Comparison of UHECR spectra from necklaces and vortons

Similar documents
Comparison of UHECR spectra from necklaces and vortons

Hard component of ultra-high energy cosmic rays and vortons arxiv:astro-ph/ v2 11 Apr 2001

Ultra High Energy Cosmic Rays I

Ultra High Energy Cosmic Rays: Observations and Analysis

COSMOGENIC AND TOP-DOWN UHE NEUTRINOS

The Pierre Auger Project. Angela Olinto University of Chicago

century. The number of events observed so far is well below hundred the primary particle content is currently unknown. The special interest in cosmic

Implications of recent cosmic ray results for ultrahigh energy neutrinos

Extensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware

Investigation on mass composition of UHE cosmic rays using CRPropa 2.0

arxiv:hep-ph/ v2 23 Sep 1998

Extremely High Energy Neutrinos

Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002

Ultrahigh Energy cosmic rays II

99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park

Frontiers: Ultra High Energy Cosmic Rays

Ultra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux

Ultra-High Energy Cosmic Rays & Neutrinos above the Terascale

Ultrahigh Energy Cosmic Rays propagation II

arxiv:astro-ph/ v1 17 Dec 2004

SEARCHES OF VERY HIGH ENERGY NEUTRINOS. Esteban Roulet CONICET, Centro Atómico Bariloche

On heavy Majorana neutrinos as a source of the highest energy cosmic rays

Neutrinos as a signature of ultrahigh energy photons at high red shift

Ultra-High Energy Cosmic Rays and Astrophysics. Hang Bae Kim Hanyang University Hangdang Workshop,

TESTING PHYSICS BEYOND SM

STATUS OF ULTRA HIGH ENERGY COSMIC RAYS

The Physics of Ultrahigh Energy Cosmic Rays. Example Poster Presentation Physics 5110 Spring 2009 Reminder: Posters are due Wed April 29 in class.

Ultra High Energy Cosmic Rays What we have learnt from. HiRes and Auger. Andreas Zech Observatoire de Paris (Meudon) / LUTh

OLD AND NEW PROCESSES OF VORTON FORMATION

Soon after the discovery of the cosmic background radiation (CBR), Greisen [1], and independently, Zatsepin amd Kuz'min [2], realized that it limits t

PoS(jhw2004)003. Deciphering the Extreme Universe. Angela V. Olinto

Cosmic Ray Astronomy. Qingling Ni

Studies of Ultra High Energy Cosmic Rays with the Pierre Auger Observatory

Particle Radiation and Cosmic Rays from Cosmic Strings

Looking Beyond the Standard Model with Energetic Cosmic Particles

Fundamental Particles

Open questions with ultra-high energy cosmic rays

UHE Cosmic Rays and Neutrinos with the Pierre Auger Observatory

astro-ph/ Dec 94

Search for clustering of ultra high energy cosmic rays from the Pierre Auger Observatory

PEV NEUTRINOS FROM THE PROPAGATION OF ULTRA-HIGH ENERGY COSMIC RAYS. Esteban Roulet CONICET, Bariloche, Argentina

Secondary particles generated in propagation neutrinos gamma rays

Gamma Rays from Dark Matter

The Pierre Auger Observatory Status - First Results - Plans

UHECRs sources and the Auger data

Absorption and production of high energy particles in the infrared background

arxiv:astro-ph/ v1 28 Oct 2004

> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!

The Pierre Auger Observatory in 2007

Possible sources of very energetic neutrinos. Active Galactic Nuclei

Recent results from the Pierre Auger Observatory

Spectra of Cosmic Rays

We can check experimentally that physical constants such as α have been sensibly constant for the past ~12 billion years

The Highest Energy Cosmic Rays

RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY

Overview: UHECR spectrum and composition Arrival directions and magnetic field Method for search for UHE nuclei sources Application to the Auger data

Implications of cosmic ray results for UHE neutrinos

Cosmogenic neutrinos II

Lecture 9 - Applications of 4 vectors, and some examples

The Scale-Symmetric Theory as the Origin of the Standard Model

New Tests of Lorentz Invariance Following from Observations of. the Highest Energy Cosmic Gamma Rays. Abstract

Ultra High Energy Cosmic Rays. Malina Kirn March 1, 2007 Experimental Gravitation & Astrophysics

Properties of Elementary Particle Fluxes in Cosmic Rays. TeVPA Aug. 7, Yuan-Hann Chang National Central University, Taiwan

arxiv: v1 [astro-ph.he] 14 Jul 2017

Dr. John Kelley Radboud Universiteit, Nijmegen

Astronomy 182: Origin and Evolution of the Universe

The Matter-Antimatter Asymmetry and New Interactions

UHECR: PROGRESS AND PROBLEMS

On the GCR/EGCR transition and UHECR origin

What is the HIGGS BOSON and why does physics need it?

