CBPF-NF-41/3 1 1 Introduction The inelasticity is a global parameter of hadronic interactions it is a crucial attribute in the calculation of the flux

Size: px
Start display at page:

Download "CBPF-NF-41/3 1 1 Introduction The inelasticity is a global parameter of hadronic interactions it is a crucial attribute in the calculation of the flux"

Transcription

1 CBPF-NF-41/3 ESTIMATIVE OF INELASTICITY COEFFICIENT FROM EMULSION CHAMBER DATA H M PORTELLA Instituto de F sica, Universidade Federal Fluminense, Av. Litor^anea s/n, Gragoatá, , Niterói, RJ, Brazil LCSdeOLIVEIRACECLIMA Centro Brasileiro de Pesquisas F sicas, Rua Dr. Xavier Sigaud 15, Urca, , Rio de Janeiro, RJ, Brazil Abstract Atmospheric diffusion of high energy cosmic rays is studied analytically the obtained integral electromagnetic fluxes are compared with the data measured by emulsion chamber detectors at mountain altitudes. We find a good consistency between them when the average nucleon inelasticity coefficient is varying between Key-words:Inelasticity; Hadrons; Emulsion Chambers; Electromagnetic Cascades; Inelastic Cross Section; Z-factors. PACS: Tp; Hd

2 CBPF-NF-41/3 1 1 Introduction The inelasticity is a global parameter of hadronic interactions it is a crucial attribute in the calculation of the fluxes in cosmic ray cascades. It is defined as the fraction of energy giving up by the leading hadron in a collision induced by an incident hadron on a target nucleon or nucleus. The inelasticity, K N, in a nucleon-induced interaction is related to the spectrumweighted moments evaluated at fl = 1 (where fl is the power index of primary spectrum) as 1 K N = Z NN (fl =1)= f NN ( ) d. Several authors have suggested that the average inelasticity-coefficient is an increasing function of the energy [1, 2], whereas others proposed that it is a decreasing function [3, 4, 5]. The behaviour of high energy cosmic rays, which reflects the nuclear interactions in the energy region 1 ο 1 TeV, indicates a constant value of the mean inelasticity equal to.5 [6]. A decreasing with energy of this parameter points out a strongly suppression of the pion production in this energy region does not agree with cosmic ray observations. The objective of this paper is to estimate the average inelasticity coefficient through the comparison of our calculations with the integral electromagnetic fluxes measured with large Emulsion Chamber Experiments at mountain altitudes. The main purpose is to describe in qualitative detail single events, i.e., shower cores in their early stage of development observed at mountain altitudes. Our calculation is performed by solving analitically the cosmic ray diffusion equations for electromagnetic showers in earth's atmosphere. In these calculations we adopt to the particle production an approximated Feynman scaling in the fragmentation region. We have used the data on proton targets on nuclear targets [7] to obtain the pion spectrum weighted moments. Although exist several functional forms to fit the behaviour of rising cross-section we assume the following one ff = ff (E=ffl) ff. So, beginning with the measured all-particle primary spectrum we diffuse the particle showers down to the detection depths we investigate our numerical results as a function of the adopted average inelasticity coefficient. 2 Hadronic electromagnetic cascades in the Earth's atmosphere The differential hadronic fluxes, H(t; E) at a depth t in the energy range E E + de are obtained integrating the nucleon pion diffusion equations using the semigroup theory. We

3 CBPF-NF-41/3 2 assume that only the pions are generated in the multiparticle production neglecting the particles with small fractions such askaons, heavy mesons, etc.. In this case the solutions are [8]; 1X ( 1) n t Y n N(t; E) = (1 Z NN (fl;ff; n)) N(;E) (1) n! n= N (E) n i=1 with Z NN (fl; ff) = f NN ( ) fl iff d (2) where is the elasticity coefficient of the nucleons in the atmosphere that is distibuted according to f NN ( ). with The pionic fluxes are Π(t; E) = 1X 1X m= n= ny i=1 Z t dz ( 1)m ( 1) n m! n! (1 Z NN (fl; ff; n)) Z ßß (fl; ff;m;n) = Z Nß (fl;ff; n) = my j=1 t z m z n Z Nß (fl;ff; n) ß (E) N (E) (1 Z ßß (fl; ff; m; n)) N(;E) N (E) (3) f ßß (x) x fl ff(j+n+1) dx (4) f Nß (x) x fl ff(n+1) dx. (5) The f Nß (x) f ßß (x) are the energy spectra of the pions produced in the nucleon-air in the pion-air interactions respectively, x is the Feynman variable (x =2p L = p S). The solutions (1) (3) are subjected to the boundary conditions N(;E)=N E (fl+1) (6) Π(;E)= (7) that represents the nucleon pion fluxes at the top of atmosphere. The above solutions are obtained considering the interaction mean-free paths in the power form, H (E) = H E ff (H = N or ß). Using naive approximations [9] we can write the solutions (1) (3) in the following forms N(t; E) =N(;E) e t! N (E) (8)! Nß (fl;e) Π(t; E) =N(;E)! N (E)! ß (E) e t!ß(e) e t! N (E) The! N (E),! ß (E) the! Nß (fl; E) functions are described in the appendix A.. (9)

4 CBPF-NF-41/3 3 The production rate of fl-rays originated from the ß decay isgiven by [1] de P fl (z; E fl )=2 2E P ß± N air + P ß± air ß± E fl (1) where P N air ß± P ß± air ß± are the production rate of the charged pions from the nucleon-air pion-air interactions are represented by P H air ß± = H(z; E ) H (E ) f Hß(x) dx x ; H = N or ß. (11) In the expression (1) we have used that the secondary pions are formed with equal multiplicity, so the number of ß is half of the number of charged pions. The differential flux of the electromagnetic component can be written as Z t F fl;e (t; E) = dz de fl P fl (z; E fl )(e + fl)(t z; E fl ;E) (12) E where (e+fl)(t z; E fl ;E) are the photons, electrons positrons produced by a single photon. They are computed using the approximation A [11] are written in the following form (e + fl)(t z; E fl ;E)= 1 2ßi Z C s Efl 1 E E N 1 (s)e 1(s)(t z)=x + N 2 (s)e 2(s)(t z)=x. (13) The functions N i (s), i (s) X are the parameters with stardized definitions in cascade theory [11]. These functions the evaluation of the electromagnetic fluxes are presented in the appendix B. In order to compare our calculations for electromagnetic showers with the emulsion chamber data measured at mountain altitudes we need to obtain the integral fluxes of this component. They are, F fl;e (t; E) = 3 Comparison with experimental data E F fl;e (t; E) de (14) Emulsion Chamber Experiments at mountain altitudes are very simple detectors constituted of multiple swich of material layers (Pb, Fe, etc.) photo-sensitive layers (X-ray films, nuclear emulsions plates, etc.). They can detect electromagnetic showers of high energy (E e;fl 1 TeV) due to its powerful spatial resolution energy determination they can study in details the cosmic-ray interactions. The experimental data are taken from J. R. Ren et al. [19] for Mt. Kanbala; C. M. G. Lattes et al. [13] for Mt. Chacaltaya M. Amenomori et al. [21] for Mt. Fuji. The experimental fluxes at Mt. Chacaltaya are revised according to the energy determination introduced by M.Okamoto T. Shibata [22] where the LPM spacing effects were taken

