PoS(EDSU2018)046 . As 2 M http://pos.sissa.it/ and can be as short as M ∗† [email protected] Speaker. The work presented is the fruit of collaborations, in particular with Aurelien Barrau, Alvise Raccanelli, and Carlo smaller black holes explode earlier, theI resulting discuss signal the have different a emission peculiar channels fluence-distance thatradio, can relation. be TeV) expected and from their the detection explosion (sub-millimetre, challenges.served wavelength In that particular, scales one with of thefunction, redshift these leaving following channels a a produces signature unique an also flattened in ob- wavelength-distance theinsights resulting on diffuse the emission. cosmological constraints, I concerning conclude bothremnant presenting the phase. the explosive first phase and the subsequent A recent understanding on how quantumnarios effects for may dark affect matter, black-hole in evolution connection opensQuantum with new fluctuations sce- the of presence the of geometry black allownelling. holes for in This black the process holes very yields to early to decay universe. aninformation into paradox. explosion white and Primordial holes possibly black via to holes a a undergoingof tun- this long decaying evolution remnant dark constitute phase, matter, a that whose peculiar cures lifetime kind the depends on their mass † ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 2nd World Summit: Exploring the Dark25-29 Side June, of 2018 the - Universe EDSU2018 University of Antilles, Pointe-à-Pitre, Guadeloupe, France Rovelli. The research ofgrant FV FIS2017-85076-P at (MINECO/AEI/FEDER, UPV/EHU UE). is supported by the grant IT956-16 of the Basque Government and by the University of the Basque Country UPV/EHU,Barrio Departamento Sarriena de s/n, Física 48940 Teórica, Leioa, Biscay,E-mail: Spain Francesca Vidotto Quantum insights on Primordial Black Holes as Dark Matter PoS(EDSU2018)046 Francesca Vidotto . This implies that 3 BH M Kg could have evaporated, ]. The search for PBHs and 12 ? , ? , ? ]: as cosmic rays of such energies are rare, ? , when the effects of the Hawking evaporation 3 BH M 1 ]. The geometry around a black hole can indeed undergo ? ]. As soon as these quantum fluctuations of the geometry take place, the ? : this is the minimal time after which quantum fluctuations of the metric can , ? [ 2 BH M 2 BH M ]. An extended mass function is compatible with different PBH formation mechanics, ] and since then observational consequences and constraints have being considered for ? ? near the hole horizon allows to define the ‘quantum break-time’ as the inverse of this 2 − BH , as short as Hawking evaporation, however, is a phenomenon predicted in the context of quantum field Hawking evaporation is a phenomenon that becomes relevant on a time scale that depends on Dark matter is maybe the most puzzling open problem, brought to physicists by mounting Since the detection by the LIGO interferometer of black holes in an unexpected mass range, A monochromatic mass spectrum has been challenged by different authors as restrictive and M 3 BH theory on a fixedto curved break background. down when This approximatelyinstance by half is the of ‘firewall’ a no-go the theorem theory mass [ with of a the hole regime has of evaporated, validity as that indicated is for likely dynamics of the horizon canof undergo the dramatic horizon, behaviours, possibly to by the an point explosion. of the very disappearance constraints are derived on the very-small-mass end of the PBH mass spectrum. quantum fluctuations on a time scale shorter than have not not yet significantly modifiedcharacteristic the timescale size after which of the the the hole. departureas from As the quantum any classical classical evolution effects become system, manifest. important theM hole This has time a can beappear much in shorter the region than outside the the hole Hawkingto horizon. evaporation In time fact, the presence of a small curvature proportional