Ultra High Energy Cosmic Rays. and

PeV Neutrinos from Star-forming Regions. Hajime Takami KEK, JSPS Fellow

IMPACT OF OSCILLATIONS ON UHE NEUTRINO ASTRONOMY

Dark matter and IceCube neutrinos

Lecture PowerPoint. Chapter 32 Physics: Principles with Applications, 6 th edition Giancoli

A few grams of matter in a bright world

NEUTRINO ASTRONOMY AT THE SOUTH POLE

The Discovery of the Higgs boson Matthew Herndon, University of Wisconsin Madison Physics 301: Physics Today. M. Herndon, Phys

The first one second of the early universe and physics beyond the Standard Model

Ultra-high energy cosmic rays from annihilation of superheavy dark matter

Ultra High Energy Cosmic Rays

Dark Matter in the Universe

High Energy Particle Production by Space Plasmas

STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE

PoS(ICRC2017)933. Cosmic rays and new fermionic dark matters. Jae-Kwang Hwang 1

Cosmic Background Radiation

IceCube: Ultra-high Energy Neutrinos

Detection of Cosmic Rays at Ultra-High Energies with Phase I of the Square Kilometre Array (SKADS) Olaf Scholten and Heino Falcke

Mass Composition Study at the Pierre Auger Observatory

Ultra-High-Energy Cosmic Rays: A Tale of Two Observatories

Lecture 03. The Standard Model of Particle Physics. Part III Extensions of the Standard Model

Project Paper May 13, A Selection of Dark Matter Candidates

OVERVIEW OF THE RESULTS

arxiv: v1 [astro-ph] 14 Nov 2007

MONOPOLE NON-ANNIHILATION AT THE ELECTROWEAK SCALE NOT!

Lorentz Invariance Violation: from theoretical and phenomenological perspectives

IceCube. francis halzen. why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector

UHECR and HADRONIC INTERACTIONS. Paolo Lipari Searching for the origin of Cosmic Rays Trondheim 18th June 2009

Astro-2: History of the Universe

Loop quantum gravity and ultrahigh energy cosmic rays

Transcription:

arxiv:astro-ph/0008525 v1 31 Aug 2000 Comparison of UHECR spectra from necklaces and vortons Luis Masperi and Milva Orsaria Centro Latinoamericano de Física, Av. Vencenslau Bráz 71 Fundos, 22290-140 Rio de Janeiro, Brazil Abstract Cosmic rays of energy higher than 10 19 ev may be explained by topological defects produced in the early stages of universe. Two suitable alternatives are: necklaces formed by magnetic monopoles connected by strings, and vortons which are loops stabilized by superconducting currents. The former are uniformly distributed in the universe, may account for cosmic rays above the ankle, suffer a transient GZK cutoff with a subsequent recovery and isotropy of observations is expected. The latter are concentrated in the galactic halo, require an additional extragalactic contribution between the ankle and the GZK cutoff, beyond which give a harder component and predict anisotropy related to mass concentration. PACS: 98.70.S, 98.80.C 1 Introduction The ultra-high energy cosmic rays (UHECR) have an energy spectrum of their flux F(E) that shows for E 3 F(E) a minimum around 5 x 10 18 ev which Presented at the Chacaltaya Meeting on Cosmic Rays Physics, La Paz, 23-27 July 2000 On leave of absence from Centro Atómico Bariloche, Argentina. E-mail: masperi@cbpf.br E-mail: orsaria@cbpf.br 1

