Hadronic Interactions Around 50 TeV

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Measurement of angular and momentum distributions of

= 5.02 TeV Pb+Pb data. In both samples, events are required to have a reconstructed vertex within 150 mm of the nominal IP along the beam axis. Events with multiple interactions in the same bunch crossing are referred to as pileup. This is negligible in the Pb+Pb data, and the ppdata was collected in low-pileup mode. The average number of interactions per


few interactions in the atmosphere. In the vertical direction the thickness of the atmosphere corresponds to ~11 interaction lengths. The number of hadronic interactions occurring for single-hadron events is shown in Figure 3. In the TeV range primary protons or helium nuclei

Diffuse Gamma-Rays Produced in Cosmic-Ray Interactions and

hadronic interactions have contributed about 20% of the total -ray photons, mostly from directly produced -rays and decays of , K0 L and K 0 S [7]. In the cosmic-ray interactions, we calculate the -ray spectrum density contributed by decays of un-stable secondary particles Q (E) nISM = X k Z dENCR(E)c ˙(E) dnk; dE (1) where dnk; dE = dnk; dE (E;E) is the -ray decay

Multi-messenger aspects of cosmic neutrinos

Hadronic interactions of CRs with gas (pp)orradiation(p ) produce a flux of neutrinos with an energy of about 5% of the initial CR nucleon. Hence, the CRs responsible for the observed neutrino

arXiv:1106.2453v1 [hep-ph] 13 Jun 2011 - CiteSeerX

The highest energy hadronic interactions measured on Earth result from the collision of cosmic rays (CR) protons and nuclei accelerated in various astrophysical sources that propagate through the universe up to the so-called Greisen-Zatsepin-Kuzmin (GZK) cutoff around

The Nine Lives of Cosmic Rays in Galaxies

AA53CH06-Grenier ARI 29 July 2015 12:16 The Nine Lives of Cosmic Rays in Galaxies Isabelle A. Grenier,1 John H. Black,2 and Andrew W. Strong3 1Laboratoire AIM Paris-Saclay, CEA/Irfu, CNRS, Universite Paris Diderot, F-91191´ Gif-sur-Yvette Cedex, France; email: [email protected]

Photonuclear Interactions in Heavy-Ion Collisions at the

=2.76 TeV) for Eγ > 6 GeV: 24.2 b - Larger than the total hadronic cross section, but a rather aribtrary number because of the selection Eγ > 6 GeV. - However, there is a strong correlation between photon energy and the range in rapidity of the produced particles Production around mid-rapidity dominated by photons with energies >> 6 GeV.

on behalf of the ATLAS Collaboration

of ~ 50 MeV 1. Mapping the material in the ATLAS Inner Detector using secondary hadronic interactions, ATLAS-CONF-2010-058 2. Charged particle multiplicities at √s = 2.36 TeV measured with the ATLAS detector, ATLAS-CONF-2010-058 5. D* mesons reconstruction in pp collisions at √s = 7 TeV, ATLAS-CONF-2010-034 6.

Hadronic interactions and primary cosmic ray composition

composition of primary cosmic rays at the energy region around 1015-10 7eV are summarised. 1. Introduction Until Lattes et al s review (1980), the study of hadronic interactions at energies around 1014eV by use of the mountain emulsion chamber (MEC) had remarkable success in the 1970s.


Physics LettersB 694 (2011) 327 345 Contents lists available at ScienceDirect PhysicsLettersB www.elsevier.com/locate/physletb

Search for pair production of heavy vectorlike quarks

50 GeV, with additional events produced at 500, 600, 1300, and 1400 GeV. Additional samples were produced assuming a doublet scenario for VLQ masses of 700, 950, and 1200 GeV, in order to study differences from the different chirality of VLQs arising in singlet and doublet models. The pair production cross section varies from 3.38 0.25 pb (m


hadronic interaction. The hadronic interaction is subject of various uncertainties and debates, in particular in energy regimes which exceed the energies of man-made accelerators and the knowledge from collider experiments. The EAS development is dominantly governed by soft processes which are not accessible to perturbative QCD.

