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Discovery of Gamma Rays from the Quiescent Sun with HAWC.
Albert, A; Alfaro, R; Alvarez, C; Arteaga-Velázquez, J C; Avila Rojas, D; Ayala Solares, H A; Babu, R; Belmont-Moreno, E; Brisbois, C; Caballero-Mora, K S; Capistrán, T; Carramiñana, A; Casanova, S; Chaparro-Amaro, O; Cotti, U; Cotzomi, J; Coutiño de León, S; De la Fuente, E; Diaz Hernandez, R; Dingus, B L; DuVernois, M A; Durocher, M; Díaz-Vélez, J C; Ellsworth, R W; Engel, K; Espinoza, C; Fan, K L; Fang, K; Fernández Alonso, M; Fleischhack, H; Fraija, N; García-González, J A; Garfias, F; González, M M; Goodman, J A; Harding, J P; Hernandez, S; Hinton, J; Huang, D; Hueyotl-Zahuantitla, F; Hüntemeyer, P; Iriarte, A; Joshi, V; Kaufmann, S; Lee, J; Linnemann, J T; Longinotti, A L; Luis-Raya, G; Malone, K; Martinez, O.
Affiliation
  • Albert A; Physics Division, Los Alamos National Laboratory, Los Alamos, NM 87544, USA.
  • Alfaro R; Instituto de F'isica, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Alvarez C; Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, México.
  • Arteaga-Velázquez JC; Universidad Michoacana de San Nicolás de Hidalgo, Morelia, Mexico.
  • Avila Rojas D; Instituto de F'isica, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Ayala Solares HA; Department of Physics, Pennsylvania State University, University Park, PA, USA.
  • Babu R; Department of Physics, Michigan Technological University, Houghton, MI, USA.
  • Belmont-Moreno E; Instituto de F'isica, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Brisbois C; Department of Physics, University of Maryland, College Park, MD, USA.
  • Caballero-Mora KS; Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, México.
  • Capistrán T; Instituto de Astronom'ia, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Carramiñana A; Instituto Nacional de Astrof'isica, Óptica y Electrónica, Puebla, Mexico.
  • Casanova S; Instytut Fizyki Jadrowej im Henryka Niewodniczanskiego Polskiej Akademii Nauk, IFJ-PAN, Krakow, Poland.
  • Chaparro-Amaro O; Centro de Investigaci'on en Computaci'on, Instituto Polit'ecnico Nacional, M'exico City, M'exico.
  • Cotti U; Universidad Michoacana de San Nicolás de Hidalgo, Morelia, Mexico.
  • Cotzomi J; Facultad de Ciencias F'isico Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla, Mexico.
  • Coutiño de León S; Department of Physics, University of Wisconsin-Madison, Madison, WI, USA.
  • De la Fuente E; Departamento de F'isica, Centro Universitario de Ciencias Exactase Ingenierias, Universidad de Guadalajara, Guadalajara, Mexico.
  • Diaz Hernandez R; Instituto Nacional de Astrof'isica, Óptica y Electrónica, Puebla, Mexico.
  • Dingus BL; Physics Division, Los Alamos National Laboratory, Los Alamos, NM 87544, USA.
  • DuVernois MA; Department of Physics, University of Maryland, College Park, MD, USA.
  • Durocher M; Department of Physics, University of Wisconsin-Madison, Madison, WI, USA.
  • Díaz-Vélez JC; Physics Division, Los Alamos National Laboratory, Los Alamos, NM 87544, USA.
  • Ellsworth RW; Departamento de F'isica, Centro Universitario de Ciencias Exactase Ingenierias, Universidad de Guadalajara, Guadalajara, Mexico.
  • Engel K; Department of Physics, University of Maryland, College Park, MD, USA.
  • Espinoza C; Department of Physics, University of Maryland, College Park, MD, USA.
  • Fan KL; Instituto de F'isica, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Fang K; Department of Physics, University of Maryland, College Park, MD, USA.
  • Fernández Alonso M; Department of Physics, University of Wisconsin-Madison, Madison, WI, USA.
  • Fleischhack H; Department of Physics, Pennsylvania State University, University Park, PA, USA.
  • Fraija N; Department of Physics, Catholic University of America, 620 Michigan Avenue NE, Washington, DC 20064.
  • García-González JA; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
  • Garfias F; Center for Research and Exploration in Space Science and Technology, NASA/GSFC, Greenbelt, MD 20771.
  • González MM; Instituto de Astronom'ia, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Goodman JA; Tecnologico de Monterrey, Escuela de Ingeniería y Ciencias, Avenue Eugenio Garza Sada 2501, Monterrey, N.L., Mexico, 64849.
  • Harding JP; Instituto de Astronom'ia, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Hernandez S; Instituto de Astronom'ia, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Hinton J; Department of Physics, University of Maryland, College Park, MD, USA.
  • Huang D; Physics Division, Los Alamos National Laboratory, Los Alamos, NM 87544, USA.
  • Hueyotl-Zahuantitla F; Instituto de F'isica, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Hüntemeyer P; Max-Planck Institute for Nuclear Physics, 69117 Heidelberg, Germany.
  • Iriarte A; Department of Physics, Michigan Technological University, Houghton, MI, USA.
  • Joshi V; Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, México.
  • Kaufmann S; Department of Physics, Michigan Technological University, Houghton, MI, USA.
  • Lee J; Instituto de Astronom'ia, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
  • Linnemann JT; Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen, Germany.
  • Longinotti AL; Universidad Politecnica de Pachuca, Pachuca, Hgo, Mexico.
  • Luis-Raya G; University of Seoul, Seoul, Rep. of Korea.
  • Malone K; Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA.
  • Martinez O; Instituto de Astronom'ia, Universidad Nacional Autónoma de México, Ciudad de Mexico, Mexico.
Phys Rev Lett ; 131(5): 051201, 2023 Aug 04.
Article in En | MEDLINE | ID: mdl-37595214
ABSTRACT
We report the first detection of a TeV γ-ray flux from the solar disk (6.3σ), based on 6.1 years of data from the High Altitude Water Cherenkov (HAWC) observatory. The 0.5-2.6 TeV spectrum is well fit by a power law, dN/dE=A(E/1 TeV)^{-γ}, with A=(1.6±0.3)×10^{-12} TeV^{-1} cm^{-2} s^{-1} and γ=3.62±0.14. The flux shows a strong indication of anticorrelation with solar activity. These results extend the bright, hard GeV emission from the disk observed with Fermi-LAT, seemingly due to hadronic Galactic cosmic rays showering on nuclei in the solar atmosphere. However, current theoretical models are unable to explain the details of how solar magnetic fields shape these interactions. HAWC's TeV detection thus deepens the mysteries of the solar-disk emission.
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Phys Rev Lett Year: 2023 Document type: Article Affiliation country:
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Phys Rev Lett Year: 2023 Document type: Article Affiliation country: