Authors
R Alfaro, Universidad Nacional Autónoma de México
C Alvarez, Universidad Autónoma de Chiapas
J C. Arteaga-Velázquez, Universidad Michoacana de San Nicolás de Hidalgo
K P. Arunbabu, Cochin University of Science and Technology
D Avila Rojas, Universidad Nacional Autónoma de México
R Babu, Michigan Technological University
E Belmont-Moreno, Universidad Nacional Autónoma de México
K S. Caballero-Mora, Universidad Autónoma de Chiapas
T Capistrán, Universidad Nacional Autónoma de México
A Carramiñana, Instituto Nacional de Astrofísica
S Casanova, Institute of Nuclear Physics Polish Academy of Sciences
P Colín-Farias, Universidad Nacional Autónoma de México
U Cotti, Universidad Michoacana de San Nicolás de Hidalgo
J Cotzomi, Benemérita Universidad Autónoma de Puebla
S Coutiño de León, University of Wisconsin-Madison
E De la Fuente, Universidad de Guadalajara
C de León, Universidad Michoacana de San Nicolás de Hidalgo
D Depaoli, Max-Planck Institute for Nuclear Physics
R Diaz Hernandez, University of Wisconsin-Madison
J C. Díaz-Vélez, University of Wisconsin-Madison
M Durocher, Los Alamos National Laboratory
M A. DuVernois, University of Wisconsin-Madison
K Engel, University of Maryland
C Espinoza, Universidad Nacional Autónoma de México
K L. Fan, University of Maryland
N. Fraija, University of Maryland at College Park
N. Fraija, Universidad Nacional Autónoma de México
J. A. García-González, Escuela de Ingeniería y Ciencias
F. Garfias, Universidad Nacional Autónoma de México
A. Gonzalez Muñoz, Universidad Nacional Autónoma de México
M. M. González, Universidad Nacional Autónoma de México
J. A. Goodman, University of Maryland at College Park
J. P. Harding, Los Alamos National Laboratory
D. Huang, University of Maryland at College Park
F. Hueyotl-Zahuantitla, Universidad Autónoma de Chiapas
A. Iriarte, Universidad Nacional Autónoma de México
S. Kaufmann, Universidad Politecnica de Pachuca
A. Lara, Universidad Nacional Autónoma de México
J. Lee, University of Seoul
H. León Vargas, Universidad Nacional Autónoma de México
A. L. Longinotti, Universidad Nacional Autónoma de México
G. Luis-Raya, Universidad Politecnica de Pachuca
K. Malone, Los Alamos National Laboratory
O. Martinez, Benemérita Universidad Autónoma de Puebla
J. Martínez-Castro, Instituto Politécnico Nacional
J. A. Matthews, University of New Mexico
P. Miranda-Romagnoli, Universidad Autónoma del Estado de Hidalgo
E. Moreno, Benemérita Universidad Autónoma de Puebla
M. Mostafá, Temple University
A. Nayerhoda, Institute of Nuclear Physics Polish Academy of Sciences
L. Nellen, Universidad Nacional Autónoma de Mexico
T. Niembro, Harvard & Smithsonian
R. Noriega-Papaqui, Universidad Autónoma del Estado de Hidalgo
N. Omodei, Stanford University
E. G. Pérez-Pérez, Universidad Politecnica de Pachuca
C. D. Rho, Sungkyunkwan University
D. Rosa-González, Instituto Nacional de Astrofísica
E. Ruiz-Velasco, Max-Planck Institute for Nuclear Physics
James M. Ryan, University of New Hampshire, DurhamFollow
H. Salazar, Benemérita Universidad Autónoma de Puebla
D. Salazar-Gallegos, Michigan State University
A. Sandoval, Universidad Nacional Autónoma de México
J. Serna-Franco, Universidad Nacional Autónoma de México
A. J. Smith, University of Maryland at College Park
Y. Son, University of Seoul
R. W. Springer, University of Utah
O. Tibolla, Universidad Politecnica de Pachuca
K. Tollefson, Michigan State University
I. Torres, Instituto Nacional de Astrofísica
R. Turner, Michigan Technological University
F. Ureña-Mena, Instituto Nacional de Astrofísica
E. Varela, Benemérita Universidad Autónoma de Puebla
L. Villaseñor, Benemérita Universidad Autónoma de Puebla
X. Wang, Michigan Technological University
I. J. Watson, University of Seoul
E. Willox, University of Maryland at College Park
S. Yun-Cárcamo, University of Maryland at College Park
H. Zhou, Shanghai Jiao Tong University
Abstract
Galactic cosmic rays (GCRs) are charged particles that reach the heliosphere almost isotropically in a wide energy range. In the inner heliosphere, the GCR flux is modulated by solar activity so that only energetic GCRs reach the lower layers of the solar atmosphere. In this work, we propose that high-energy GCRs can be used to explore the solar magnetic fields at low coronal altitudes. We used GCR data collected by the High-Altitude Water Cherenkov observatory to construct maps of GCR flux coming from the Sun’s sky direction and studied the observed GCR deficit, known as Sun shadow (SS), over a 6 yr period (2016–2021) with a time cadence of 27.3 days. We confirm that the SS is correlated with sunspot number, but we focus on the relationship between the photospheric solar magnetic field measured at different heliolatitudes and the relative GCR deficit at different energies. We found a linear relationship between the relative deficit of GCRs represented by the depth of the SS and the solar magnetic field. This relationship is evident in the observed energy range of 2.5–226 TeV, but is strongest in the range of 12.4 33.4 TeV, which implies that this is the best energy range to study the evolution of magnetic fields in the low solar atmosphere.
Department
Space Science Center
Publication Date
4-25-2024
Journal Title
The Astrophysical Journal
Publisher
American Astronomical Society
Recommended Citation
R. Alfaro et al 2024 ApJ 966 67
Rights
© 2024. The Author(s).
Comments
This is an open access article published by American Astronomical Society in The Astrophysical Journal in 2024, available online: https://dx.doi.org/10.3847/1538-4357/ad3208