quantity, i.e. within the age of theand universe possibly only produced PBHs very with high-energy mass cosmic smaller rays than [ 10 the mass of the black hole. In Planck units, the evaporation time scale is different PBH mass ranges exploiting different observables [ from critical collapse to cosmicone strings. (like the An ones extended detected mass bypossibility LIGO function, to and encompassing saturate above) very DM and massive with sub-solar ones PBHs. as well, makes more viable the observational evidences in astronomy.theoretical landscape, While on for the long experimentalexperiments side, the to where idea space the telescopes, of search no new effort evidencetion spanned for particles encourages from dark us dominated matter accelerator to the particles explore hasof solutions manifested. new that particles. This involve gravitational situa- physics rather than the presence Primordial Black Holes (PBHs) haveincreasing. experienced a According renovated to interest, aera, that and variety seems they so of are far a scenarios, possible steadily not PBHs candidate subject for are to dark produced big-bang matter in (DM). nucleosynthesis PBHsas constraints the are non-baryonic on radiation-dominated constituted dark baryons, by therefore matter matter they (DM). thatSeventies behave The is [ to idea all that effect PBHs could contribute to DM dates back to the unrealistic [ Quantum insights on Primordial Black Holes as Dark Matter 1. Primordial Black Holes for constraints on PBHs haspresence mostly of considered Hawking an evaporation almost for monochromatic PBHs mass of spectrum, small mass. and the PoS(EDSU2018)046 we and ?? 2 BH M Francesca Vidotto . Notice that the . Then we can write , i.e. a white hole. 3 BH M bounce and ] via a quantum region. This is 2 BH is the one most probable. As the ? M 2 BH M anti-trapping surface . The collapse continues beyond this surface 2 ]. ? trapping surface ]. At this point the appearance of an effective quantum pressure ? [ ], so far only Loop Quantum Gravity provides sufficiently-defined tools ? , ? Planck Star discreteness, that modifies both the kinematics and the dynamics of the theory. The ]. Quantum discreteness plays a fundamental role: this is not just a space discreteness, but ? . Standard decay physics suggests that the shortest value For the sake of the phenomenology, it is possible to study the BH decay considering a parametri- The classical curvature singularity at the center of BHs is cured in the quantum theory by non- Notice that two time-scales should be distinguished. One is associated with the proper time On the other hand, primordial black holes are small and old enough to have an observable A non-singular black hole forms as usual in the collapse of some matter and it is associated , ? 3 , BH spacetime ? sation that spans the whole window of allowed lifetimes between to compute explicitly this lifetime [ perturbative effects. In Loop Quantum Gravity[ singularity resolution has been studied extensively of the collapsing matter thattrough forms the the BH: dynamical seen horizon fromConsider and the the then center case expands of of trough the BHsby hole, the formed photons: the in horizon the matter the (now bounce collapses early a will universe thento white-hole when happen cross this horizon). at the matter the region was speed inside basically of theA constituted light, horizon different and (this time last is roughly scale of the is thelong time associated order light due of to takes to micoseconds an for the observer a hugeholes situated BH in (but outside of the finite) the solar sky mass). horizon: redshift. and they this behave This for is is us extremely as the stable reason objects! decay why for we observers do situated see outside astrophysical of black the horizon as we are. From the discussion in Sec. Quantum insights on Primordial Black Holes as Dark Matter 2. Quantum Gravity bounce connects two classical solution ofthe the definition Einstein of equations a [ quantum