2675 DPyC SMF false [["0", "Event Poster"], ["minutes", "Minutes"], ["notes", "Notes"], ["paper", "Paper"], ["poster", "Poster"], ["slides", "Slides"], ["summary", "Summary"]] Cinvestav ea481e58ca9c64e14d7982cb66bcd604 3312 <p style="text-align:justify">The <strong>XXI Mexican School on Particles and Fields</strong> takes place from <strong>October 19th to 23rd, 2026</strong>, in the city of Puebla, Puebla, M&eacute;xico. The format of the school is&nbsp;such that the morning sessions are devoted to theoretical and experimental reviews, whereas parallel thematic sessions shall be held in the afternoons. All the reviews and seminars are delivered by experts of international prestige on subjects which are of current interest to the global scientific community and are also actively pursued within M&eacute;xico. ​</p> <p style="text-align:justify">In order to equip graduate students and attending postdocs with the necessary tools to perform fully in the school, courses of interest are taught, with English being the language of instruction. An informal and friendly atmosphere is encouraged during the courses so that the students can overcome their inhibitions and actively participate in the discussions. ​</p> <p style="text-align:justify"><em><u><strong>Organizing Committee</strong></u></em></p> <p style="text-align:justify">Dr. Isabel Pedraza Morales (President DPyC-SMF) [BUAP]<br /> Dr. Humberto G. Maury Cuna (Vice-President DPyC-SMF)&nbsp;[UGTO]</p> <p style="text-align:justify"><em><u><strong>Local Organizing Committee</strong></u></em></p> <p style="text-align:justify">Dr. Haydee Hern&aacute;ndez [BUAP]<br /> Dr. Arturo Fern&aacute;ndez [BUAP]<br /> Dr. Humberto Salazar [BUAP]<br /> Dr. Olga F&eacute;lix Beltr&aacute;n [BUAP]</p> False Puebla

1. Edificio Carolino, Calle 4 Sur 104, Centro, Puebla, Puebla. 2. Ciudad Universitaria 2, Calle Heberto Rodríguez N°119, Colonia San Antonio Toluquilla, C.P. 72960, San Pedro Zacachimalpa, Puebla

2026-10-19T07:30:00 2026-10-23T19:30:00 2026-07-01T10:52:23 2026-10-30T16:10:28 Mexico/General Benemérita Universidad Autónoma de Puebla 65efd11437264d48aa1f7486255a57bc Universidad de Guanajuato 0bba80e6b6d806cda49089f089616ab2 BUAP 5848375cb8b0db28e94350f19dcb744f Benemerita Universidad Autonoma de Puebla 398909c50ebb53abfbd6c5540e4e5066 49 false [["0", "Event Poster"], ["minutes", "Minutes"], ["notes", "Notes"], ["paper", "Paper"], ["poster", "Poster"], ["slides", "Slides"], ["summary", "Summary"]] 0 Poster Benemérita Universidad Autónoma de Puebla BUAP be3f1f746775892cdf17c33ceb5753ec Facultad de Ciencias Físico Matemáticas, BUAP 94f6b6d92aeff62e5b9cb9b2e75b222f Facultad de Ciencias Fisico Matematicas BUAP, Mexico 81489ac17fbe3b967aba80a1a0143bf4 FCFM-BUAP 3d97e440c55d59551edad6adffecbb4a Benemérita Universidad Autónoma de Puebla BUAP be3f1f746775892cdf17c33ceb5753ec Edificio Carolino

Edificio Carolino, Calle 4 Sur 104, Centro, Puebla, Puebla.

Salón de Proyecciones 2026-10-22T17:00:00 2026-10-22T19:00:00 02:00 High-energy cosmic rays produce Extensive Air Showers (EAS) when interacting with the Earth’s atmosphere, generating, among other particles, muons that can reach underground detectors such as ALICE. Muon multiplicity provides information on the energy and composition of primary cosmic rays. However, discrepancies between experimental measurements and the predictions of hadronic interaction models, known as the Muon Puzzle, remain a challenge for the description of these air showers. During LHC Run 1, ALICE found that the rate of high-muon-multiplicity events was compatible with QGSJET-II-04 predictions under the assumption of a primary composition dominated by heavy elements. This result motivated the present work, whose objective was to analyze a larger data sample collected during Run 2 (2015–2018) and to evaluate the ability of different hadronic interaction models to describe the observed muon multiplicity. In this work, we study the muon multiplicity distribution measured by ALICE during LHC Run 2 to evaluate whether the QGSJET-II-04, EPOS-LHC, and SIBYLL 2.3d models can describe the observations for different primary cosmic-ray compositions. The data are compared with Monte Carlo simulations performed using CORSIKA, considering proton and iron primaries as representatives of light and heavy compositions, respectively. The results show that QGSJET-II-04 reasonably reproduces the muon multiplicity distribution for $4 < N_{\mu} < 50$ when a heavy primary composition is considered, whereas SIBYLL 2.3d and EPOS-LHC exhibit muon deficits of approximately 20% and 30%, respectively, over different multiplicity intervals. For events with $N_{\mu} > 100$, the rates predicted by QGSJET-II-04 and SIBYLL 2.3d assuming an iron composition are compatible with the data, while EPOS-LHC underestimates the observed rate. Overall, the results are consistent with a predominantly heavy composition for high-muon-multiplicity events, associated with primary energies $E_{\mathrm{prim}}$ close to $10^{17}\,\mathrm{eV}$, and provide constraints on current hadronic interaction models and on possible more exotic mechanisms of muon production. 0 doc http://indico.nucleares.unam.mx/images/word.png word file ppt http://indico.nucleares.unam.mx/images/powerpoint.png powerpoint file pdf http://indico.nucleares.unam.mx/images/pdf_small.png pdf file odt http://indico.nucleares.unam.mx/images/writer.png writer file odp http://indico.nucleares.unam.mx/images/impress.png presentation file ods http://indico.nucleares.unam.mx/images/calc.png spreadsheet file other http://indico.nucleares.unam.mx/images/file_small.png unknown type file link http://indico.nucleares.unam.mx/images/link.png link