is called the ankle, then a maximum before the GZK cutoff[1] at 5 x 10 19 ev due to the interaction with the CBR and a recovery after it at 10 20 ev. Whereas the cosmic rays below the ankle are most probably of galactic origin, it is not clear which is the explanation of the subsequent rise. The possibility that it is due to an extragalactic source seems to be supported by a partial GZK cutoff which would affect cosmic rays traveling at least 50Mpc. But the subsequent observed spectrum up to the highest energy event of 3 x 10 20 ev indicates a hard component which may be or not related to that which appears above the ankle. It is difficult to explain the observed events[2] beyond the GZK cutoff with ordinary astrophysical objects which are not identified if they are close to us, and that would require non standard messengers not interacting with CBR if they are very far away[3]. A solution may be the top-down mechanism where some type of superheavy microscopical object with mass of the order of the Grand Unification Theory (GUT) scale decays very slowly producing the observed UHECR. Since a general feature is a hard spectrum at emission F(E em ) 1/E em, these superheavy objects might be either condensed in the galactic halo or uniformly distributed in the universe. The former case may correspond to closed cosmic strings stabilized by superconducting currents called vortons[4] or to superheavy particles whose interaction with the ordinary ones is of gravitational order generically denoted as cryptons[5]. Since they were presumably produced at the GUT scale, they behave afterwards as cold dark matter (CDM) and should have concentrated in the galactic halo. The latter case may be instead represented by necklaces[6] where ordinary cosmic strings whose dynamics makes them evolve to a scaling solution, i.e. a uniform distribution in space, incorporate monopoles and antimonopoles that annihilate very slowly. We will give a brief description of vortons and particularly show that if they represent a small fraction of the halo CDM, they may account for the apparent hard component of the UHECR spectrum above 10 20 ev. An additional extragalactic component would be necessary to explain the ankle feature. Compared to this, an also small fraction of the critical density of universe represented by necklaces may give, with a reasonable law for the energy degrading due to interaction with CBR, the maximum of E 3 F(E) immediately below the GZK cutoff. The hard spectrum at emission allows a recovery 2

above it at least up to the highest observed UHECR which would be impossible for extragalactic sources with the ordinary law F(E em ) 1/E 3 em. 2 Vortons in halo. Considering sources that emit n X (t) GUT boson particles X per unit space and time, each of them giving N c UHECR, the total flux on earth will be F = 1 ( ) t0 3. a(t) dt N c n X (t), (1) 4π t in a(t 0 ) where a is the scale parameter of universe, t 0 its age and t in the initial time of contributions. For quasistable objects like vortons concentrated in halo with density n(t). which emit by tunneling an X with a lifetime τ, n X = n/τ and the total flux is F h = N c 4π n h(t 0 ) t τ, (2) where t 50kpc is the halo size. The energy spectrum F h (E) = 1 4π n h(t 0 ) t τ N c δ(e E i ) (3) i=1 must be averaged on the intervals E i between produced particles to compare with observations F h (E i ) = 1 n h (t 0 ) t E i 4π τ. (4) Since the production of UHECR comes from the hadronization of the very energetic quark into which the X particle decays, by dimensional arguments there are no relevant ordinary mass parameters and we may expect E i E i, F h (E i ) 1 E i, (5) i.e. a hard spectrum consistent with accurate QCD calculations[7] apart from energies close to m X. 3

It is interesting that according to Eq.(5) the average probability of UHECR production on energy intervals will be dγ de 1 τ 1 E, (6) which integrated on the ultra-high energy range 10 19 10 24 ev to agree with the total flux Eq.(2) must give Γ = dγ de de = N c τ, (7) with N c 10, that is a reasonably accepted value[8]. Therefore we may take the equally spaced particles in log E according to E 1 10 19 ev, E 2 10 19.5 ev, E 3 10 20 ev, E 4 10 20.5 ev...e 10 10 23.5 ev so that E i 0.7E i. Since from eq.(4) the flux in each energy bin is the same, one may normalize it roughly at the expected value for 10 20 ev n h (t 0 ) 4π t τ = 1 km 2 century. (8) A vorton is a loop of ordinary cosmic string with an energy per unit length µ m 2 X stabilized by N massless fermionic carriers giving therefore a total energy E v = µl + N2 L, (9) which is minimized at E v 2Nm X by a length L N/m X. The decay of the vorton with emission of X by tunneling gives a lifetime τ t 0 for N 1000. Therefore to satisfy Eq.(8) one only needs a fraction 10 6 of the average energy density of the halo 0.3 GeV/cm 3 represented by vortons. This small density may be the remnant of the collapse of most vortons at the electroweak phase transition[8]. This contribution of vortons to E 3 F(E) will be a hard component which reproduces the observed flux above the GZK cutoff as is seen in fig.1. One must therefore complement it with another possibly extragalactic component which may explain the spectrum between the ankle and GZK energy. A similar analysis may be done for cryptons being necessary to explain their required density. 4