tunnelling,analogy a with characteristic nuclear non-perturbative physics, quantum phenomenon. wediscuss In the can hole then lifetime, refer that to characterises the the time-scale black-to-white of tunnelling the process. as a decay, and conclude that the black-holeM lifetime should last, indecay is natural a units, fully non-perturbative for process, a ato non-perturbative compute quantum time theory the of between hole gravity lifetime. is This necessary different computation quantum-gravity provides approaches. a While possible instabilities terrain leading toin to discriminate different a approaches between black-hole [ decay are present a with the accompanied byrespect the to other formation model of of non-singular a blackthe horizon. holes, other because hand, the This collapse this do scenario is producesit is a not can horizon. an rather On be event conservative fully horizon with but characterised a as dynamical a horizon with a finite lifetime, hence quantum equations of motions can beintuition translated into of effective how equations, that quantum provideforce effects a compelling appears concretely when affects the black energylapse. hole density Instead evolution: of approaches the an Planckian singularity, the values, effective repulsive repulsive preventing force any triggers a further new col- expanding phase. and reaches a maximal contraction:suggestive this name phase of of the collapsestarts is the referred expansion in the and literature the with consequent the creation of an The passage from a contacting solution to an expanding one is called a PoS(EDSU2018)046 ) ]. ? ) a ?? [ (2.1) ?? ) that ?? Francesca Vidotto Kg for the shorter 23 in the CMB from the energy ]. These measurements acquire ? , ? , Pl t 2  superseding the constraint on PBHs as DM Pl BH m 3 M  κ 4 = . τ as: κ relaxes the constraints from microlensing of object smaller than ; to understand further the cosmological implication of the BH affects the galaxy number count in large-scale galaxy surveys, in par- ]. As we are interested in how these data may evolve with redshift while ? Lacking of a detailed astrophysical model for the BH explosion, emission with a parameter are the Planck time and the Planck mass. τ pl Kg: those of smaller mass have had already evaporated. In the case of a quantum- m . Remarkably, this ]. ? 12 [ 2 BH and M is shorter than the evaporation time, the effects of such a quantum-gravity phenomenon pl t τ Astrophysical signals produced in the explosive event associated to the BH decay could be The scenario leads to a threshold in the minimal mass of PBHs present today. In the case of PBH decay has the peculiar property of lowering the DM energy-density content of the Uni- This scenario leads to a number of consequences with observational significance, listed below. If PBHs form a component of DM, this would be DM decaying with a mass-dependent decay Effects of the quantum-gravitational BH decay could be identified • • • • • a signal determined byin the presence temperature of of magnetic the fields photons can emitted produce (high-energy a channel), signal ( in the radio (Rees’ mechanism), and ( signal determined by the size of the hole exploding (low-energy channel). and (iv) the emission in channels can be studied on the basis of heuristic arguments. Two channels can be expected: ( detectable directly. injection by the PBHdecay explosion future research should aim atcombining investigating these different effects and observables, developing a taking constraintfunction. into analysis account the possibility of an extended PBH mass obtained from the Hawking evaporation Hawking evaporation, a minimal mass was setequal by to the fact 10 that PBHs evaporatinggravitational today have decay, a the mass mass of those exploding today can be as high as 10 time –a peculiar feature as other decayingtime DM candidates have a fixed decay time. As the decaying where 3. Phenomenology dominate over Hawking evaporation; this leads to lifetime such