The Application of the Monte Carlo Code FLUKA in Radiation

The module for hadronic interactions is called PEANUT (PreEquilibrium Approach to Nuclear Thermalization) and consists of a phenomenological description (Dual Parton Model-based Glauber-Gribov cascade) of high-energy interactions (up to 20 TeV), a generalized intra-nuclear *Corresponding author, E-mail:[email protected]

Primary proton and helium spectra at energy range from 50

50 cm, covering an area about 10 m2, which is used to check hadronic interaction models. YAC-IIand YAC-III are used to obtain the individual component spectra of pri-mary cosmic rays in a wide range over 3 decades between 50 TeV and 100 PeV in the near future. YAC-I

arXiv:astro-ph/0106494v1 27 Jun 2001

high-energy hadrons (>100 GeV) by up to 50 % and of the electron number (>3 MeV) by ≃15 %, calculated for EAS of vertical incidence at sea level. The depth of shower

Hard X-rays as distinct features of PeVatrons+

are effectively produced in E-M and hadronic interactions are effectively detected by space- and ground-based instruments one of the highest priorities of new generation detectors > 10 TeV photons but these gamma-rays are very fragile, especially at >> 10 TeV (effectively

A possible approach to check the interaction models by

Putting the above together, the experimental test on the hadronic interaction models used in the AS simulation codes can be made at primary energy around 20 TeV by YAC low energy mode with high statistics. 5. Acknowledgements The authors would like to express their thanks to the members of the Tibet AS G collaboration for the fruitful discussions.

The Galactic diffuse gamma ray emission in the energy

Galactic latitude around the equator (50% of the emission above 10 GeV is contained in the region at 100 TeV due to the presence of the knee in CR spectra. The effects of the knee have been calculated using a simple model of p production in hadronic interactions and the model [13] for the CR spectra.

Hadronic Interaction Studies with the ARGO-YBJ Experiment

around the core position at groundfor simulated proton ini-tiated showers with 104 < Np8 < 3 104. The particle den-sities obtained with QGSJET-II and SYBILL are shown in the upper panel, while the percentage deviation among the two models is given in the lower one. /m-3) 1m Log10(LDF-Slope 0.5 1 1.5 2 2.5 3 3.5 4 4.5) 2 (g/cm dm X 0 50 100 150

Search for long-lived neutral particles produced in pp

the ID is the interactions between SM particles and the material in the inner detector, which may create multitrack vertices that are displaced from the IP. Other sources of background are hadronic jets, vertices reconstructed from fake tracks that are created from multiple unrelated energy deposits, and vertices reconstructed from random track

Cosmic-Ray Studies with Experimental Apparatus at LHC

15/10/2020  be explained using the hadronic interaction models available at that time. The main conclusion of LEP experiments about these phenomena was that events with intermediate multiplicity of muons (Nm 50) are reproducible using the standard particle production mechanisms, but the high multiplicity muon

Extending the Calibration of the ATLAS Hadronic

dominated by the resolution of the hadronic calorimeter itself. The hadronic calorimeter resolution has been measured in test bed studies and is given by: Equation 3: σ Hcal E = 50 %GeV E + 3% Thus, at E = 200 GeV, for a desired uncertainty in the calibration of 1%, we need ~40 events, and at 1 TeV ~20.

Test of hadronic interaction models in the forward region

around 5 TeV can be reduced by increasing the non-diffractive part of the inelastic cross section of nucleon air interactions. An examination of hadron multiplicities points towards harder spectra of secondary pions and kaons being needed in the calculations. (Some figures in this article are in colour only in the electronic version) 1

Multi-Parton Interactions and Underlying Event: A PYTHIA

Multi-Parton Interactions and Underlying Event: A PYTHIA perspective Christian Bierlich, [email protected] University of Copenhagen Lund University June 3rd, 2020, 10th Hard Probes 1. Introduction A brief overview of Pythia s venture into heavy ion physics. Why?

A study of the material in the ATLAS inner detector using

ABSTRACT: The ATLAS inner detector is used to reconstruct secondary vertices due to hadronic interactions of primary collision products, so probing the location and amount of material in the inner region of ATLAS. Data collected in 7 TeV pp collisions at the LHC, with a minimum bias trigger, are used for comparisons with simulated events.

