DOCSLIB.ORG

The Merger Rate of Black Holes in a Primordial Black Hole Cluster

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Merger Rate of Black Holes in a Primordial Black Hole Cluster Communication The Merger Rate of Black Holes in a Primordial Black Hole Cluster Viktor D. Stasenko * and Alexander A. Kirillov Moscow Engineering Physics Institute, National Research Nuclear University MEPhI, 115409 Moscow, Russia; [email protected] * Correspondence: [email protected] Abstract: In this paper, the merger rate of black holes in a cluster of primordial black holes (PBHs) is investigated. The clusters have characteristics close to those of typical globular star clusters. A cluster −2 that has a wide mass spectrum ranging from 10 to 10 M (Solar mass) and contains a massive 3 central black hole of the mass M• = 10 M is considered. It is shown that in the process of the evolution of cluster, the merger rate changed significantly, and by now, the PBH clusters have passed the stage of active merging of the black holes inside them. Keywords: black hole cluster; black hole merging; merger rate; primordial black holes; Fokker– Planck equation 1. Introduction Since the registration of gravitational waves from black hole mergers, interest in primor- dial black holes (PBHs) and their clusters has increased. Models of the formation of PBH clusters are considered with a narrow mass spectrum [1–3] and a wide one [4–6]. The first type of clusters appears in the early Universe due to the collapse of density perturbations. The second type describes cluster formation via gravitational collapse of domain walls appearing Citation: Stasenko, V.D.; Kirillov, in the early Universe as a result of the evolution of scalar fields in the inflationary epoch; see A.A. The Merger Rate of Black Holes review [7] and references therein. A cluster is formed after detachment from the Hubble flow in a Primordial Black Hole Cluster. and consequent collapse of domain walls into PBHs. Finally, it forms at the redshift z ∼ 104 Physics 2021, 3, 372–378. https:// and obtains characteristics close to those of globular star clusters. Despite the similarities, the doi.org/10.3390/physics3020026 considered PBHs clusters might have black holes with a wide range of masses and a massive black hole at the center. We discussed the evolution of these systems in Refs. [8,9] in the Received: 19 March 2021 Accepted: 10 May 2021 framework of two-body relaxation; however, the question of the black hole merger rate was Published: 17 May 2021 not studied. This paper continues the previous investigation and explores the merger rate of black holes during the evolution of such clusters. Publisher’s Note: MDPI stays neutral There are two possibilities: mergers of black holes with each other and with a massive with regard to jurisdictional claims in central black hole (CBH). The first possibility was discussed in Refs. [7,10–13] in the context 4 published maps and institutional affil- of PBH clusters with narrow mass spectra (with the number of PBH NPBH . 10 ) and in iations. Refs. [14–22] in the context of a dense globular star cluster. The second possibility was considered for globular star clusters [23–28] and galactic nuclei [29–33] in the loss-cone treatment [34,35]. In the calculations described in this paper, it is shown that during cluster evolution, mergers mainly occur with a central black hole; nevertheless, the merger rate is low. Copyright: © 2021 by the authors. Licensee MDPI, Basel, Switzerland. 2. Estimations This article is an open access article distributed under the terms and Let us estimate the merger rate of black holes for a single-mass PBH cluster. For the 5 conditions of the Creative Commons cluster with the total mass M = 10 M (Solar mass)p and the characteristic radius R ∼ 1 pc, −1 Attribution (CC BY) license (https:// the characteristic velocity of the PBHs is v = GM/R ≈ 20 km s [7], where G is the creativecommons.org/licenses/by/ 4.0/). Physics 2021, 3, 372–378. https://doi.org/10.3390/physics3020026 https://www.mdpi.com/journal/physics Physics 2021, 3 373 Newtonian gravitational constant. The merger cross-section of two black holes with masses m and m0 is given by [14,36]: 85p 2/7 G2(m + m0)10/7m2/7m02/7 s = 2p p . (1) 6 2 c10/7jv − v0j18/7 This cross-section describes the formation of PBHs of binaries due to gravitational radiation. In the present calculations, it is assumed that the lifetime of a binary is less than the dynamical time of the PBH cluster, the approximation