3 Necklaces in universe These hybrid topological defects may be formed by a sequence of GUT symmetry breakings G H x U(1) H x Z 2, (10) where in the first monopoles would be produced and then would be attached to the ordinary strings which appear in the second one as beads of a necklace. The relevant parameter for the necklace dynamics is r = m/(µd) where m is the monopole mass, d its separation from the antimonopole in the string and µ the tension of the latter. For r 10 6 the distance between strings at present is small 3Mpc. The evolution of the necklace networks is scale invariant, i.e. they would be distributed uniformly in the universe and represent a constant fraction of its energy. Monopoles and antimonopoles trapped in the necklaces at the end would annihilate producing X particles with a rate. n X (t) r2 µ = α t 3 m X t (11) 3 Therefore the expression for the UHECR flux eq.(1) would apply but with an early t in compatible with avoiding their redshift below 10 19 ev which is roughly of the order of the matter-radiation equivalence time. r 2 µ cannot be larger than 10 28 GeV 2 to avoid a diffuse gamma radiation above the experimental bound. The total flux will be F u = N c α t 2 0 ln ( ) t0 t in (12) Even though at emission the UHECR produced by an X are equally spaced in log E em as discussed in Sec.2, their redshift would cause a softening of the law 1/E for the flux spectrum on earth. But more important than this effect is the interaction of cosmic rays with CBR. The pγ total cross-section at the highest energy is 0.2 mb, and rises up to 0.6 mb for the resonance mass. Then to evaluate the flux spectrum, we may proceed as follows. Instead of taking one cosmic ray in each bin as in the case of vortons in halo, we will consider N i to account for the degrading of energy so that F U (E i ) = α t 2 0 ( ) t0 Ni ln (13) t in E i 5

Therefore we may parameterize for all cases log [ Ei 3 F(E i) ] ( ) Ei = log J + log N i + 2 log 10 19 ev, (14) where J, related to the properties of sources, will be adjusted to fit the observed events. For the case of vortons all N i = 1. For necklaces to determine the effective N i and considering the mean free path associated to the quoted σ pγ and the density of 3K photons, we will take 1% of probability that the cosmic ray for production keeps its energy. This is consistent with the fact that the sources of non degrading protons are concentrated in a radius 50Mpc out a whole space 100 times larger. For higher E i this probability will increase to 3% following σ pγ. We will assume that the missing events are transferred in equal parts to the two inmediate lower bins. According to the bins defined in Sec.2, that of E 3 is particularly affected by the resonant scattering. The inmediate lower one has only the upper 10% of the bin in the resonance region so that 90% of its events keep their energy and the rest is transferred to the bin of E 1. In this way it turns out N 1 = 4.09 N 2 = 5.15 N 3 = 0.05 N 4 = 0.14 N 5 = 0.12 N 6 = 0.10 N 7 = 0.08 N 8 = 0.06 N 9 = 0.04 N 10 = 0.03 and the flux spectrum eq.(14) is shown in fig.2. We see that the existence of an ankle and the recovery after a transient GZK are successfully reproduced. A check of the calculation is that the normalization for the bin of 10 19 ev must be α t 2 0 ( ) t0 ln t in N 1 = 1 km 2 yr, (15) which is satisfied for α = 10 37 sec 1 coming from m X = 10 15 GeV. This is similar to the normalization for ordinary strings[9] the difference being that for them µ m 2 X and the present separation between strings is three orders of magnitude larger than for necklaces. As a consequence our simplified treatment is much more suitable for the latter because protons for sources within a radius 50Mpc would be detected whereas photons would be mostly absorbed. It is clear that the feature of fig.2 is consequence of the hard component corresponding to quark hadronization reflected in the last term of eq.(14). If one should have considered an ordinary law 1/E 3 at emission, the corresponding flux due to uniformly distributed extragalactic sources would be 6