Hadronic Interaction Studies with the ARGO-YBJ Experiment

around the core position at groundfor simulated proton ini-tiated showers with 104 < Np8 < 3 104. The particle den-sities obtained with QGSJET-II and SYBILL are shown in the upper panel, with the percentage deviation among the two models is given in the lower one. /m-3) 2m Log10(LDF-Slope 0.5 1 1.5 2 2.5 3) 2 (g/cm dm X 0 50 100 150 200 250

Extensive Air Showers and Particle Physics

photoproduction interactions on the 3K background. More problems: such detections continue, the current world statistics is around 10 events 1020 eV = = 2.4x1034 Hz = 1.6x108 erg = 170 km/h tennis ball √s equivalent is 430 TeV

PAPER OPEN ACCESS Ground-based Gamma-Ray Astronomy: an

18/5/2020  the dust (with wavelength & 50 m). The other components of the interstellar radiation eld give smaller contributions that are visible in the inset of the gure. The survival probability has a deeper minimum P surv ˇ0.30 for E ˘2.2 PeV that is due to the CMBR, and a second minimum at E ˘50 TeV [1].


Hadronic physics in Geant4: cross sections and models for hadron-nucleus interaction up to TeV For neutrons from thermal energies to TeV Models are tuned with thin target data (not calorimeters test-beam) Models are assembled in physics lists: stable configurations (few billions of events simulated) Example: QGSP BERT (used at LHC since 3-4 years)

Air Shower Simulations'

are discussed. The basic principles of hadronic interaction models and some gemeral simulation techniques are explained. Also a brief introduction to the installation and use of CORSIKA is given. Keywords: cosmic rays, air showers, simulations, hadronic interactions PACS: 02.70.Uu, I3.85.Tp, 96.50.sd, 96.50.sf Introduction

Centrality dependence of π ,andp production in Pb-Pb

hadronic phase does not affect particle abundances [10,15]. It was also suggested that the temperature of the hadronic ( chemical ) freeze-out can be related to the phase transition temperature [12,16,17]. Abundances of particles have been fitted very successfully over a wide range of energies (from√ s NN = 2GeVto √ s NN = 200GeV[11,12

Gamma-ray signatures of cosmic ray acceleration

The interactions be-tween CRs and the interstellar gas makes the galactic disk a prominent source of di use gamma rays at energies above ˇ100 MeV [23]. No di use emis-sion has been rmly detected at TeV energies from the galactic disk, though some evidence for the

Proton-oxygen collisions at the LHC - Indico

Wanted: p-O collisions to accurately simulate hadronic showers in air Current uncertainties 50 % in pion multiplicity, need better than 10 % Needed by community of 900+ scientists (Auger, TA, IceCube, ) Moderate luminosity sufficient (100 M events) Interest expressed by


suming the multi-TeV diffuse flux observed by MI-LAGRO is produced through hadronic interactions. This model requires the assumption of a harder CR spectrum in the inner part of the Galaxy than the canonical 2.7 spectral index of the CRs observed at Earth. Consequently we obtain a higher value for the multi-TeV neutrino flux from the same Galac-

Testing Hadronic Interactions Using Hybrid Observables

Testing Hadronic Interactions Using Hybrid Observables Jakub Vícha 1. Introduction The mass composition of ultra-high energy cosmic rays (UHECR, >1018 eV) can be inferred from measurements of the depth of shower maximum (X max), which is currently the most reliable observable that is sensitive to the mass composition of UHECR. The interpretation of the X

Characteristics of extensive air showers around the energy

(IACT) performance values around 1 TeV are angular reso- most obvious differentiating characteristic of hadronic ver-sus purely electromagnetic (EM) cascades is the presence of pions, The electromagnetic interactions are handled by the EGS4 model [24].