similar to one used in Refs. [14,17,22]. The merger rate can be estimated as G ≈ Nvsn, where N is the number of PBHs in the cluster, n is the number density of the PBHs. For simplicity, let us consider a cluster with a constant number density of n = 3N/4pR3. Thus, the merger rate is: M 17/14 R −31/14 G ∼ 10−10 yr−1. (2) 105 M 1 pc During the cluster evolution, black holes evaporate from the core. This process is a slow diffusion in the velocity space. Therefore, one can assume that black holes escaping the cluster carry away zero energy. Hence, the total energy of the core is conserved. According to the virial theorem, the total energy is E = −G(mN)2/2R. Therefore, in the process of BH evaporation, the core size is R ∝ N2. As a result, the relationship between the number of black holes in the cluster core and the merger rate is: G ∝ N−3.2. In this study, one considers the clusters with a massive CBH. As a result of the capture of less massive black holes, the CBH mass grows as M˙ • = rscv, where r is the density of 2 2 black holes in the cluster, and sc = 4prg(c/v) is the cross-section for particle capture by a Schwarzschild black hole [37], rg is the gravitational radius of the CBH. Estimation of M˙ • gives −5/2 1/2 2 −11 R M M• −1 M˙ • ∼ 10 M yr . (3) 1 pc 105 M 103 M If the mass of the CBH M• is much less than the core mass, Mc, then the CBH does −4.5 not affect the core collapse. Hence, the growth rate of the CBH evolves as M˙ • ∝ N . Hence, the merger rate of the BHs may play a significant role in both cases. Note that when the core contracts significantly, the CBH stops the collapse and causes an expansion phase [27,28,33,38,39]. Note that there is also another mechanism of creating PBH binaries in a cluster based on three-body interaction. The third body can carry away enough energy to form a binary from the two others. The formed binaries lose energy through interactions with single black holes and gravitational radiation. As a result, pairs of mergers are caused. This possibility was studied for globular star clusters with black holes in Refs. [17–22]. In addition, these binaries might significantly affect the cluster evolution, stop the core collapse, and cause gravothermal oscillations [40–44]. These binaries will descend towards the cluster center under the influence of dynamical friction. In the case considered in this paper, they will be 3 destroyed as a result of interactions with the massive central black hole (∼10 M )[45,46]. The characteristic time scale for this process is [34]: v3 v 3 r −1 m −1 ∼ B ≈ B B tdf 2 1.7 −1 5 −1 Myr, (4) 4pG mBr ln L 20 km s 10 M pc 20 M where vB and mB are the velocity and the mass of the PBH binary, and ln L = 10, where ln L is the Coulomb logarithm. On the other hand, the merger time tgw of two black holes of the same mass m in a circular orbit with the separation a due to an emission of gravitational waves is given by the expression [37]: − 5c5a4 a 4 m 3 tgw = ≈ 1.6 Myr. (5) 512G3m3 0.01 au 10 M Physics 2021, 3 374 The condition tgw < tdf leads to the maximum value of a for a binary system that merges before its destruction: 1/4 3/4 −2 tdf m a . 10 au. (6) 2 Myr 10 M The probability of the formation of such hard binaries requires a careful analysis. Thus, we assume that all binaries that are forming are destroyed by the CBH. The destruction mechanism also remains true if the PBH binaries are primordial in a cluster. These binaries may have a similar origin that of those formed in the early Universe [47–49]. 3. Merger Rate of Black Holes The merger rate of black holes with the mass m per unit of phase space, per unit of mass, and per unit of time is given by [14]: Z Z g = f (r, v, m) dm0 dv0 f (r, v0, m0) jv − v0j sm, m0, jv − v0j, (7) where f is the distribution function of black holes in the cluster and s is the merger cross section is defined by (1). The expression (1) shows that the cross-section is s = s(m, m0)jv − v0j−18/7. In the case of spherical symmetry, Equation (7) reads: 14p f (r, v, m) Z Z h i g = dm0 dv0 v0s(m, m0) f (r, v0, m0) (v + v0)3/7 − jv − v0j3/7 . (8) 3v Let us take the delta-functional approximation for the distribution function of the i-th black hole type: n (r) f (r, v, m) = i d v2 − v2(r) d(m − m ), (9) i 2pv i i 2 where vi (r) is the mean-squared velocity [50]: 0 Z 3/2 2 4p h i vi (r) = dE fi(E) 2 E − f(r) , (10) ni(r) f(r) and mi and ni are, respectively, the mass and the number density of the i-th PBH type and f(r) is the gravitational potential of the cluster.
