Azimuthal asymmetry in the risetime of the surface detector signals of the Pierre Auger Observatory

The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the partic...

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Detalles Bibliográficos
Autores: Aab, A., Allekotte, Ingomar, Almela, Daniel Alejandro, Bertou, Xavier Pierre Louis, Dova, Maria Teresa, Figueira, Juan Manuel, Filevich, Alberto, Garcia, Beatriz Elena, Golup, Geraldina Tamara, Gomez Berisso, Mariano, Gómez Vitale, P. F., González, N., Hampel, Matias Rolf, Hansen, Patricia Maria, Harari, Diego Dario, Jarne, C., Mariazzi, Analisa Gabriela, Melo, Diego Gabriel, Micheletti, Maria Isabel, Mollerach, Maria Silvia, Pallotta, Juan Vicente, Platino, Manuel, Quel, Eduardo Jaime, Ristori, Pablo Roberto, Roulet, Esteban, Rovero, Adrian Carlos, Sánchez, F., Sato, R., Scarso, C., Sciutto, Sergio Juan, Supanitsky, Alberto Daniel, Taborda, O. A., Tapia, A., Videla, M., Wahlberg, Hernan Pablo, Wainberg, O., The Pierre Auger Collaboration
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2016
País:Argentina
Institución:Consejo Nacional de Investigaciones Científicas y Técnicas
Repositorio:CONICET Digital (CONICET)
Idioma:inglés
OAI Identifier:oai:ri.conicet.gov.ar:11336/125472
Acceso en línea:http://hdl.handle.net/11336/125472
Access Level:acceso abierto
Palabra clave:AUGER
MASS COMPOSITION
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
Descripción
Sumario:The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the particles into the detectors. The magnitude of the effect depends upon the zenith angle and state of development of the shower and thus provides a novel observable, (secθ)max, sensitive to the mass composition of cosmic rays above 3×1018 eV. By comparing measurements with predictions from shower simulations, we find for both of our adopted models of hadronic physics (QGSJETII-04 and EPOS-LHC) an indication that the mean cosmic-ray mass increases slowly with energy, as has been inferred from other studies. However, the mass estimates are dependent on the shower model and on the range of distance from the shower core selected. Thus the method has uncovered further deficiencies in our understanding of shower modelling that must be resolved before the mass composition can be inferred from (secθ)max.

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