5 CBPF-NF-41/3 4 into account. This revision followed the same procedure made by N.M. Amato N. Arata [2] for determination of total hadron fluxes. In order to make a comparison with electromagnetic fluxes measured with these detectors it is necessary to check the main assumptions made in our calculations; a) Primary cosmic-ray radiation The energy spectra obtained by Emulsion Chamber Experiments at mountain altitude are in the region of 3 ο 5 TeV for (e; fl) component 3 ο 4 TeV for hadronic shower. So, we need to include in our calculations the primary spectrum up to knee (ß 1 15 ev). In the present work we assume the primary cosmic-ray radiation in integral form reported by J. Belli Filho et al. [14] from JACEE data [15]. N 1 (; E) =1: (E=5TeV) 1:7 (/cm 2.s.st) (15) where E(TeV/nucleus). Nucleonic intensity att =, equivalent to primary cosmic-ray radiation is given by N(; E) =A 1 fl N 1 (; E) (16) where A is the average mass number of cosmic ray nuclei; we adopta =14: which is the value in low energy region (E/part < 1 14 ev). b) Collision mean free paths We use to fit the behaviour of rising with energy of the p-air inelastic cross-section the following form [7, 14, 16, 17], ff N (E) =ff N (E=TeV) ff (17) with ff N = 3 mb ff =:6 [7, 14]. So, the collision mean free path of the nucleon in the earth's atmosphere is expressed by N (E) = N (E=TeV) ff (18) with N = 8 g/cm 2 [7, 14]. For the pion mean free paths we assume that ß = N ß 1:4 that they have the same energy dependence, like inthenucleon case [14]. Thus, we have ß (E) = ß (E=TeV) ff (19) with ß = 112 g/cm 2. c) Secondary pions:

6 CBPF-NF-41/3 5 The functions f Nß (x) f ßß (x) are the energy distribution of secondary nucleons pions for nucleon-air pion-air interactions, respectively. We have used in this calculation the data on proton targets on nuclear targets [7] to obtain these functions they are written as f Nß (x) =2:8 (1 x) x e 5x (2) f ßß (x) = 2:6 x 1+ x 3 + :32 :45 x e2(x 1) (21) these functions are for two charged states of pions the contribution of leading pions are taken into account in the last one. Figures 1-3 show the comparison of our solution with the integral electromagnetic fluxes measured at Mt. Kanbala (52 g/cm 2 ), Mt. Chacaltaya (54 g/cm 2 ) Mt. Fuji (65 g/cm 2 ), respectively. Two curves are also drawn in the figures for <K N > =.5.65, taking into account the above mentionated itens. 4 Conclusions We have solved the diffusion equations of cosmic-ray hadrons analytically after this we derived the integral electromagnetic fluxes using the approximation A of the electromagnetic cascade theory. These fluxes at mountain atmospheric depths decrease when we include in our calculation the rising of the cross-section the decreasing of the mean nucleon elasticity. We conclude that the naive assumptions for the secondary production based on approximate scaling in the fragmentation region is possible to explain experimental data on integral electromagnetic fluxes detected in large emulsion chamber experiments. This scenario requires a mean nucleon inelasticity coefficient varying from.5 to.65. At low energy (few TeV) the agreement between experimental data the calculated fluxes shows that <K N >ß :5, that is the adjust indicated by former workers in the cosmic ray literature. For E > 1 TeV we see from the figure that < K N >ß :65. Therefore, with this simple analysis we see that the nucleon inelasticity coefficient appears to show a tendency of rising with energy according to Mini-jet Models [17] Quark-Gluon String Models [2]. These integral fluxes are somewhat affected when the coefficient ff changes in the interval.6 to.1, which is the appropriated values to explain the experimental data for mountain emulsion chambers experiments. In the latter the fit between our calculation the experimental data is obtained for < K N > changing between approximately These results are in agreement with that of L. Jones [18] based in an analysis on inclusive reactions data from accelerator, with analytical calculations on nucleon fluxes at sea level [9] with hadron electromagnetic fluxes at mountain altitudes [8, 1].

7 CBPF-NF-41/3 6 Appendix A Hadronic cascades where The functions! N (E),! ß (E) Z Nß (fl; E) in the hadronic fluxes (8) (9) are [9] Z NN(fl) 1 2 Z NN(fl; ff)! N (E) =! N E :6 = 1 N (E)! ß (E) =! ß E :6 = 1 ß (E)! Nß (E) = Z Nß(fl;ff) N (E) Z NN (fl; ff) = Z ßß (fl; ff) = Z ßß(fl) 3 2 Z ßß(fl;ff) = 1 N (E) (22) (23) x fl ff f Nß (x) dx (24) fl ff f NN ( ) d (25) x fl ff f ßß (x) dx. (26) The functions f Nß (x) f ßß (x) are the energy distribution of secondary nucleons pions for nucleon-air pion-air interactions, respectively (see item c of section 3). The nucleon elasticity distribution is assumed to be [9] where f NN ( ) =(1+fi)(1 ) fi (27) = E=E fi fulfills a consistency relation between the mean elasticity average inelasticity, so that < N > + < K > = 1, for nucleons. When fi = we have the nucleon uniform distribution of elasticity (< > = :5). Appendix B Electromagnetic cascades The production rate of fl-rays produced from ß decay expression (1) can be written as P fl (z; E fl )= N E (fl+1 ff+z ff! N ) fl e z! N ZNß (fl ff + zff! N ) Z ßß(fl ff + zff! N ) fl +1 ff + zff! N N ß! Nß (E) + N E (fl+1 ff+zff!ß)! N (E)! ß (E) (fl +1 ff + zff! ß ) The Z-factors Z Nß Z ßß is the last expression are! Nß (E)e z!ß Z ßß (fl ff + zff! ß ) (! N (E)! ß (E)) ß. (28) Z Nß (fl ff + zff! N )= x fl ff+zff! N f Nß (x)dx (29)

8 CBPF-NF-41/3 7 Z ßß (fl ff + zff! i )= The expression (28) was obtained considering the expansion x fl ff+zff! i f ßß (x) dx i = N or ß. (3) 1 H (E) = 1+ffln(E=E ) H ; H = N or ß (31) The differential flux of the electromagnetic component (12) is obtained from this production rate evaluated at the poles s 1 = fl ff + zff! N s 2 = fl ff + zff! ß. The integral flux is put in the form F fl;e (t; E) =F fl 1;e(t; E)+F fl 2;e(t; E) (32) with F fl 1;e(t; E) = F fl 2;e(t; E) = where with Z t Z t dz N E s1 e z! N s 1 (s 1 +1) dz N E s2 e z!ß s 2 (s 2 +1) N 1 (s 1 )e 1(s1)(t z)=x + N 2 (s 1 )e 2(s1)(t z)=x C 1 (s 1 ) N 1 (s 2 )e 1(s2)(t z)=x + N 2 (s 2 )e 2(s2)(t z)=x C 2 (s 2 ) (33) (34) C 1 (s 1 )= Z Nß(s 1 )! Nß (E) Z ßß (s 1 ) (35) N (! N (E)! ß (E)) ß C 2 (s 2 )= Z Nß (s i )= Z ßß (s i )=! Nß (E) Z ßß (s 2 ) (36) (! N (E)! ß (E)) ß x s i f Nß (x) dx (37) x s i f ßß (x) dx. (38) The functions N i i are the usual parameters with definitions in cascade theory can be obtained in the reference [11]. X is the radiation length in the atmosphere (X = 37:1g/cm 2 ).

