/2 and an exchange ψ ↔ φ. The reduced Hamiltonian expressed in terms of the components of the reduced inverse metric reads where µ is the mass of the probe and the coefficient functions A, B, C ψ , F , Ω ψ , K, Λ ψ are the non-zero components of the reduced inverse metric and µ is the rest mass of the probe spin-less particle. At θ = 0 one has Since we are not interested in motion along the compact circle direction we can safely set P y = 0 (3.57) and, for convenience of the notation, so that we get where the 'effective potentials' read Since A/ B ≥ 0 always, one has either E > E + > E − or E < E − < E + where, depending on whether the particle is co-rotating (↑↑), ie J J ψ > 0, or counter-rotating (↑↓), ie J J ψ < 0, one has for r ≤ r e , E ↑↓ − ≤ −µ As we will see momentarily, the Penrose process can only take place in the latter case. In Figs. 1, 2, 3 we have plotted E ↑↓ ± as a function of r for some 'reasonable' choice of the parameters M, a 1 , a 2 of JMaRT (determined by the choice of m, n, δ 1 , δ 5 and a 1 or, equivalently, R) and of the angular momentum J of the (massive µ = 0 or mass-less µ = 0) probe particle. Despite their complexity, thanks to the existence of a frame-dragging term dtdψ in Eq. 4, these solutions expose the expected presence of regions with negative energy inside the ergo-sphere that can be studied computationally and plotted. For comparison we also plot E ↑↑ ± in Fig. 4. As evident from the plots of E ± there are two kinds of geodesics in the θ = 0 plane: unbounded ones for E ≥ µ and trapped ones E ≤ −µ. In the former case the massive probe impinges from infinity, reaches a turning point r * where P r = 0 and gets deflected back to infinity, possibly after making several turns around the 'center' (x = 0 ie r 2 = r 2 + < 0) of the fuzzball. In the latter case, the particle cannot escape to infinity and remains forever inside the fuzzball. The relevant equations can be integrated in terms of non-elementary functions and we will not attempt to present a detailed analysis here. Instead we turn our attention on the Penrose process in JMaRT.

Penrose process in JMaRT and its efficiency
The presence of an ergo-region in JMaRT allows the Penrose process to take place, whereby a counterrotating particle acquires negative energy after crossing the ergo-sphere and if it splits into two or more fragments, one of the product may escape to infinity with an energy larger than the initial particle, while the other fragment(s) get trapped in the fuzzball for a 'long' time. Following [20,13], mutatis mutandis we will derive the efficiency of Penrose process in JMaRT metric. Let us consider a spin-less probe with rest mass µ 0 , energy E 0 ≥ µ 0 (positive branch) and orbital angular momentum J 0 opposite to the angular momentum of JMaRT (counter-rotating ↑↓). Very much as in Penrose original analysis, it seems reasonable and computationally convenient to assume that the probe splits exactly at the turning point r = r * where P r (r * ) = 0. At this point the angular velocity reaches a maximum and the tidal tearing of the probe is more likely to take place. This has the additional advantage of simplifying the analysis since one gets a relation between r, E 0 and J 0 of the form which can be (implicitly) solved for r = r * as a function of E 0 (positive counter-rotating branch) and J 0 .    Denoting by E 1 , E 2 and J 1 , J 2 the energies and (orbital) angular momenta of the two (spin-less) fragments with rest masses µ 1 and µ 2 , conservation of energy and angular momentum yield which has two solutions, symmetric under the exchange 1 ↔ 2. Assuming that particle 1 escapes to infinity (positive branch of the energy) while particle 2 gets trapped in the fuzzball (negative branch of the energy), one can first express J 1 and J 2 in terms of E 1 = E + (µ 1 ) and E 2 = E − (µ 2 ) and get 10 Plugging these in the second equation and solving the system for E 1,2 yields Note the role of the "fake square" that is ubiquitous in 3-body phase space. Note that F(µ 0 2 , µ 1 2 , µ 2 2 ) ≥ 0 for µ 0 ≥ µ 1 + µ 2 as required by standard kinematics considerations. In the symmetric case Note also that A > 0 and Ω ψ > 0 while C ψ > 0 for r > r e and C ψ < 0 for r < r e . The efficiency η of Penrose process for JMaRT is given by the energy E 1 − E 0 gained by the 'probe' particle escaping to infinity with respect to energy of the incoming particle E 0 . As a function of the radial decay point, that we have identified with the radial turning point r * , implicitly determined by the choice of E 0 and J 0 , viz.