Load more

Recommended publications
  • Searching for Evaporating Primordial Black Holes Using Fermi Gamma Ray Telescope Data
    Searching for Evaporating Primordial Black Holes using Fermi Gamma Ray Telescope Data Jagdev Bains CID 00552650 Horns Group, DESY A thesis submitted for the degree of MSci May 2011 Abstract All confirmed photon event data (≥ 100MeV) recorded by the Fermi Gamma Ray Telescope's (FGRT's) Large Area Telescope (LAT) was used to attempt to locate photons emitted by evaporating primordial black holes (PBHs) via Hawking radiation. An 'event' is a single photon recorded by the LAT. HEALPix was used to group photons spatially into pixels with unique iden- tification numbers, and all events within these pixels were sorted in time. The time interval between subsequent photons in each pixel was calculated and a histogram made for each pixel. The expected time distribution of events was compared with the measured for each pixel to identify any can- didates for further analysis; if the expected varied significantly with the measured at the smallest time intervals (26µs − 10s). Several pixels were found that met the criteria for further analysis, however they were all found to include known high energy photon sources. No pixels were found with extra photons at short time intervals that could not be attributed to gamma- ray bursts (GRBs) or known sources. A limit was calculated on the range at which the LAT could detect a PBH burst, between 16.69 and 289.16pc. Alle photonischen (≥ 100MeV) und vom Large Area Telescope (LAT) des Fermi Gamma Ray Telescope's (FGRT's) dokumentierten, bestaetigten Ereignisse wurden benutzt, um Photonen zu lokalisieren, die durch sich verfluechti- gende primordiale schwarze Loecher (PBHs) mit Hilfe der Hawking Strahlung emittiert wurden.
    [Show full text]
  • Arxiv:2105.11481V1 [Astro-Ph.CO] 24 May 2021
    Ultrahigh-energy Gamma Rays and Gravitational Waves from Primordial Exotic Stellar Bubbles Yi-Fu Cai,1, 2, 3, ∗ Chao Chen,1, 2, 3, y Qianhang Ding,4, 5, z and Yi Wang4, 5, x 1Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China 2School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui 230026, China 3CAS Key Laboratory for Research in Galaxies and Cosmology, University of Science and Technology of China, Hefei, Anhui 230026, China 4Department of Physics, The Hong Kong University of Science and Technology, Clear Water Bay, Kowloon, Hong Kong, P.R.China 5Jockey Club Institute for Advanced Study, The Hong Kong University of Science and Technology, Clear Water Bay, Kowloon, Hong Kong, P.R.China We put forward a novel class of exotic celestial objects that can be produced through phase transitions occurred in the primordial Universe. These objects appear as bubbles of stellar sizes and can be dominated by primordial black holes (PBHs). We report that, due to the processes of Hawking radiation and binary evolution of PBHs inside these stellar bubbles, both electromagnetic and gravitational radiations can be emitted that are featured on the gamma-ray spectra and stochastic gravitational waves (GWs). Our results reveal that, depending on the mass distribution, the exotic stellar bubbles consisting of PBHs provide not only a decent fit for the ultrahigh-energy gamma-ray spectrum reported by the recent LHAASO experiment, but also predict GW signals that are expected to be tested by the forthcoming GW surveys.