mass verse as the decay convertsUniverse effectively though DM ages. into This radiation, modifyingticular measuring the the equation galaxy of clustering, state galaxyThe lensing of LSS and the surveys Redshift-Space by Distortions SKA (RSD) the will provide radio key continuum data [ inthe this SKA respect survey by do detecting not individual measuredivision galaxies directly of the in the redshift, galaxy we catalog can into applyparticular tomographic different interest techniques redshift if such bins as PBHs [ the willlifetime-mass be scaling detected would using be different constrained observables:measure from then a this quantum-gravity the phenomenon type quantum-gravity from of late-universe analyses, data. opening the possibility to Quantum insights on Primordial Black Holes as Dark Matter the BH lifetime PoS(EDSU2018)046 , the TeV Francesca Vidotto ]. Observing signals ? 4 ]. ? ] for the analysis of the signal detectability. ? ] that allowed to circumvent the problem and make most of the ? channel is constituted by the matter, primarily photons, re-emitted with the high energy ], during the reheating over-dense region can collapse forming PBHs with different sizes . The mechanism relies on the production during the explosion of a shell of relativistic ? A further question is the possible gravitational-wave production via the black-to-white bounce: The The study of high-energy cosmic emissions from PBH explosions was initiated in the Seventies Interestingly, the scenario discussed in this paper gives a crucial difference with respect to the GHz 1 PBH explosions in theionised visible interstellar medium, universe exploding virtually PBHs accessible.∼ can produce a He secondary noticed radiocharged pulse that, particles: of in the the shell order presence behaves of from of as a a a spherical superconductor volume that centred expels inradio the the signal interstellar was original magnetic investigated BH in field sites. details in The [ structure of the resulting secondary we omit this here,interesting even and deserve if further in investigations. the era of multimessanger3.1 astronomy this High Energy question Channel is particularly same temperature it had atmodel the [ time of the collapse that formed the PBH. In the original collapse and the problem detecting sourcesRees at proposed a a cosmological mechanism distance [ was immediately realised. Martin old models of PBH. In fact,to PBH emit explosions at a the high end energyPlanckian. of burst, the This Hawking was where evaporation the the were case expected total forbursts all mass were exploding therefore of PBHs, expected the independently to object fromaspect have their converted that all original into made the mass. more the same The difficult burst fluence, thecharacteristic was and detection. feature. just the fluence On The to the other be lifetimecan hand, very of be our small the expected scenario - presents blackhole before an aorder is the different of a Page magnitude function time, of of whensive, when its the and it mass black they formed. and producing holes a the has primaryRees’ PBHs explosion conserved emission mechanism observed a of is exploding lower mass very far fluence efficient ofemission, away than in the almost those are transforming preserving same at those the the a original less primary closer fluence, emissioninformation mas- distance. therefore about into the The the fluence the original of secondary mass the of radio radiorelation the burst for PBH carries the source. the radio Therefore signal a can characteristicmeasured fluence-distance single at out cosmological PBH distance. decays with respect to other astrophysical sources Quantum insights on Primordial Black Holes as Dark Matter gravitational waves. The main parameter thatthe determines BH the mass. specific We will features now of examine all these these channels signal separately. is determined by the Hubble horizon.energy As of the the temperature photons in at the reheating