9 CBPF-NF-41/3 8 References [1] J. D. de Deus, Phys. Rev. D32 (1985) [2] A. B. Kaidalov K. A. Ter-Martyrosian, Phys. Lett. B117 (1982) 247; A. B. Kaidalov K. A. Ter-Martyrosian, Sov. J, Nucl. Phys. 4 (1984) 135. [3] G. N. Fowler et al., Phys. Rev. D35 (1987) 87; G. N. Fowler et al., Phys. Rev. C4 (1989) [4] A. Ohsawa K. Sawayanagi, Phys. Rev. D49 (1992) [5] Z. Wlodarczyk et al., J. Phys. G 21 (1995) 281. [6] C. R. A. Augusto et al., Phys. Rev. D61 (1999) 123; A. Ohsawa, Prog. Theor. Phys., 92 (1994) 15. [7] H. M. Portella, PhD Thesis (CBPF: Centro Brasileiro de Pesquisas F sicas, Brazil), (1989). [8] H. M. Portella, N. Amato, R. H. C. Maldonado A. S. Gomes, J. Phys. A: Math. Gen. 31 (1998) [9] J. Belli Filho et al., Il Nuovo Cimento A11 (1989) 897. [1] H. M. Portella et al., ICRR-Report Institute for Cosmic Ray Research, University oftokyo (1999) 31. [11] J. Nishimura, Hbuch Der Physik (Reading: Springer-Verlag) (1967) 1. [12] M. Akashi et al., Il Nuovo Cimento A65 (1981) 355. [13] C. M. G. Lattes et al., Proc. 13 th Int. Symp. on Very High Energy Cosmic Ray Interactions (Denver) 13 (1973) [14] J. Belli Filho et al., Prog. Theor. Phys. 83 (199) 58. [15] T. H. Burnett et al. (JACEE Collaboration), Proc. of the Int. Symp. on Cosmic Ray particle Physics (ICRR, Univeristy oftokyo) (1984) 468. [16] B. Z. Kopeliovich et al., Phys.Rev. D39 (1989) 769. [17] T. K. Gaisser, Cosmic Ray Particle Physics (Cambridge: Cambridge University Press), (199). [18] L. W. Jones, Proc. of 2 th Int. Symp. on Very High Energy Cosmic Ray Interactions (La Paz-Rio de Janeiro) (1982) 1. [19] J. R. Ren et al., Nuovo Cimento 1C (1987) 43. [2] N. M. Amato N. Arata, Proc. 5 th Int. Symp. on Very High Energy Cosmic Ray Interactions (Lodz) (1988) 49. [21] M. Amenomori et al., Proc. 18 th Int. Cosmic Ray Conf. (Bangalore) 11 (1983) 57. [22] M. Okamoto T. Shibata, Nucl. Inst. Meth. A257 (1987) 155.

10 CBPF-NF-41/3 9 Figure Captions Figure 1 - Integral electromagnetic spectrum at Mt. Kanbala (52 g/cm 2 ). The full lines represent the calculated flux for <K N >=:65 the dashed lines for <K N >=:5. All lines are for ff =:6. The experimental data are taken from J. R. Ren et al. [19]. Figure 2 - Integral electromagnetic spectrum at Mt. Chacaltaya (54 g/cm 2 ). The full lines represent the calculated flux for <K N >=:65 the dashed lines for <K N >=:5. All lines are for ff =:6. The experimental data are taken from C. M. G. Lattes et al.(black dots) [13]. Figure 3 -Integral electromagnetic spectrum at Mt. Fuji (65 g/cm 2 ). The full lines represent the calculated flux for <K N >=:65 the dashed lines for <K N >=:5. All lines are for ff =:6. The experimental data are taken from M Amenomori et al. [21].

11 CBPF-NF-41/3 1

12 CBPF-NF-41/3 11

13 CBPF-NF-41/3 12

Hadronic Interaction Studies with ARGO-YBJ

Hadronic Interaction Studies with ARGO-YBJ Hadronic Interaction Studies with ARGO-YBJ Ivan De Mitri University of Salento and Istituto Nazionale di Fisica Nucleare Lecce, Italy On behalf of the ARGO-YBJ Collaboration Hadron-Hadron & Cosmic Ray

More information

Detection of high energy electromagnetic and hadron components of air-shower cores in the new hybrid experiment Pamir-XXI

Detection of high energy electromagnetic and hadron components of air-shower cores in the new hybrid experiment Pamir-XXI EPJ We of Conferences 145, 15001 (2017) Detection of high energy electromagnetic and hadron components of air-shower cores in the new hyrid experiment Pamir-XXI M. Tamada 1,a, N. Inoue 2, A. Misaki 2,

More information

Charged Current Quasielastic Analysis from MINERνA

Charged Current Quasielastic Analysis from MINERνA Charged Current Quasielastic Analysis from MINERνA Anushree Ghosh CBPF - Centro Brasileiro de Pesquisas F sicas, Rua Dr. Xavier Sigaud 150, Urca, Rio de Janeiro, Rio de Janeiro, 22290-180, Brazil on behalf

More information

Cosmic-ray energy spectrum around the knee

Cosmic-ray energy spectrum around the knee Cosmic-ray energy spectrum around the knee M. SHIBATA Department of Physics, Yokohama National University, Yokohama, 240-8501, Japan Interesting global and fine structures of cosmic-ray energy spectrum

More information

PROTON AND LIGHT ION INTERACTIONS IN COSMIC RAY EXPERIMENT STRATOSPHERE IN THE COMPARISON WITH THE RECENT COLLIDER RESULTS

PROTON AND LIGHT ION INTERACTIONS IN COSMIC RAY EXPERIMENT STRATOSPHERE IN THE COMPARISON WITH THE RECENT COLLIDER RESULTS PROTON AND LIGHT ION INTERACTIONS IN IN THE COMPARISON WITH THE RECENT COLLIDER RESULTS A.Kh. Argynova a, N.I. Kochelev b, T.N. Kvochkina c, A.A. Loktionov a,t.kh. Sadykov a, N.N. Zastrozhnova a, a, S.Zh.