    [Show full text]
  • Primordial Black Holes from Thermal Inflation
    IMPERIAL/TP/2019/TM/01 KCL-PH-TH/2019-33 Primordial Black Holes from Thermal Inflation Konstantinos Dimopoulos,a Tommi Markkanen,b;c Antonio Racioppic and Ville Vaskonend aConsortium for Fundamental Physics, Physics Department, Lancaster University, Lancaster LA1 4YB, UK bDepartment of Physics, Imperial College London, Blackett Laboratory, London, SW7 2AZ, UK cNational Institute of Chemical Physics and Biophysics, R¨avala 10, 10143 Tallinn, Estonia dPhysics Department, King's College London, London WC2R 2LS, UK E-mail: [email protected], [email protected], tommi.markkanen@kbfi.ee, antonio.racioppi@kbfi.ee, [email protected] Abstract. We present a novel mechanism for the production of primordial black holes (PBHs). The mechanism is based on a period of thermal inflation followed by fast-roll inflation due to tachyonic mass of order the Hubble scale. Large perturbations are generated at the end of the thermal inflation as the thermal inflaton potential turns from convex to concave. These perturbations can lead to copious production of PBHs when the relevant scales re-enter horizon. We show that such PBHs can naturally account for the observed dark matter in the Universe when the mass of the thermal inflaton is about 106 GeV and its coupling to the thermal bath preexisting the late inflation is of order unity. We consider also the possibility of forming the seeds of the supermassive black holes. In this case we find that the mass of the thermal inflaton is about 1 GeV, but its couplings have to be very small, ∼ 10−7. Finally we study a concrete realisation of our mechanism through a running mass model.
    [Show full text]
  • Primordial Black Holes As a Dark Matter Candidate Are Severely Constrained by the Galactic Center 511 Kev Γ-Ray Line
    PHYSICAL REVIEW LETTERS 123, 251101 (2019) Primordial Black Holes as a Dark Matter Candidate Are Severely Constrained by the Galactic Center 511 keV γ-Ray Line Ranjan Laha * Theoretical Physics Department, CERN, 1211 Geneva 23, Switzerland (Received 25 June 2019; revised manuscript received 9 October 2019; published 16 December 2019) We derive the strongest constraint on the fraction of dark matter that can be composed of low mass primordial black holes by using the observation of the Galactic Center 511 keV γ-ray line. Primordial black holes of masses ≲1015 kg will evaporate to produce eÆ pairs. The positrons will lose energy in the Galactic Center, become nonrelativistic, then annihilate with the ambient electrons. We derive robust and conservative bounds by assuming that the rate of positron injection via primordial black hole evaporation is less than what is required to explain the SPI/INTEGRAL observation of the Galactic Center 511 keV γ-ray line. Depending on the primordial black hole mass function and other astrophysical uncertainties, these constraints are the most stringent in the literature and show that primordial black holes contribute to less than 1% of the dark matter density. Our technique also probes part of the mass range which was completely unconstrained by previous studies. DOI: 10.1103/PhysRevLett.123.251101 Introduction.—Is it possible to constrain the primordial a few hundred M⊙. PBHs are one of the oldest candidates black hole (PBH) density such that it cannot contribute to of dark matter, and their abundance has been studied in a the entire dark matter density over its viable mass range? Answering this question will have important implications 0 for the search of the identity of dark matter and inflationary 10 dynamics which can give rise to PBHs [1–6].
    [Show full text]
  • Solving Puzzles of GW150914 by Primordial Black Holes
    Prepared for submission to JCAP Solving puzzles of GW150914 by primordial black holes S. Blinnikov,a;b;c;d;1 A. Dolgov,b;a N.K. Poraykoe;a and K.Postnovc;a;f aITEP, Bol. Cheremushkinsaya ul., 25, 117218 Moscow, Russia bNovosibirsk State University, Novosibirsk, 630090, Russia cSternberg Astronomical Institute, Moscow M.V. Lomonosov State University, Universitetskij pr., 13, Moscow 119234, Russia dKavli IPMU (WPI), Tokyo University, Kashiwa, Chiba, Japan eMax-Planck-Institut f¨urRadioastronomie, Bonn, Germany f Faculty of Physics, Moscow M. V. Lomonosov State University, 119991 Moscow, Russia E-mail: [email protected], [email protected], [email protected], [email protected] Abstract. The black hole binary properties inferred from the LIGO gravitational wave signal GW150914 posed several serious problems. The high masses and low effective spin of black hole binary can be explained if they are primordial (PBH) rather than the products of the stellar binary evolution. Such PBH properties are postulated ad hoc but not derived from fundamental theory. We show that the necessary features of PBHs naturally follow from the slightly modified Affleck-Dine (AD) mechanism of baryogenesis. The log-normal distribution of PBHs, predicted within the AD paradigm, is adjusted to provide an abundant population of low-spin stellar mass black holes. The same distribution gives a sufficient number of quickly growing seeds of supermassive black holes observed at high redshifts and may comprise an appreciable fraction of Dark Matter which does not contradict any existing observational limits. Testable predictions of this scenario are discussed. arXiv:1611.00541v2 [astro-ph.HE] 29 Nov 2016 1Corresponding author.