highbecame is energy available of channel in the is the expected forthcoming order in years of this toin the range. observe this in New this instruments channel energy should is window [ limitedrays by interact a with significative the observationalwithin CMB, horizon: our allowing galactic at the neighbourhood. such See signal a [ to high travel energy, cosmic to usRees’ only Mechanism when and Fast the Radio source Bursts is located PoS(EDSU2018)046 ], whose ) we can ? ?? Francesca Vidotto , but a study of the GeV for a standard astrophysical z ]. Some Short Gamma Ray Bursts [ ? [ 5 MeV , the peak of the signal in the millimetres. The corresponding , the signal is emitted with energy in the κ κ . The curve flattens at large distance: the shorter wavelength from smaller black z ], a fact that future radio surveys with higher sensitivity can help to clarify ]. Recent studies seems to indicate that FRBs follow a non-standard fluence- channel is more promising in terms of detectability. This emission channel ? ? , ? and the observational dept allows to detect events in all the visible universe. mm 2 . In blue, the dependence of the observed wavelength from the redshift low energy ∼ ]. ? Fast Radio Bursts (FRB) have been discovered a decade ago and their origin is today still For the highest values of For the lowest values of The , BH ? R ]. Finally, the FRB signal, is polarised, hinting to the presence of a magnetic field at the source ? ? Figure 1: object. In red, thefunction expected of wavelength the (unspecified redshift units) of the signal from black hole explosions as a holes exploding earlier get compensated by the redshift. photon emission with the codemore PHYTIA likely indicates to that be the detected, photons are with those higher in density, the therefore frequencies are beyond the sensitivityhand, of in most a decay radio we telescopes,be expect such some a as event probability happening SKA-mid. distribution within of SKA-mid On themechanism frequency the event are range. to other not happen, Furthermore, fully therefore the established, there details leaving of could open the the decay possibility of the presence of some factors an open question.as BH FRB exploding source. via a FRBsmodel black-to-white presents presented transition a here. number constitutes They of aTheir are singular magnitude natural extremely features of candidate energetic their that impulsive enormous canmass events, fluence be into can at radiation easily be cosmological [ explained matched distance. by by the the conversion of the whole PBH Quantum insights on Primordial Black Holes as Dark Matter distance relation [ [ [ indeed compute the mass oftoday. black For holes a whose lifetime lifetime in the is lowerof the end Hubble of the time, viable yielding window, the an Schwarzschild explosion radius is of the order source is still unclear, are possible candidates in this range. 3.2 Low energy channel should be present if thethe explosion excites Schwarzschild a radius. mode correspondent This to depends the BH on size, the given actual roughly value by of the lifetime. Using ( PoS(EDSU2018)046 direct decayed ]. A number of direct+decayed enlarged ? Francesca Vidotto parameter. The spectrum was κ k=0.05 ). Observation of burst whose source has a ?? 6 ]. The units in the ordinate axis are not specified: the normalisation of the ? in [ κ ] represented by the flattened curve (Fig. The diffuse emission of the low energy channel, and below the diffuse emission of the high energy ? An exact localisation of burst sources could be proven difficult. This involve the dispersion The peculiar wavelength-redshift relation can be proven also without the knowledge of the PBH exploding in a quantum decay present a unique feature that makes them distinguishable Generic astrophysical objects have an observed wavelength that scale linearly with the dis- Figure 2: channel. We show here the onesstudied for for the the shortest full BH range lifetime, of i.e. the lowest spectrum