The efficiency is negative when r * > r e as evident from the plot in Fig. 5. For some choice of the parameters, η is larger than one (Figs. 6, 7). In general, contrary to what happens for rotating BHs, reviewed in the Appendix, there is no upper bound on η. This looks particularly promising for the acceleration of UHECR, including strangelets, by non-BPS rotating fuzz-balls that should replace putative rotating BHs of the kind found by Kerr. The case of JMaRT should be taken as a toy model in many respects. First of all the relevant dynamics is at least five-dimensional. Second, though non-BPS, the charges play a crucial role in the very existence of the solution that should be thought of as some excited state of a BPS configuration. Last but not least, achieving phenomenologically reasonable values for the mass and angular momenta require extrapolation to very large charges that may look rather unnatural. We have shown that the Penrose process can take place not only in singular rotating (Kerr) BHs but also in smooth horizonless geometries that are expected to represent the micro-states of (charged) rotating BHs. The common and crucial feature being the presence of an ergoregion. We have considered the case of JMaRT, which is in a loose sense a non-BPS fuzzball in D = 5. Actually it is over-rotating wrt to classical BHs with the same mass and charges so it is only a gravitational soliton. Anyway, we took it as a toy model for our analysis and computed the efficiency η of a non-collisional Penrose process in rotating geometries of this kind. Contrary to the case of Kerr BHs, reviewed in the Appendix, η is not bounded from above and depends in a highly non-trivial fashion of the parameters of the fuzz-ball as well as on the masses of the probe and of the fragments and above all on the 'radial' position where the decay occurs. As expected the efficiency is positive only if the in-falling particle is counter-rotating and the splitting happens inside the ergo-region. In order to make quantitative predictions on the relevance of such a mechanism for the acceleration of UHECR and in particular strangelets one should estimate the distribution of such or similar objects in our galaxy / universe as well as of rotating fuzz-balls with large enough mass and angular momentum to be useful as cosmic slings thus allowing one to reach the GZK cutoff energy of the UHECRs. Sling-shot by other small magnetized objects such as white dwarves, neutron stars (and quark stars) has been proposed by Blandford & Znajek, Berti, Brito & Cardoso, Banados and West. We plan to address these and related issues in the near future [81]. For the time being, we would like to comment on upper limits that MINI-EUSO can set on the flux of strangelets and on the Penrose mechanism for their acceleration derived in Section 3 for non-BPS fuzz-balls and reviewed in the Appendix for Kerr BH.  MINI-EUSO is an instrument to be placed inside the International Space Station (ISS), looking toward the Earth from a nadir-facing window in the Russian Zvezda module [84]. The main telescope employs a Fresnel optics with a Multi-Anode-photomultiplier (MAPMT) focal surface (48 × 48 pixels), with ancillary cameras in the Near-Infrared and Visible regions. Mini-EUSO will map the earth in the UV range (300-400 nm) with a spatial resolution of 6.11 km and a temporal resolution of 2.5 µs, searching for Ultra-High Energy Cosmic rays E > 5 · 10 20 eV and studying a variety of atmospheric events such as transient luminous events (TLEs), bioluminescence and meteors. The spatial and temporal sampling of the detector allows searching for strange quark matter tracks in the atmosphere, discriminating them from meteors from the light curve (intensity and speed). An estimation of the upper limit of flux which can be posed by one month of night observations of MINI-EUSO is about 10 −21 cm −2 s −1 sr −1 in the mass range above 5 · 10 24 GeV/c 2 [82]. that means 11 r e (θ) = M + M 2 − a 2 cos 2 θ (4.6) The ergo-sphere lies outside the horizon except at the poles, θ = 0, π, where they touch each other. In the ergo-region, inside the ergo-sphere, all particles, including photons, must rotate with the hole since g tt > 0. The presence of the ergo-region allows Penrose process to take place as we will see momentarily.
Focussing for simplicity on geodesics in the equatorial plane θ = π/2 allows to write the restricted metric in the compact form ds 2 = −A dt 2 + C dφ 2 + 2Ω dtdφ + B dr 2 (4.7) where , C = r 2 + a 2 + 2M r a 2 , Ω = − 2M a r (4.8) Computing the conjugate momenta P µ = g µνẋ ν and setting 12 P t = −E , P φ = J , P r = P (4.9) one finds where µ is the mass of the probe particle. The geodesic is null for µ = 0. Resolving for the radial momentum P in terms of E and J one finds where the 'effective potentials' read E ± = −ΩJ ± (Ω 2 + AC)(J 2 − Cµ 2 ) C (4.12) Since BC/AC + Ω 2 ≥ 0 outside the horizon either E ≥ E + > E − or E ≤ E − < E + . E ± determine allowed negative-energy regions. For co-rotating particles (J a ≥ 0) E ↑↑ + is always positive, while while for counter-rotating particles (J a ≤ 0) E ↑↓ + becomes negative inside the ergo-sphere (r e = 2M ). As mentioned above, if a positive energy counter-rotating particle enters the ergo-sphere it acquires negative energy and 'decays' into two or more products, one of which has negative energy and falls into the horizon, then the particle that escapes may have more energy than the initial particle. In this way Kerr BH loses mass angular momentum. Following [20,13], we now review the efficiency of the Penrose process in Kerr BH. For simplicity we will assume that the in-falling massive particle has E = µ ('rest mass'), that the products are massless scalars (no spin) µ 1 = µ 2 = 0 and that the decay takes place at the turning point r = r * (with r H < r * < r e = 2M ) where P r = 0. Since energy and angular momentum are conserved, we have For massless particles J i = αE i , while J = βE for the massive one with α and β depending on the turning point r * where the decay/splitting takes place. The second equation then simplifies drastically to α 1 E 1 + α 2 E 2 = βE (4.14) Solving the 'linear' system one has Taking the positive branch for E = E + and E 1 = E 1,+ and the negative branch for E 2 = E 2,− < 0, one gets E 1 > E The efficiency of the process can be estimated in the following way. Since ∆E = E 1 − E = −E 2 is the gained energy, the efficiency of Penrose process as a function of r * is given by since r H ≤ r * ≤ 2M = r e (θ = π/2) for the very process to take place. In fact the maximum is reached when r * = r H = M + √ M 2 − a 2 and a = M (extremal Kerr BH).