    [Show full text]
  • Table of Contents (Print)
    PHYSICAL REVIEW D PERIODICALS For editorial and subscription correspondence, Postmaster send address changes to: please see inside front cover (ISSN: 1550-7998) APS Subscription Services P.O. Box 41 Annapolis Junction, MD 20701 THIRD SERIES, VOLUME 94, NUMBER 6 CONTENTS D15 SEPTEMBER 2016 The Table of Contents is a total listing of Parts A and B. Part A consists of articles 061501–064038, and Part B articles 064039–069903(E) PART A RAPID COMMUNICATIONS Spacetime foam induced collective bundling of intense fields (7 pages) ............................................................ 061501(R) Teodora Oniga and Charles H.-T. Wang New dynamical instability in asymptotically anti–de Sitter spacetime (6 pages) ................................................... 061901(R) Umut Gürsoy, Aron Jansen, and Wilke van der Schee Low energy signatures of nonlocal field theories (6 pages) ........................................................................... 061902(R) Alessio Belenchia, Dionigi M. T. Benincasa, Eduardo Martín-Martínez, and Mehdi Saravani ARTICLES Light dark matter scattering in outer neutron star crusts (7 pages) ................................................................... 063001 Marina Cermeño, M.Ángeles Pérez-García, and Joseph Silk Implications of gamma-ray observations on proton models of ultrahigh energy cosmic rays (10 pages) ...................... 063002 A. D. Supanitsky Analogue black holes in relativistic BECs: Mimicking Killing and universal horizons (14 pages) ............................. 063003 Bethan Cropp, Stefano
    [Show full text]
  • Primordial Black Hole Dark Matter from Single Field Inflation
    IFT-UAM/CSIC-17-084 Primordial black hole dark matter from single field inflation Guillermo Ballesteros a and Marco Taoso b a Institut de Physique Théorique, Université Paris Saclay, CEA, CNRS b Instituto de Física Teórica UAM/CSIC, Calle Nicolás Cabrera 13-15, Cantoblanco E-28049 Madrid, Spain. Abstract We propose a model of inflation capable of generating a population of light black holes (about 10−16 – 10−14 solar masses) that might account for a significant fraction of the dark matter in the Universe. The effective potential of the model features an approximate inflection point arising from two-loop order logarithmic corrections in well-motivated and perturbative particle physics examples. This feature decelerates the inflaton before the end of inflation, enhancing the primordial spectrum of scalar fluctuations and triggering efficient black hole production with a peaked mass distribution. At larger field values, inflation occurs thanks to a generic small coupling between the inflaton and the curvature of spacetime. We compute accurately the peak mass and abundance of the primordial black holes using the Press-Schechter and Mukhanov-Sasaki formalisms, showing that the slow-roll approximation fails to reproduce the correct results by orders of magnitude. We study as well a qualitatively similar implementation of the idea, where the approximate inflection point is due to competing terms in a generic polynomial potential. In both models, requiring a significant part of the dark matter abundance to be in the form of black holes implies a small blue scalar tilt with a sizable negative running and a tensor spectrum that may be detected by the next-generation probes of the cosmic microwave background.