depends on the percentage of PBHs as DM. measure of the receivedobject, signal, for instance and a possibly galaxy. A theBH further source exploding technique is far being available, away hosted and aremeasured it in burst is less lessen a peculiar massive, with of known with a decaying astronomical distance. PBHs. a lower flux ofIntensity energy: mapping the flux of energy of the distance of the source, by studying the radiation integrated over the detectable past explosions. The known distance will allow to seequantum-gravitational whether nature data of fit the such process a at curve. the If origin. so, it would be a signature of the from other astrophysical sources.mass. The Therefore, time smaller at PBH which explodealso earlier, the depends i.e. decay on at happens their a mass: is distancelow the a from energy smaller channels. us. function black Signal of The holes, from signal the distant the theywavelength sources BH shorter due produce get wavelength to redshifted, in a partially the smaller compensating the high mass. shorter and in the tance. On the otherinitial mass, hand, reach Hawking the evaporation Planckdescribed ends size above in and gives a the produce completely a standard different signalredshift effect: theory with the [ when modified such BHs, relation wavelength. between of wavelength The and any phenomenon Quantum insights on Primordial Black Holes as Dark Matter that could shift the wavelength possiblyfor of transients 1-2 orders the of highest magnitude. frequenciesthat This accessible the makes to worthy quantum-gravitational SKA-mid. to Bh explore explosion In mayhints particular, be seems it linked to has to support been Fast this suggested Radioenormous Bursts conjecture, energy [ such flux as the the rapid BH impulse, converts efficiently a its mostly mass extra-galactic intoSignature origin, radiation. of the PBH decay PoS(EDSU2018)046 ]. ? , where 4 BH M . ∼ ]. The second Francesca Vidotto ? ] for a large range ? . (1975), no. 5489, ]. The latter scenario is ? 253 . 1604.05349 Nature 1609.01143 1608.02174 (2016), no. 4, 44029, 7 D94 (2016), no. 6, 63530, . (2016), no. 12, 44, D94 ]. Kg Phys. Rev. ? 9 1612 − 10 ∼ JCAP Phys. Rev. . This appears for both the high energy and the low energy channel, as can be ?? for the case of the shortest lifetime. In principle the result depends on the PBH mass ]. ? ?? , ? parameter in the PBH lifetime. The signal has been obtained using the PYTHIA code ], and one where PBHs are formed in a bouncing cosmology [ κ ? is the original mass of the black hole rather than the final remnant mass [ extended mass function,” Galactic gamma-ray background,” matter from Planck data,” 251–252. Quantum gravity provides a concrete mechanism to describe the final stage of the life of the Two observations support the idea that these remnants are stable on timescales much longer The viability of these remnants as a light dark matter component has been proposed in [ ], that for a given initial energy computes the particle production for the process. The resulting BH [4] A. M. Green, “Microlensing and dynamical constraints on primordial black hole dark matter with an [3] L. Chen, Q.-G. Huang, and K. Wang, “Constraint on the abundance of primordial black holes in dark [2] B. J. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, “Constraints on primordial black holes from the [1] G. F. Chapline, “Cosmological effects of primordial black holes,” ? References M Two possible scenario are currentlytime investigated: [ one in which PBHsparticularly are intriguing formed because at the BHphase reheating can of act a bouncing as universe, a givinginflation an [ dust almost component scale-invariant power that spectrum even dominates in the absence of contracting black hole, that doesabove. not In fact, finish the at black-to-white transition thea allows residual end for small a of Planck new mass remnant the phase, evaporation characterised nor by with with thethan explosion the age described of thea universe. black The hole first forms, observation it iswhite has based decays a are on large dramatic classical internal events that General volume. changes Relativity.