More information

TeV energy physics at LHC and in cosmic rays

TeV energy physics at LHC and in cosmic rays Vulcano 2016 TeV energy physics at LHC and in cosmic rays Anatoly Petrukhin National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia Many physicists dream and hope to find

More information

Cosmic Ray Interaction Models: an Overview

Cosmic Ray Interaction Models: an Overview EPJ Web of Conferences will be set by the publisher DOI: will be set by the publisher c Owned by the authors, published by EDP Sciences, 2016 Cosmic Ray Interaction Models: an Overview Sergey Ostapchenko

More information

Threshold Photo-production of J/5 Mesons J. Dunne Jefferson Lab

Threshold Photo-production of J/5 Mesons J. Dunne Jefferson Lab hreshold Photo-production of J/5 Mesons J. Dunne Jefferson Lab Introduction With the advent of higher energies at Jefferson Lab, the study of charmonium becomes possible. he threshold production of J/5

More information

arxiv: v1 [hep-ex] 18 May 2015

arxiv: v1 [hep-ex] 18 May 2015 ALICE summary of light flavour results at intermediate and high p arxiv:55.477v [hep-ex] 8 May 5 uva Richert, on behalf of the ALICE collaboration Lund University, Department of Physics, Div. of Particle

More information

Energy Spectrum of all Electrons and Positron Fraction

Energy Spectrum of all Electrons and Positron Fraction Energy Spectrum of all Electrons and Positron Fraction Dr. Rena Majumdar Department of Physics Bhairab Ganguly College Kolkata-56, India renabkp021@gmail.com Abstract The absolute differential energy spectrum

More information

Abstract. Introduction

Abstract. Introduction The experimental feature on the data of the primary proton identification in stratospheric X-ray emulsion chambers at energies >10 TeV (RUNJOB experiment). Abstract. The RUNJOB balloon-born emulsion chamber

More information

Produced in nuclear processes (e.g. fusion reactions) Solar neutrinos and supernova neutrinos

Produced in nuclear processes (e.g. fusion reactions) Solar neutrinos and supernova neutrinos Sources of Neutrinos Low energy neutrinos (10 th of MeV) Produced in nuclear processes (e.g. fusion reactions) Solar neutrinos and supernova neutrinos High energy neutrinos (10 th of GeV) Produced in high

More information

arxiv: v1 [nucl-ex] 1 Dec 2007

arxiv: v1 [nucl-ex] 1 Dec 2007 Multiplicity and angular distribution of particles emitted in relativistic nuclear-nuclear interactions M. K. Suleymanov1, 2, E. U. Khan 1, A Kravchakova 3, Mahnaz Q. Haseeb 1,S. M. Saleem 1, Y. H. Huseynaliyev

More information

The atmospheric muon charge ratio: a probe to constrain the atmospheric ν µ / ν µ ratio

The atmospheric muon charge ratio: a probe to constrain the atmospheric ν µ / ν µ ratio The atmospheric muon charge ratio: a probe to constrain the atmospheric ν µ / ν µ ratio Nicoletta Mauri INFN - Sezione di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy DOI: http://dx.doi.org/.3204/desy-proc-2016-05/11

More information

The MINERnA Experiment

The MINERnA Experiment The MINERnA Experiment What is Minerna? Why Mienrna? n / n CCQE sections Inclusive n sections n beam and n flux Outlook INPC 2013 June 4 th 13 Alessandro Bravar for the Mienrna Collaboration The MINERnA

More information

Publications of Francesco Arneodo: journal articles

Publications of Francesco Arneodo: journal articles Publications of Francesco Arneodo: journal articles Figure 1: Citation report from ISI Web of Science (IF=31.0) [1] E. Aprile et al., First Axion Results from the XENON100 Experiment, arxiv.org (submitted

More information

The residual radioactivity of a water-copper beam dump for the TESLA Test Facility

The residual radioactivity of a water-copper beam dump for the TESLA Test Facility Internal Report DESY D3-92 November 1998 The residual radioactivity of a water-copper beam dump for the TESLA Test Facility A. Leuschner and K. Tesch Internal Report DESY D3-92 November 1998 The residual

More information

STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE

STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE I. BACIOIU * Institute of Space Science, P.O. Box MG-23, RO-077125 Bucharest-Magurele, Romania, E-mail: iuliana.bacioiu@spacescience.ro Abstract.

More information

Numerical study of the electron lateral distribution in atmospheric showers of high energy cosmic rays

Numerical study of the electron lateral distribution in atmospheric showers of high energy cosmic rays American Journal of Modern Physics 2013; 2(6): 287-291 Published online October 20, 2013 (http://www.sciencepublishinggroup.com/j/ajmp) doi: 10.11648/j.ajmp.20130206.13 Numerical study of the electron

More information

arxiv:hep-ph/ v1 25 Nov 1999

arxiv:hep-ph/ v1 25 Nov 1999 1 Narrow muon bundles from muon pair production in rock V. A. Kudryavtsev a, E. V. Korolkova b and N. J. C. Spooner a arxiv:hep-ph/9911493v1 25 Nov 1999 a Department of Physics and Astronomy, University

More information

Longitudinal profile of Nµ/Ne in extensive air showers: Implications for cosmic rays mass composition study

Longitudinal profile of Nµ/Ne in extensive air showers: Implications for cosmic rays mass composition study Iranian Journal of Physics Research, Vol. 13, No. 3, 2013 Longitudinal profile of Nµ/Ne in extensive air showers: Implications for cosmic rays mass composition study D Purmohammad Department of Physics,

More information

Emission of Helium Nuclei in Relativistic Proton Interactions Leading to Total Break up of Ag and Br Nuclei. Z.Physik A 279, 407 (1976).

Emission of Helium Nuclei in Relativistic Proton Interactions Leading to Total Break up of Ag and Br Nuclei. Z.Physik A 279, 407 (1976). Emission of Helium Nuclei in Relativistic Proton Interactions Leading to Total Break up of Ag and Br Nuclei. Z.Physik A 279, 407 (1976). Inelastic Interactions of 69.0 GeV/c Protons with Emulsion Nuclei.

More information

Constraints on the energy spectra of charged particles predicted in some model interactions of hadrons with help of the atmospheric muon flux

Constraints on the energy spectra of charged particles predicted in some model interactions of hadrons with help of the atmospheric muon flux Constraints on the energy spectra of charged particles predicted in some model interactions of hadrons with help of the atmospheric muon flux L G Dedenko 1,2, G F Fedorova 1, T M Roganova 1 1 Skobeltsyn

More information

High-p T Neutral Pion Production in Heavy Ion Collisions at SPS and RHIC

High-p T Neutral Pion Production in Heavy Ion Collisions at SPS and RHIC High- Neutral Pion Production in Heavy Ion Collisions at SPS and RHIC K. Reygers for the WA98 and the PHENIX collaboration Institut für Kernphysik der Universität Münster Wilhelm-Klemm-Str. 9, D-4849 Münster,

More information

energy loss Ionization + excitation of atomic energy levels Mean energy loss rate de /dx proportional to (electric charge) 2 of incident particle

energy loss Ionization + excitation of atomic energy levels Mean energy loss rate de /dx proportional to (electric charge) 2 of incident particle Lecture 4 Particle physics processes - particles are small, light, energetic à processes described by quantum mechanics and relativity à processes are probabilistic, i.e., we cannot know the outcome of

More information

Cosmic Rays. This showed that the energy of cosmic rays was many times that of any other natural or artificial radiation known at that time.