    [Show full text]
  • X-Ray and Gamma-Ray Limits on the Primordial Black Hole Abundance
    Physics Letters B 808 (2020) 135624 Contents lists available at ScienceDirect Physics Letters B www.elsevier.com/locate/physletb X-ray and gamma-ray limits on the primordial black hole abundance from Hawking radiation ∗ ∗ ∗ Guillermo Ballesteros a,b, , Javier Coronado-Blázquez a,b, , Daniele Gaggero a, a Instituto de Física Teórica UAM/CSIC, Calle Nicolás Cabrera 13-15, Cantoblanco E-28049 Madrid, Spain b Departamento de Física Teórica, Universidad Autónoma de Madrid (UAM), Campus de Cantoblanco, 28049 Madrid, Spain a r t i c l e i n f o a b s t r a c t 16 Article history: The non-observation of extragalactic Hawking radiation from primordial black holes of 10 g sets a Received 28 April 2020 conservative strong bound on their cosmological abundance. We revisit this bound and show how it can Received in revised form 4 July 2020 be improved (both in mass reach and strength) by an adequate modeling of the combined AGN and blazar Accepted 13 July 2020 emission in the MeV range. We also estimate the sensitivity to the primordial black hole abundance of Available online 16 July 2020 a future X-ray experiment capable of identifying a significantly larger number of astrophysical sources Editor: M. Trodden contributing to the diffuse background in this energy range. © 2020 The Author(s). Published by Elsevier B.V. This is an open access article under the CC BY license 3 (http://creativecommons.org/licenses/by/4.0/). Funded by SCOAP . 1. Introduction from the observed distribution of white dwarfs [7], as well as from the disruption of neutron stars in the PBH mass range from 19 23 The isotropic background radiation that fills the Universe and 10 g to 10 g [8] has been challenged [9], opening the possibil- 22 extends over more than 16 orders of magnitude in frequency ity that PBHs of mass below ∼ 5 × 10 g –with higher masses –from radio waves all the way up to high-energy gamma rays [1]– being constrained by microlensing [10]– could explain all the carries information on the emission mechanisms of different astro- DM.
    [Show full text]
  • Cosmological Implications of Primordial Black Holes
    Prepared for submission to JCAP Cosmological implications of Primordial Black Holes Jos´eLuis Bernala;b Nicola Bellomoa;b Alvise Raccanellia Licia Verdea;c aICC, University of Barcelona, IEEC-UB, Mart´ıi Franqu`es,1, E08028 Barcelona, Spain bDept. de F´ısica Qu`antica i Astrof´ısica, Universitat de Barcelona, Mart´ı i Franqu`es1, E08028 Barcelona, Spain cICREA, Pg. Llu´ısCompanys 23, 08010 Barcelona, Spain E-mail: [email protected], [email protected], [email protected], [email protected] Abstract. The possibility that a relevant fraction of the dark matter might be comprised of Pri- mordial Black Holes (PBHs) has been seriously reconsidered after LIGO's detection of a ∼ 30M binary black holes merger. Despite the strong interest in the model, there is a lack of studies on possible cosmological implications and effects on cosmological parameters inference. We investigate correlations with the other standard cosmological parameters using cosmic microwave background observations, finding significant degeneracies, especially with the tilt of the primordial power spec- trum and the sound horizon at radiation drag. However, these degeneracies can be greatly reduced with the inclusion of small scale polarization data. We also explore if PBHs as dark matter in simple extensions of the standard ΛCDM cosmological model induces extra degeneracies, especially between the additional parameters and the PBH's ones. Finally, we present cosmic microwave background con- straints on the fraction of dark matter in PBHs, not only for monochromatic PBH mass distributions but also for popular extended mass distributions. Our results show that extended mass distribution's constraints are tighter, but also that a considerable amount of constraining power comes from the high-` polarization data.
    [Show full text]
  • Low-Mass Black Holes As the Remnants of Primordial Black Hole Formation
    REVIEW Received 31 Aug 2012 | Accepted 22 Nov 2012 | Published 18 Dec 2012 DOI: 10.1038/ncomms2314 Low-mass black holes as the remnants of primordial black hole formation Jenny E. Greene1 Bridging the gap between the approximately ten solar mass ‘stellar mass’ black holes and the ‘supermassive’ black holes of millions to billions of solar masses are the elusive ‘intermediate- mass’ black holes. Their discovery is key to understanding whether supermassive black holes can grow from stellar-mass black holes or whether a more exotic process accelerated their growth soon after the Big Bang. Currently, tentative evidence suggests that the progenitors of 4 5 supermassive black holes were formed as B10 –10 M} black holes via the direct collapse of gas. Ongoing searches for intermediate-mass black holes at galaxy centres will help shed light on this formation mechanism. ver the last decade we have come to understand that supermassive black holes, with masses of millions to billions of times the mass of the Sun, are very common in the Ocentres of massive galaxies1. We would like to understand when and how they formed and grew. We cannot yet watch the first supermassive black holes form. They did so soon after the Big Bang, and light from those distant events is beyond the reach of today’s telescopes. However, we do have two very interesting limits on the formation of the first black holes. The first comes from observations of the most distant known black holes: light is emitted by material falling into the deep gravitational potential of the black hole.