“reabsorption” Hawking the of size When evaporation the of or the large macroscopic horizon internal black-to- surface; volume on can the only other happens hand, on the a longer timescale 4. PBH remnants and dark matter Quantum insights on Primordial Black Holes as Dark Matter instruments performing intensity mapping campainsrespect. can The therefore study provide the the integrated desired emissionof from data PBH in the decay this has been started in[ [ radiation is not thermal,relation but of it Fig. carries aseen in distortion Fig. due tospectrum, the but characteristic different hypothesis redshift-wavelength forhave the only mass a spectrum very have weak been dependence tested [ showing that the result observation uses a basicdiscrete prediction spectrum of for geometrical Loop quantities. Quantum Inreveal particular, Gravity. the at presence the Spacetime Planck of scale a quantization an minimal yields area non-zero measurement a eigenvalue. PoS(EDSU2018)046 . 21 8 (1993) 70 Class. Quant. . Astropart. 1401.6562 . Class. Quant. Francesca Vidotto Int. J. Mod. Phys. D Class. Quant. Grav. (aug, 1974) 399–416. 1407.0989 . Phys. Rev. Lett. Front. Phys.(Beijing) 1303.4722 168 . (2015) 18. (2013), no. 18, 181302. (jan, 2014) 1442026, mnras 23 111 \ 1606.07434 AASKA14 1605.05268 (jul, 2014) 104020, PoS 92 . . . 8 . Phys. Rev. Lett. (2017) 3650, . Int. J. Mod. Phys. D 468 . . Phys. Rev. D . 1307.3228 . . (1977) 333. 1507.05424 1506.08015 266 1705.05567 0509075 astro-ph/9907347 1607.00364 (2017). Nature 1207.3123 gr-qc/0407058 hep-th/9301052 to Appear Mon. Not. Roy. Astron. Soc. (2013) 62, (2016), no. 5, 55006, (2006) 391–411, (2000) 269–275, 02 33 23 12 (oct, 2016) 1644021, Phys. (2004) 4793–4804, (2013), no. 6, 714–747. quantum gravity: a closer look,” Quantum Gravity: the Planck-Star Tunnelling-Time,” Redshifts,” “Cosmology with SKA Radio Continuum Surveys,” Grav. JHEP Covariant Loop Quantum Gravity,” analysis of Kepler source microlensing data,” clustering,” “Clustering-based redshift estimation: method and application to data,” spark black to white hole tunneling,” 25 Grav. extended mass functions,” 2837–2840, [7] A. Almheiri, D. Marolf, J. Polchinski, and J. Sully, “Black Holes: Complementarity or Firewalls?,” [6] A. Barrau, “Primordial black holes as a source of extremely high-energy cosmic rays,” [8] H. M. Haggard and C. Rovelli, “Black hole fireworks: quantum-gravity effects outside[9] the horizon H. M. Haggard and C. Rovelli, “Quantum gravity effects around Sagittarius A*,” [5] B. Carr, M. Raidal, T. Tenkanen, V. Vaskonen, and H. Veermäe, “Primordial black hole constraints for [25] M. Rees, “No Title,” [24] A. Barrau, B. Bolliet, F. Vidotto, and C. Weimer, “Phenomenology of bouncing black holes in [16] M. Christodoulou, C. Rovelli, S. Speziale, and I. Vilensky, “Realistic Observable in Background-Free [21] E. D. Kovetz, A. Raccanelli, and M. Rahman, “Cosmological Constraints with Clustering-Based [22] B. Carr and S. Hawking, “Black[23] holes inF. the M. early Rieger, Universe,” E. Ona-Wilhelmi, and F. A. Aharonian, “TeV astronomy,” [15] B. Kol and E. Sorkin, “On black-brane instability in an arbitrary dimension,” [19] M. Jarvis, D. Bacon, C. Blake, M. Brown, S. Lindsay, A. Raccanelli, M. Santos, and D. J. Schwarz, [10] C. Rovelli and F. Vidotto, “Evidence for Maximal Acceleration and Singularity Resolution in [12] A. Corichi and P. Singh, “Loop quantization of the Schwarzschild interior revisited,” [17] K. Griest, A. M. Cieplak, and M. J. Lehner, “New limits on[18] primordial blackF. hole V. Alvise dark Raccanelli matter Licia from Verde, an “Effects of primordial black holes quantum tunneling on galaxy [20] B. Ménard, R. Scranton, S. Schmidt, C. Morrison, D. Jeong, T. Budavari, and M. Rahman, [11] A. Ashtekar and M. Bojowald, “Quantum geometry and the Schwarzschild singularity,” [13] C. Rovelli and F. Vidotto, “Planck stars,” Quantum insights on Primordial Black Holes as Dark Matter [14] R. Gregory and R. Laflamme, “Black strings and p-branes are unstable,” PoS(EDSU2018)046 . . 