Cosmic Rays. This showed that the energy of cosmic rays was many times that of any other natural or artificial radiation known at that time. Cosmic Rays 1. Discovery As long ago as 1900, C. T. R. Wilson and others found that the charge on an electroscope always 'leaked' away in time, and this could never be prevented, no matter how good the

More information

arxiv: v1 [nucl-th] 21 Nov 2018

arxiv: v1 [nucl-th] 21 Nov 2018 arxiv:8.0889v [nucl-th] 2 Nov 208 Strongly intensive fluctuations and correlations in ultrarelativistic nuclear collisions in the model with string fusion Vladimir Kovalenko, Saint Petersburg State University

More information

Year- 1 (Heavy- Ion) Physics with CMS at the LHC

Year- 1 (Heavy- Ion) Physics with CMS at the LHC Year- 1 (Heavy- Ion) Physics with CMS at the LHC Edwin Norbeck and Yasar Onel (for the CMS collaboration) University of Iowa For the 26 th Winter Workshop on Nuclear Dynamics Ocho Rios, Jamaica 8 January

More information

Parameters Sensitive to the Mass Composition of Cosmic Rays and Their Application at the Pierre Auger Observatory

Parameters Sensitive to the Mass Composition of Cosmic Rays and Their Application at the Pierre Auger Observatory WDS'12 Proceedings of Contributed Papers, Part III, 137 141, 2012. ISBN 978-80-7378-226-9 MATFYZPRESS Parameters Sensitive to the Mass Composition of Cosmic Rays and Their Application at the Pierre Auger

More information

Photon and neutral meson production in pp and PbPb collisions at ALICE

Photon and neutral meson production in pp and PbPb collisions at ALICE Photon and neutral meson production in pp and PbPb collisions at ALICE Dieter Roehrich University of Bergen, Norway for the ALICE Collaboration Nuclear collisions at the LHC Photons as a probe for the

More information

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

UHECR and HADRONIC INTERACTIONS. Paolo Lipari Searching for the origin of Cosmic Rays Trondheim 18th June 2009 UHECR and HADRONIC INTERACTIONS Paolo Lipari Searching for the origin of Cosmic Rays Trondheim 18th June 2009 ~60 years of UHECR Energy Hadronic interaction Modeling Mass A Energy measurement problem solved.

More information

Verification of the CORSIKA code in the TeV energy

Verification of the CORSIKA code in the TeV energy Verification of the CORSIKA code in the.01-500 TeV energy range 1 S.V. Ter-Antonyan and L.S. Haroyan Yerevan Physics Institute, Alikhanyan Br.2, 375036 Yerevan, Armenia Comparisons of the world experimental

More information

STUDY ON MASS COMPOSITION OF EXTENSIVE AIR SHOWER WITH ULTRA HIGH ENERGY COSMIC RAYS USING Q PARAMETER AND THEIR MUON COMPONENT

STUDY ON MASS COMPOSITION OF EXTENSIVE AIR SHOWER WITH ULTRA HIGH ENERGY COSMIC RAYS USING Q PARAMETER AND THEIR MUON COMPONENT U.P.B. Sci. Bull., Series A, Vol. 79, Iss. 3, 2017 ISSN 1223-7027 STUDY ON MASS COMPOSITION OF EXTENSIVE AIR SHOWER WITH ULTRA HIGH ENERGY COSMIC RAYS USING Q PARAMETER AND THEIR MUON COMPONENT Maryam

More information

The LHCf data hadronic interactions and UHECR showers. Paolo Lipari LHCf meeting Catania, 6th july 2011

The LHCf data hadronic interactions and UHECR showers. Paolo Lipari LHCf meeting Catania, 6th july 2011 The LHCf data hadronic interactions and UHECR showers Paolo Lipari LHCf meeting Catania, 6th july 2011 ~50 years of UHECR Problems of determination of: Energy Mass A Hadronic interaction Modeling Measure

More information

HYPERON PRODUCTION ASYMMETRIES IN 500 GeV/c PION NUCLEUS INTERACTIONS

HYPERON PRODUCTION ASYMMETRIES IN 500 GeV/c PION NUCLEUS INTERACTIONS HYPERON PRODUCTION ASYMMETRIES IN 5 GeV/c PION NUCLEUS INTERACTIONS J. SOLANO representing the FERMILAB E79 COLLABORATION and J. MAGNIN, F.R.A. SIMÃO Centro Brasileiro de Pesquisas Físicas - CBPF Rio de

More information

Hadronic Showers. KIP Journal Club: Calorimetry and Jets 2009/10/28 A.Kaplan & A.Tadday

Hadronic Showers. KIP Journal Club: Calorimetry and Jets 2009/10/28 A.Kaplan & A.Tadday Hadronic Showers KIP Journal Club: Calorimetry and Jets 2009/10/28 A.Kaplan & A.Tadday Hadronic Showers em + strong interaction with absorber similarities to em-showers, but much more complex different

More information

The Multiple Muon Charge Ratio in MINOS Far Detector

The Multiple Muon Charge Ratio in MINOS Far Detector The Multiple Muon Charge Ratio in MINOS Far Detector C. M. Castromonte and R. A. Gomes Instituto de Física - Universidade Federal de Goiás, Brazil M. C. Goodman and P. Schreiner Argonne National Laboratory,

More information

Decay. Scalar Meson σ Phase Motion at D + π π + π + 1 Introduction. 2 Extracting f 0 (980) phase motion with the AD method.

Decay. Scalar Meson σ Phase Motion at D + π π + π + 1 Introduction. 2 Extracting f 0 (980) phase motion with the AD method. 1398 Brazilian Journal of Physics, vol. 34, no. 4A, December, 2004 Scalar Meson σ Phase Motion at D + π π + π + Decay Ignacio Bediaga Centro Brasileiro de Pesquisas Físicas-CBPF Rua Xavier Sigaud 150,

More information

How air shower and heavy ion physics benefit from each other

How air shower and heavy ion physics benefit from each other How air shower and heavy ion physics benefit from each other K. Werner and T. Pierog 5th October 29 SUBATECH, Univ. of Nantes IN2P3/CNRS EMN, Nantes, France Forschungszentrum Karlsruhe, Inst. f. Kernphysik,

More information

Hot Hypernucleus Formation in High-Energy Photonuclear Reactions

Hot Hypernucleus Formation in High-Energy Photonuclear Reactions Brazilian Journal of Physics, vol., no., September, 99 Hot Hypernucleus Formation in High-Energy Photonuclear Reactions M. Gonçalves, E.C. de Oliveira, E.L. Medeiros, S. de Pina, and S.B. Duarte Instituto

More information

Cosmic Ray Interaction Models: Overview

Cosmic Ray Interaction Models: Overview Cosmic Ray Interaction Models: Overview Sergey Ostapchenko Frankfurt Institute for Advanced Studies [] ISMD-2015 Wildbad Kreuth, October 4-9, 2015 Cosmic ray studies with extensive air shower techniques

More information

PoS(ICRC2015)424. YAC sensitivity for measuring the light-component spectrum of primary cosmic rays at the knee energies

PoS(ICRC2015)424. YAC sensitivity for measuring the light-component spectrum of primary cosmic rays at the knee energies YAC sensitivity for measuring the light-component spectrum of primary cosmic rays at the knee energies L. M. Zhai a,b, J. Huang a, D. Chen b, M. Shibata c, Y. Katayose c, Ying Zhang a, Xu Chen a, X. B.