given by eq.(14) without the last term and as shown in fig.3 would reasonably reproduce the observed events below the GZK cutoff but without recovery above it. We must note comparing figs. 1 and 2 that J is one order of magnitude larger for necklaces than for vortons which is consequence of the fact that the latter fit the flux at 10 20 ev and the former that at 10 19 ev with a partial compensation due to degrading of energy. It is important to note that with the above values of r, µ and a monopole mass m 10 16 GeV the energy per unit length due to monopoles turns out to be 10 22 GeV 2 and the fraction of critical density 10 9, slightly smaller than that of ordinary strings. 4 Conclusions We have seen that both vortons in halo and necklaces in universe may be a solution for the problem of UHECR above 10 20 ev. From the observational point of view the difference will be the expected anisotropy in the former case because of the asymmetric position of the sun in the galaxy compared to the isotropy of the latter characteristic of a cosmological origin. Regarding this, it must be noted that the anisotropy detected below the ankle is not observed above it[10], which would be consistent with the appearance of an extragalactic component, a larger statistics being needed at the highest energy to see if new galactic sources contribute. Referring to elementary particle theory it is interesting that the most appropriate GUT models are different. For necklaces, since it is necesary that the breaking of the abelian symmetry leaves a discrete Z 2 unbroken, a GUT model based on SO(10) is suitable. For vortons on the other hand the E 6 GUT model is better because the breaking of the contained additional abelian symmetry produces the necessary superconducting current with exotic fermions, whereas necklaces would not be formed due to the fact that its Higgs content does not allow an unbroken Z 2. Acknowledgement We are grateful to Pedro Miranda and the organizing committee of the Chacaltaya Meeting on Cosmic Rays Physics for the warm hospitality at La Paz. MO thanks Fundación Antorchas for partial financial support. 7

References [1] K. Greisen, Phys. Rev. Lett. 16 (1966) 798; G. Zatsepin and V. Kuzmin, JETP Lett. 4 (1966) 78; F. Aharonian and J. Cronin, Phys. Rev. D 50 (1994) 1892. [2] M. Takeda et al., Phys. Rev. Lett. 81 (1998) 1163; D. J. Bird et al., Astropart. Phys. 441 (1995) 144. [3] A. V. Olinto, astro-ph/0002006; V. Berezinski, astro-ph/0001163. [4] R. L. Davis and E. P. S. Shellard, Nucl. Phys. B 323 (1989) 209; R. Brandenberger, B. Carter, A. C. Davis and M. Trodden, Phys. Rev. D 54 (1996) 6059. [5] V. A. Kuzmin and V. A. Rubakov, Yadern. Fiz. 61 (1998) 1122, V. Berezinsky, M. Kachelriess and A. Vilenkin, Phys. Rev. Lett. 79 (1997) 4302; K. Hamaguchi, Y. Nomura and T. Yanagida, Phys. Rev. D 59 (1999) 063503; R. Benakli, J. Ellis and D. V. Nanopoulos, Phys. Rev. D 59 (1999) 047301. [6] V. Berezinski and A. Vilenkin, Phys. Rev. Lett. 79 (1997) 5202; V. Berezinski, P. Blasi and A. Vilenkin, Phys. Rev. D 58 (1998) 103515. [7] M. Birkel and S. Sarkar, Astropart. Phys. 9 (1998) 297. [8] L. Masperi and M. Orsaria, Int. J. Mod. Phys. A 14 (1999) 3581. [9] P. Bhattacharjee, Phys. Rev. Lett. 81 (1998) 260. [10] M. Takeda et al., astro-ph/9902239. 8

27 arxiv:astro-ph/0008525 v1 31 Aug 2000 log ( E 3 F (E) [ ev 2 /(m 2 s sr ) ] ) 26 25 24 23 22 18.5 18,5 19.0 19,0 19.5 19,5 20.0 20,0 20.5 20,5 21.0 21,0 log ( E [ ev ] ) Fig.3. Ordinary extragalactic component. Broken line is drawn to help the eye since points are calculated from eq.(14) without the last term due to F(E) 1/E 3, with N i of sec.3 and log J = 24. 11

27 26 arxiv:astro-ph/0008525 v1 31 Aug 2000 log ( E 3 F(E) [ ev 2 /(m 2 s sr) ] ) 25 24 23 22 18.5 18,5 19.0 19,0 19.5 19,5 20.0 20,0 20.5 20,5 21.0 21,0 log ( E [ ev ] ) Fig.2. Necklaces in universe. Broken line es drawn to help the eye since points are calculated from eq.(14) with N i of sec.3 obtained degrading energy and log J = 23.5 10

27 26 arxiv:astro-ph/0008525 v1 31 Aug 2000 log ( E 3 F(E) [ ev 2 /m 2 s sr ] ) 25 24 23 22 18.5 18,5 19.0 19,0 19.5 19,5 20.0 20,0 20.5 20,5 21.0 21,0 log ( E [ev] ) Fig.1. Vortons in halo. Hard component comes from eq.(14) with N i = 1 and log J = 22.5. Observed data are from AGASA and from Fly s Eye. 9