The Cosmic Ray Proton Spectrum determined with the Imaging

protons over a limited energy range around 1.5 TeV. Although the IACT sys-tem is designed for the detection of γ-rays with energies above 500 GeV, it has also a large detection area of 106 m2 3 msr for primary protons of energies above 1 TeV and the capability to reconstruct the primary proton energy with

Gamma ray observations above 30 TeV with Lhaaso

Hadronic interactions p p p0 + other particles p0 2 g The gamma ray spectrum is simmetric around mp /2 = 67.5 MeV in a log-log scale (p0 bump) Above a few GeV has the same slope of the parents protons There is no suppression at high energy as IC, unless the parent proton spectrum has a cutoff

Outline - NASA

10 Scintillators 5×5×50 cm3 , each viewed by two 2 dia. PMTs Multiple detector locations possible (secondary neutrons are present all around the detector mass) e/ppy discrimination enhanced by material selection for hadronic interactions and neutron moderation Boron-loaded scintillator Logs(10) Photomultiplier tubes(20)

Nature of 100 TeV Hadronic Interactions in the Forward

up to 100 TeV has been directly measured [2]. Thus, in this energy region, it might be possible to study separately the phenomena of hadronic interactions in the forward region from cosmic ray fixed target experiments, and escaping from the two-factor-twining puzzle. Near the energy region we are interested in, the collider experiments of in-

Gamma Ray Astronomy with LHAASO - TAUP Conference

Hadronic interactions pp p0 + other particles p0 2 g The gamma ray spectrum is simmetric around mp /2 = 67.5 MeV in a log-log scale (p0 bump) Above a few GeV has Gamma ray astronomy at 50-100 TeV is a field of research completely new.

Exploring Potential Signatures of QGP in UHECR Ground Pro les

sample size of potential QGP-positive initial interactions. All initial interaction events were simulated in 50 event batches using EPOS-LHC and CRMC v1.4 and v1.5.5. The simulations were of vertical Neon (Ne) primaries at 100 PeV (0.1 EeV) hitting a Carbon (C) target at rest (p s

sqrt{s}=8 $$ TeV proton-proton collisions

The ATLAS detector [50,51] provides nearly full solid angle2 coverage around the collision point with an inner tracking system (inner detector, or ID) covering the pseudorapidity range j j<2:5, electromagnetic (EM) and hadronic calorimeters covering j j< 4:9, and a muon spectrometer covering j j< 2:7 that provides muon trigger capability up to

j a b a e c;f;n g c e a arXiv:1711.02643v2 [astro-ph.HE

exceeding 50 GeV. Of particular interest for the study of hadronic interactions was a 320 m2 hadronic sampling calorimeter (E h > 20 GeV) with a total depth of 11 hadronic inter-action lengths, interspaced with nine lay-ers of liquid ionization chambers [6], see Fig.2. To extend the energy range up to 1018 eV was the motivation for the exten-

Cosmic Ray Electron Spectrum with the Fermi-LAT

LAT as electron detectorNot only rays I Detector is designed for E. M. showers I Naturally including electrons (e+ + e) I Triggering on (almost) every particle that crosses the LAT I On-board filtering to remove many charged particles I Keeps all events with more than 20 GeV in the CAL I Prescaled (⇥250) unbiased sample of all trigger types I Event reconstruction assumes a

Performance of pile-up mitigation techniques for jets in

Mean Number of Interactions per Crossing 0 5 10 15 20 25 30 35 40 45 /0.1]-1 Recorded Luminosity [pb 0 20 40 60 80 100 120 140 160 180 ATLAS Online Luminosity s = 8 TeV, ∫Ldt = 21.7 fb-1, <μ> = 20.7 s = 7 TeV, ∫Ldt = 5.2 fb-1, <μ> = 9.1 Fig. 1 The luminosity-weighted distribution of the mean number of interactions per bunch crossing for

Searches for long-lived particles in ATLAS

Displaced jets in the hadronic calorimeter(Eur. Phys. J. C 79 (2019) 481) Targeted Hidden Sector model Long-lived scalars decay in the hadronic calorimeter Key object is a jet with large 2 #!/2 $% ratio (CalRatiojets) Reinterpretation of Displaced hadronic jets in the calorimeter ATL-PHYS-PUB-2020-007 arXiv: 1810.12602

Recent results from the Pierre Auger Observatory

(50 joule). Other events with energies around 1020 eV had been reported in the previous 30 years, but this was clearly the most energetic! It was known as the Oh-My-God particle. o In 1994 The AGASA group in Japan and the Yakutsk group in Russia each reported an event with an energy of 2 x