More information

CHIARA OPPEDISANO ELENCO PUBBLICAZIONI SCIENTIFICHE

CHIARA OPPEDISANO ELENCO PUBBLICAZIONI SCIENTIFICHE CHIARA OPPEDISANO ELENCO PUBBLICAZIONI SCIENTIFICHE PUBBLICAZIONI SU RIVISTE SCIENTIFICHE INTERNAZIONALI (1) NA60 Collaboration, Precision study of the η µµγ and ω µ+µµπ0 electromagnetic transition form-factors

More information

The measurement of non-photonic electrons in STAR

The measurement of non-photonic electrons in STAR The measurement of non-photonic electrons in STAR Czech Technical University in Prague, Faculty of Nuclear Sciences and Physical Engineering, Břehová 7, 11519, Prague 1, Czech Republic E-mail: olga.hajkova@fjfi.cvut.cz

More information

Prompt Neutrino Fluxes from Charm Production in the Atmosphere

Prompt Neutrino Fluxes from Charm Production in the Atmosphere Prompt Neutrino Fluxes from Charm Production in the Atmosphere Yu Seon Jeong Yonsei University Wor in progress with M. H. Reno, and C. S. Kim, and with A. Bhattacharya, I. Sarcevic, and R. nberg YongPyong-High1

More information

32 nd International Cosmic Ray Conference, Beijing 2011

32 nd International Cosmic Ray Conference, Beijing 2011 32 nd International Cosmic Ray Conference, Beijing 2011 The Protons in Primary Cosmic Rays in the Energy Range 10 15-10 17 ev According to Data from the PAMIR Experiment V.S. Puchkov 1, E.A. Kanevskaya

More information

Neutrinos from charm production: atmospheric and astrophysical applications

Neutrinos from charm production: atmospheric and astrophysical applications Neutrinos from charm production: atmospheric and astrophysical applications Mary Hall Reno Department of Physics and Astronomy University of Iowa Iowa City, Iowa, 52242, USA 1 Introduction High energy

More information

Polarizing Helium-3 for down quark spin enrichment. Nigel Buttimore

Polarizing Helium-3 for down quark spin enrichment. Nigel Buttimore Polarizing Helium-3 for down quark spin enrichment Nigel Buttimore Trinity College Dublin 12 September 2012 Diffraction 2012 Polarized Helium-3 OUTLINE Introduction to the spin structure of polarized protons

More information

Particle accelerators

Particle accelerators Particle accelerators Charged particles can be accelerated by an electric field. Colliders produce head-on collisions which are much more energetic than hitting a fixed target. The center of mass energy

More information

Review of LHCb results on MPI, soft QCD and diffraction

Review of LHCb results on MPI, soft QCD and diffraction Review of LHCb results on MPI, soft QCD and diffraction Marcin Kucharczyk on behalf of LHCb collaboration HNI Krakow EDS Blois 2015, Borgo (Corse), 30.06.2015 Outline LHCb - general purpose forward experiment

More information

arxiv: v1 [hep-ex] 18 Jan 2016

arxiv: v1 [hep-ex] 18 Jan 2016 Jet measurements in pp, p Pb and Pb Pb collisions with ALICE at the LHC arxiv:6.446v [hep-ex] 8 Jan 6 Centre for Astroparticle Physics and Space Science, Bose Institute, Kolkata, 79 (INDIA) E-mail: sprasad@cern.ch

More information

Nuclear Surface Effects in Heavy Ion Collision at RHIC and SPS 1 Klaus Werner

Nuclear Surface Effects in Heavy Ion Collision at RHIC and SPS 1 Klaus Werner 0-0 SQM 2006 Nuclear Surface Effects in Heavy Ion Collision at RHIC and SPS 1 Klaus Werner The fact that nuclei have diffuse surfaces (rather than being simple spheres) has dramatic consequences on the

More information

Experimental results on the atmospheric muon charge ratio

Experimental results on the atmospheric muon charge ratio DOI:.51/epjconf/2016123007 Experimental results on the atmospheric muon charge ratio N. Mauri a Dipartimento di Fisica e Astronomia dell Università di Bologna and INFN, Sezione di Bologna, Viale Berti

More information

Electromagnetic and hadronic showers development. G. Gaudio, M. Livan The Art of Calorimetry Lecture II

Electromagnetic and hadronic showers development. G. Gaudio, M. Livan The Art of Calorimetry Lecture II Electromagnetic and hadronic showers development 1 G. Gaudio, M. Livan The Art of Calorimetry Lecture II Summary (Z dependence) Z Z 4 5 Z(Z + 1) Z Z(Z + 1) 2 A simple shower 3 Electromagnetic Showers Differences

More information

Jet Evolution in Hot and Cold Matter

Jet Evolution in Hot and Cold Matter Jet Evolution in Hot and Cold Matter Hans J. Pirner (September 2010, Heidelberg) with S. Domdey, B. Kopeliovich, K. Zapp, J. Stachel, G. Ingelman. J. Rathsman, A. Accardi, D. Gruenewald, V. Muccifora Outline

More information

Study of Charm Production in Forward Cone at Energy E Lab 75 TeV with two-storey XREC Exposed at Mountain Altitudes

Study of Charm Production in Forward Cone at Energy E Lab 75 TeV with two-storey XREC Exposed at Mountain Altitudes Study of Charm Production in Forward Cone at Energy E Lab 75 TeV with two-storey XREC Exposed at Mountain Altitudes A.S.Borisov 1,a, A.P.Chubenko 1, V.G.Denisova 1, V.I.Galkin 2, Z.M.Guseva 1, E.A.Kanevskaya

More information

PoS(DIS2017)208. Nuclear PDF studies with proton-lead measurements with the ALICE detector

PoS(DIS2017)208. Nuclear PDF studies with proton-lead measurements with the ALICE detector Nuclear PDF studies with proton-lead measurements with the ALICE detector a,b for the ALICE Collaboration a Institute for Subatomic Physics, Department for Physics and Astronomy and EMMEφ, Faculty of Science,

More information

Mapping the Nuclear Matter Phase Diagram with STAR: Au+Al at 2.8 AGeV and Au+Au at 19.6 GeV

Mapping the Nuclear Matter Phase Diagram with STAR: Au+Al at 2.8 AGeV and Au+Au at 19.6 GeV Mapping the Nuclear Matter Phase Diagram with STAR: Au+Al at 2.8 AGeV and Au+Au at 19.6 GeV Samantha G Brovko June 14, 2011 1 INTRODUCTION In ultra-relativistic heavy ion collisions a partonic state of

More information

DIFFERENT H.E. INTERACTION MODELS

DIFFERENT H.E. INTERACTION MODELS COMPARISON OF EAS SIMULATION RESULTS USING CORSIKA CODE FOR DIFFERENT H.E. INTERACTION MODELS Dept. of Physics, Gauhati University, Assam, INDIA 15th Sep, 2010 Out line of the talk Introduction Primary

More information

Characteristics study of projectile s lightest fragment for

Characteristics study of projectile s lightest fragment for 1 Characteristics study of projectile s lightest fragment for 84 Kr 36 - emulsion interaction at around 1 A GeV N. Marimuthu 1, 2, V. Singh 1 *, S. S. R. Inbanathan 2 1 High Energy Physics laboratory,

More information

Nuclear Physics and Astrophysics

Nuclear Physics and Astrophysics Nuclear Physics and Astrophysics PHY-30 Dr. E. Rizvi Lecture 4 - Detectors Binding Energy Nuclear mass MN less than sum of nucleon masses Shows nucleus is a bound (lower energy) state for this configuration

More information

Secondary particles generated in propagation neutrinos gamma rays

Secondary particles generated in propagation neutrinos gamma rays th INT, Seattle, 20 Feb 2008 Ultra High Energy Extragalactic Cosmic Rays: Propagation Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Energy loss processes protons