181 191 1810.02680 Francesca Vidotto Phys. Rev. D - 1805.03872 R. Astron. Soc. . . Comput. Phys. Commun. . (2007) 166–236, . . 1404.5821 442 1412.0342v1 1810.04357 9 Phys. Rept. 1409.4031 1602.03235v2 (sep, 2014) . . 90 (oct, 2018) 1. . Nature 1410.3012 1810.09459 . . 1805.03224 Remnants: A Surprising Scenario for the End of a Black Hole,”. 1804.04147 astro-ph/0701748 Rasmussen, and P. Z. Skands, “An Introduction to PYTHIA 8.2,” (2015) 159–177, D. Champion, P. Chandra, G. DaS. Costa, Johnston, C. M. Delvaux, M. C. Kasliwal, Flynn, E. N.J. F. Gehrels, S. Keane, J. Mulchaey, S. C. Greiner, Keller, Ng, A. J. E. Jameson, Kocz,P. O. Tisserand, M. Ofek, W. Kramer, Van D. G. Straten, A. Leloudas, and Perley, D. C. A.multiwavelength Malesani, Wolf, Possenti, follow-up,” “A Tech. B. real-time Rep. P. fast 0000, Schmidt, radio 2014. Y. Shen, burst: B. polarization Stappers, detection and Intergalactic Medium,” tech. rep., 2016. measurements,” Source-Count Distribution for Fast Radio Bursts,” M. Sammons, A. W. Hotan, M.A. A. P. Voronkov, R. Chippendale, J. C. Beresford, Haskins, M. M.Sadler, Brothers, Leach, E. A. M. R. J. Marquarding, Troup, Brown, D. J. J. McConnell, Tuthill, D. M.G. M. Bunton, A. Gürkan, T. Whiting, Pilawa, G. E. J. Heald, M. R. and Allison, C.a C. J. wide-field S. Riseley, survey,” “The Anderson, dispersion-brightness M. relation E. for Bell, fast J. radio D. bursts Collier, from L. Shao, S. Andrianomena, E. Athanassoula,A. D. Bosma, Bacon, M. R. Brüggen, Barkana, C. G. Burigana,Connors, Bertone, C. Á. C. Bœhm, de Bonvin, F. la Calore, Cruz-Dombriz, J. P.Y. A. K. Z. R. S. Ma, Cembranos, Dunsby, R. N. C. Maartens, Fornengo, Clarkson, M. D. R.P. Méndez-Isla, J. Gaggero, M. S. Quinn, I. T. D. M. Harrison, Mohanty, Regis, J. S. P. Larena, G. Saha,T. Murray, Venumadhav, M. F. D. Vidotto, Sahlén, F. Parkinson, M. Villaescusa-Navarro, A. Y. Sakellariadou, Wang, Pourtsidou, J. C.Gaensler, Silk, Weniger, and L. T. A. Wolz, Trombetti, F. Weltman, F. Zhang, “Fundamental Vazza, B. Physics M. with the Square Kilometer Array,” (1977) 489. Part. Fields, Gravit. Cosmol. [35] E. Nakar, “Short-Hard Gamma-Ray Bursts,” [37] E. Bianchi, M. Christodoulou, F. D ’ambrosio, C. Rovelli, and H.[38] M. Haggard, “WhiteC. Holes Rovelli as and F. Vidotto, “White-hole dark matter and the origin of[39] past low-entropy,” C. Rovelli and F. Vidotto, “Small[40] black/white hole stabilityC. and Rovelli and dark F. matter,” Vidotto, “Pre-big-bang black-hole remnants and the past low entropy,” [36] T. Sjöstrand, S. Ask, J. R. Christiansen, R. Corke, N. Desai, P. Ilten, S. Mrenna, S. Prestel, C. O. [34] A. Barrau and C. Rovelli, “Planck star phenomenology,” [31] E. Petroff, M. Bailes, E. D. Barr, B. R. Barsdell, N. D. R. Bhat, F. Bian, S. Burke-Spolaor, M. Caleb, [32] T. Akahori, D. Ryu, and B. M. Gaensler, “Fast Radio Bursts as[33] Probes ofW. Lu, Magnetic P. Fields Kumar, in and the R. Narayan, “Fast radio burst source properties from polarization [28] C. W. James, R. D. Ekers, J. P. Macquart, K. W. Bannister, and R. M. Shannon, “The Slope of the Quantum insights on Primordial Black Holes as Dark Matter [26] R. D. Blandford, “Spectrum of a radio pulse from an exploding black hole,” [29] R. M. Shannon, J.-P. Macquart, K. W. Bannister, R. D. Ekers, C. W. James, S. Osłowski, H. Qiu, [30] P. Bull, S. Camera, K. Kelley, H. Padmanabhan, J. Pritchard, A. Raccanelli, S. Riemer-Sørensen, [27] A. Barrau, C. Rovelli, and F. Vidotto, “Fast Radio Bursts and White Hole Signals,” PoS(EDSU2018)046 . (jun, 1999) Francesca Vidotto 1206.4196 60 Phys. Rev. D 10 023507. [42] R. H. Brandenberger, “The Matter Bounce Alternative to Inflationary Cosmology,” Quantum insights on Primordial Black Holes as Dark Matter [41] D. Wands, “Duality invariance of cosmological perturbation spectra,”