    [Show full text]
  • Table of Contents (Print)
    PHYSICAL REVIEW D PERIODICALS For editorial and subscription correspondence, Postmaster send address changes to: please see inside front cover (ISSN: 1550-7998) APS Subscription Services P.O. Box 41 Annapolis Junction, MD 20701 THIRD SERIES, VOLUME 94, NUMBER 8 CONTENTS D15 OCTOBER 2016 The Table of Contents is a total listing of Parts A and B. Part A consists of articles 081101–084026, and Part B articles 084027–089902(E) PART A RAPID COMMUNICATIONS Coherent observations of gravitational radiation with LISA and gLISA (5 pages) ................................................ 081101(R) Massimo Tinto and José C. N. de Araujo Viscosity of fused silica and thermal noise from the standard linear solid model (5 pages) ..................................... 081102(R) N. M. Kondratiev and M. L. Gorodetsky Anomalous magnetohydrodynamics in the extreme relativistic domain (6 pages) ................................................. 081301(R) Massimo Giovannini Quantum simulation of traversable wormhole spacetimes in a dc-SQUID array (6 pages) ....................................... 081501(R) Carlos Sabín Black hole field theory with a firewall in two spacetime dimensions (6 pages) ................................................... 081502(R) C. T. Marco Ho (何宗泰), Daiqin Su (粟待欽), Robert B. Mann, and Timothy C. Ralph ARTICLES Modulation sensitive search for nonvirialized dark-matter axions (13 pages) ...................................................... 082001 J. Hoskins, N. Crisosto, J. Gleason, P. Sikivie, I. Stern, N. S. Sullivan, D. B. Tanner, C. Boutan, M. Hotz, R. Khatiwada, D. Lyapustin, A. Malagon, R. Ottens, L. J. Rosenberg, G. Rybka, J. Sloan, A. Wagner, D. Will, G. Carosi, D. Carter, L. D. Duffy, R. Bradley, J. Clarke, S. O’Kelley, K. van Bibber, and E. J. Daw Search for ultrarelativistic magnetic monopoles with the Pierre Auger observatory (12 pages) ................................
    [Show full text]
  • Arxiv:2105.10506V1 [Hep-Ph] 21 May 2021
    Probing the Particle Spectrum of Nature with Evaporating Black Holes Michael J. Baker1, ∗ and Andrea Thamm2, y 1ARC Centre of Excellence for Dark Matter Particle Physics, School of Physics, The University of Melbourne, Victoria 3010, Australia 2School of Physics, The University of Melbourne, Victoria 3010, Australia (Dated: May 25, 2021) Photons radiated from an evaporating black hole in principle provide complete information on the particle spectrum of nature up to the Planck scale. If an evaporating black hole were to be observed, it would open a unique window onto models beyond the Standard Model of particle physics. To demonstrate this, we compute the limits that could be placed on the size of a dark sector. We find that observation of an evaporating black hole at a distance of 0.01 parsecs could probe dark sector models containing one or more copies of the Standard Model particles, with any mass scale up to 300 TeV. Introduction { Determining the particle spec- When the temperature rises above a particle mass trum of nature is one of the fundamental goals of threshold, a new radiation process becomes avail- physics. The last 120 years have seen a huge ad- able, the black hole loses mass at a faster rate, and vance in our understanding of the elementary parti- the temperature increases at a faster rate. This cles, from J.J. Thomson's discovery of the electron in continues until the temperature reaches the Planck 1897 [1] to the discovery of the Higgs boson at CERN scale, at which point quantum gravity effects become in 2012 [2,3], completing the Standard Model (SM) important.
    [Show full text]