More information

Scaling of multiplicity distribution in high energy hadron-nucleus interactions

Scaling of multiplicity distribution in high energy hadron-nucleus interactions IOSR Journal of Applied Physics (IOSR-JAP) e-issn: 2278-4861.Volume 6, Issue 5 Ver. II (Sep.-Oct. 2014), PP 15-19 Scaling of multiplicity distribution in high energy hadron-nucleus interactions Tufail

More information

The NUCLEON Space Experiment Preliminary Results. Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, , Russia

The NUCLEON Space Experiment Preliminary Results. Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, , Russia The NUCLEON Space Experiment Preliminary Results A. Turundaevskiy a1, E.Atkin a, V.Bulatov c, V.Dorokhov c, N.Gorbunov d, S.Filippov c, V.Grebenyuk d, D.Karmanov a, I.Kovalev a, I.Kudryashov a, M.Merkin

More information

Physics 736. Experimental Methods in Nuclear-, Particle-, and Astrophysics. Lecture 3

Physics 736. Experimental Methods in Nuclear-, Particle-, and Astrophysics. Lecture 3 Physics 736 Experimental Methods in Nuclear-, Particle-, and Astrophysics Lecture 3 Karsten Heeger heeger@wisc.edu Review of Last Lecture a colleague shows you this data... what type of reaction is this?

More information

QCD at Cosmic energies VII

QCD at Cosmic energies VII Impact of Minijet & Heavy-quark Production on the Muon Anomaly in Atmospheric Showers from Ultrahigh Energy Cosmic Rays QCD at Cosmic energies VII Chalkida, 19th May 2016 Sun Guanhao (HKUST, CERN) David

More information

Same-sign dileptons as a signature for heavy Majorana neutrinos in hadron-hadron collisions

Same-sign dileptons as a signature for heavy Majorana neutrinos in hadron-hadron collisions arxiv:hep-ph/9703441v1 27 Mar 1997 Same-sign dileptons as a signature for heavy Majorana neutrinos in hadron-hadron collisions F. M. L. Almeida Jr. (1), Y. A. Coutinho (1), J. A. Martins Simões (1), P.

More information

Cosmic Rays: A Way to Introduce Modern Physics Concepts. Steve Schnetzer

Cosmic Rays: A Way to Introduce Modern Physics Concepts. Steve Schnetzer Cosmic Rays: A Way to Introduce Modern Physics Concepts Steve Schnetzer Rutgers CR Workshop May 19, 2007 Concepts Astrophysics Particle Physics Radiation Relativity (time dilation) Solar Physics Particle

More information

FUTURE SPIN EXPERIMENTS AT SLAC

FUTURE SPIN EXPERIMENTS AT SLAC SLAC-PUB-9658 February 2003 FUTURE SPIN EXPERIMENTS AT SLAC Stephen Rock for the Real Photon Collaboration University of Mass, Amherst MA 01003 Abstract. A series of three photo-production experiments

More information

The Development of Particle Physics. Dr. Vitaly Kudryavtsev E45, Tel.:

The Development of Particle Physics. Dr. Vitaly Kudryavtsev E45, Tel.: The Development of Particle Physics Dr. Vitaly Kudryavtsev E45, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Discovery of the muon and the pion Energy losses of charged particles. This is an important

More information

Gluons at high x in Nuclei at EIC

Gluons at high x in Nuclei at EIC Gluons at high x in Nuclei at EIC in collaboration with: E. Chudakov, D. Higinbotham, C. Hyde, C. Weiss Jefferson Lab DNP 2015 Fall meeting, Santa Fe, NM Outline Motivation HERA and ZEUS experience EIC

More information

Charged Current Inclusive Scattering in MINERnA

Charged Current Inclusive Scattering in MINERnA Charged Current Inclusive Scattering in MINERnA What is Minerna? Why Minerna? n beam and n flux n / n inclusive x-sections x-section ratios (A-depndence) Outlook NUFACT 2013 August 21 st 13 Alessandro

More information

arxiv: v1 [hep-ph] 30 Dec 2018

arxiv: v1 [hep-ph] 30 Dec 2018 Jet fragmentation in a QCD medium: Universal quark/gluon ration and Wave turbulence arxiv:1812.11533v1 [hep-ph] 30 Dec 2018 Y. Mehtar-Tani Brookhaven National Laboratory, Physics Department, Upton, NY

More information

Probing QCD approach to thermal equilibrium with ultrahigh energy cosmic rays

Probing QCD approach to thermal equilibrium with ultrahigh energy cosmic rays Probing QCD approach to thermal equilibrium with ultrahigh energy cosmic rays Department of Physics&Astronomy, Lehman College, CUNY, NY 10468, USA Department of Physics, Graduate Center, City University

More information

Complex amplitude phase motion in Dalitz plot heavy meson three body decay.

Complex amplitude phase motion in Dalitz plot heavy meson three body decay. Complex amplitude phase motion in Dalitz plot heavy meson three body decay. arxiv:hep-ph/0211078v1 6 Nov 2002 Ignacio Bediaga and Jussara M. de Miranda Centro Brasileiro de Pesquisas Físicas, Rua Xavier

More information

Measurement of the cosmic ray all-particle and light-component energy spectra with the ARGO- YBJ experiment

Measurement of the cosmic ray all-particle and light-component energy spectra with the ARGO- YBJ experiment Journal of Physics: Conference Series PAPER OPEN ACCESS Measurement of the cosmic ray all-particle and light-component energy spectra with the ARGO- YBJ experiment To cite this article: Ivan De Mitri and

More information

Study of muon bundles from extensive air showers with the ALICE detector at CERN LHC

Study of muon bundles from extensive air showers with the ALICE detector at CERN LHC doi:.88/174-6596/718/5/0509 Study of muon bundles from extensive air showers with the ALICE detector at CERN LHC K Shtejer 1, 1 Dipartimento di Fisica dell'università and Sezione INFN, Turin, Italy Centro

More information

Physics with Exotic Nuclei

Physics with Exotic Nuclei Physics with Exotic Nuclei Hans-Jürgen Wollersheim NUclear STructure, Astrophysics and Reaction Outline Projectile Fragmentation A Route to Exotic Nuclei Fragmentation Cross Sections Nuclear Reaction Rates

More information

Transport Theoretical Studies of Hadron Attenuation in Nuclear DIS. Model Results Summary & Outlook

Transport Theoretical Studies of Hadron Attenuation in Nuclear DIS. Model Results Summary & Outlook Transport Theoretical Studies of Hadron Attenuation in Nuclear DIS T. Falter, W. Cassing,, K. Gallmeister,, U. Mosel Contents: Motivation Model Results Summary & Outlook Motivation elementary en reaction

More information

arxiv: v1 [hep-ph] 19 Nov 2018

arxiv: v1 [hep-ph] 19 Nov 2018 Probing QCD approach to thermal equilibrium with ultrahigh energy cosmic rays arxiv:1811.07728v1 [hep-ph] 19 Nov 2018 Department of Physics & Astronomy, Lehman College, CUNY, NY 10468, USA Department of

More information

THIS work is devoted to the description of the simulation

THIS work is devoted to the description of the simulation IEEE TRANSACTIONS ON NUCLEAR SCIENCE, VOL. 53, NO. 2, APRIL 2006 513 Geant4 Simulation of Production and Interaction of Muons A. G. Bogdanov, H. Burkhardt, V. N. Ivanchenko, S. R. Kelner, R. P. Kokoulin,

More information

Low mass dileptons from Pb + Au collisions at 158 A GeV

Low mass dileptons from Pb + Au collisions at 158 A GeV PRAMANA cfl Indian Academy of Sciences Vol. 60, No. 5 journal of May 2003 physics pp. 1073 1077 Low mass dileptons from Pb + Au collisions at 158 A GeV SOURAV SARKAR 1, JAN-E ALAM 2;Λ and T HATSUDA 2 1

More information

arxiv:hep-ph/ v1 11 Mar 1994

arxiv:hep-ph/ v1 11 Mar 1994 An interesting charmonium state formation and decay: p p D 2 P γ M. Anselmino a, F. Caruso b,c, F. Murgia d and M.R. Negrão b arxiv:hep-ph/9403272v Mar 994 a Dipartimento di Fisica Teorica, Università

More information

String Parton Models in Geant4

String Parton Models in Geant4 String Parton Models in Geant4 G.Folger, J.P.Wellisch CERN, CH-2 Geneva, Switzerland Dual parton or quark gluon string model are the by now almost standard theoretical techniques by which one can arrive

More information

Study of charm fragmentation in e + e annihilation and ep scattering

Study of charm fragmentation in e + e annihilation and ep scattering Study of charm fragmentation in e + e annihilation and ep scattering - Summer Student Report - by Thomas Lübbert H1 Collaboration at DESY Advisor: Co-Advisor: Dr. Günter Grindhammer Andrej Liptaj September

More information

On the intrinsic charm and the recombination. J.C. Anjos, J. Magnin y. Centro Brasileiro de Pesquisas Fsicas. G. Herrera z

On the intrinsic charm and the recombination. J.C. Anjos, J. Magnin y. Centro Brasileiro de Pesquisas Fsicas. G. Herrera z CBPF-NF-053/01 On the intrinsic charm and the recombination mechanisms in charm hadron production J.C. Anjos, J. Magnin y Centro Brasileiro de Pesquisas Fsicas Rua Dr. Xavier Sigaud 150, CEP 22290-180,

More information

arxiv:astro-ph/ v1 15 Mar 2002

arxiv:astro-ph/ v1 15 Mar 2002 Fluxes of cosmic rays: A delicately balanced anomalous thermal equilibrium Constantino Tsallis, 1 Joao C. Anjos, 1 Ernesto P. Borges 1,2 1 Centro Brasileiro de Pesquisas Fisicas, Rua Xavier Sigaud 150

More information

Visit for more fantastic resources. AQA. A Level. A Level Physics. Particles (Answers) Name: Total Marks: /30

Visit   for more fantastic resources. AQA. A Level. A Level Physics. Particles (Answers) Name: Total Marks: /30 Visit http://www.mathsmadeeasy.co.uk/ for more fantastic resources. AQA A Level A Level Physics Particles (Answers) Name: Total Marks: /30 Maths Made Easy Complete Tuition Ltd 2017 1. This question explores

More information

Hadronization with JLab 6/12 GeV

Hadronization with JLab 6/12 GeV Hadronization with JLab 6/12 GeV Next generation nuclear physics with JLab12 and EIC Florida International University February 10-13th, 2016 Lamiaa El Fassi (On behalf of EG2 and CLAS Collaborations) Outline

More information

Chapter 2 Radiation-Matter Interactions

Chapter 2 Radiation-Matter Interactions Chapter 2 Radiation-Matter Interactions The behavior of radiation and matter as a function of energy governs the degradation of astrophysical information along the path and the characteristics of the detectors.

More information

Longitudinal Double Spin Asymmetry in Inclusive Jet Production at STAR

Longitudinal Double Spin Asymmetry in Inclusive Jet Production at STAR Longitudinal Double Spin Asymmetry in Inclusive Jet Production at STAR Katarzyna Kowalik for the STAR Collaboration Lawrence Berkeley National Laboratory, Berkeley, California 94720 Abstract. This contribution

More information

Strange Hadron Production from STAR Fixed-Target Program

Strange Hadron Production from STAR Fixed-Target Program Strange Hadron Production from STAR Fixed-Target Program (for the STAR Collaboration) Department of Engineering Physics, Tsinghua University, Beijing 84, China E-mail: musman_mughal@yahoo.com We report

More information

arxiv:hep-ex/ v2 2 Feb 2001

arxiv:hep-ex/ v2 2 Feb 2001 CR-459 hep-ex/00009 RECENT RESULTS ON PARTICLE PRODUCTION FROM J. H. VOSSEBELD CERN, CH - 2 Geneva 23, Switzerland E-mail: Joost.Vossebeld@cern.ch arxiv:hep-ex/00009v2 2 Feb 200 Three recent studies are

More information

HARP collaboration results on the proton-nuclei interactions at a few GeV energies

HARP collaboration results on the proton-nuclei interactions at a few GeV energies HARP collaboration results on the proton-nuclei interactions at a few GeV energies HARP : A fixed-target experiment at the CERN Proton Synchrotron (2000-2002) aimed at measurement of hadron production

More information

Photo-production of vector mesons in 2.76 TeV ultra-peripheral Pb+Pb collisions at ALICE. Daniel Tapia Takaki. On behalf of the ALICE Collaboration

Photo-production of vector mesons in 2.76 TeV ultra-peripheral Pb+Pb collisions at ALICE. Daniel Tapia Takaki. On behalf of the ALICE Collaboration Photo-production of vector mesons in 2.76 TeV ultra-peripheral Pb+Pb collisions at ALICE On behalf of the ALICE Collaboration Rencontres du Viet Nam: 14th Workshop on Elastic and Diffractive Scattering

More information

From the Knee to the toes: The challenge of cosmic-ray composition

From the Knee to the toes: The challenge of cosmic-ray composition New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition Jörg R. Hörandel University of Karlsruhe www-ik.fzk.de/~joerg New Views of

More information

Measurement of the Cosmic Ray Energy Spectrum with ARGO-YBJ

Measurement of the Cosmic Ray Energy Spectrum with ARGO-YBJ Measurement of the Cosmic Ray Energy Spectrum with ARGO-YBJ Ivan De Mitri ( on behalf of the ARGO-YBJ collaboration ) Dipartimento di Matematica e Fisica " E. De Giorgi", Universita del Salento, Lecce,

More information

1 The pion bump in the gamma reay flux

1 The pion bump in the gamma reay flux 1 The pion bump in the gamma reay flux Calculation of the gamma ray spectrum generated by an hadronic mechanism (that is by π decay). A pion of energy E π generated a flat spectrum between kinematical

More information

Lecture 3. lecture slides are at:

Lecture 3. lecture slides are at: Lecture 3 lecture slides are at: http://www.physics.smu.edu/ryszard/5380fa16/ Proton mass m p = 938.28 MeV/c 2 Electron mass m e = 0.511 MeV/c 2 Neutron mass m n = 939.56 MeV/c 2 Helium nucleus α: 2 protons+2

More information

Propagation in the Galaxy 2: electrons, positrons, antiprotons

Propagation in the Galaxy 2: electrons, positrons, antiprotons Propagation in the Galaxy 2: electrons, positrons, antiprotons As we mentioned in the previous lecture the results of the propagation in the Galaxy depend on the particle interaction cross section. If

More information