Waseda Univ. Uses CALET to Measure Boron Flux in Cosmic Rays

Cosmic rays (CR) constitute high-energy particles that mainly originate outside our solar system. These primary CR interact with interstellar matter to produce secondary CR. The secondary nature of their origin is reflected in the higher abundance of light elements, such as boron (B), in secondary CR relative to the solar system. Likewise, the primary CR can be quantified in terms of the amount of carbon (C) nuclei. Consequently, measurements of the secondary-to-primary abundance ratios (as B/C) are possible. This can help realize better galactic CR propagation models by constraining their parameters that are proportional to the average material path length (λ) traversed by CR in the galaxy at high energies.

Existing studies indicate that λ follows a power-law variation. It is inversely related to E raised to the δ^th power, where E is the CR energy per nucleon and δ is called the diffusion spectral index. The galactic CR propagation can be investigated by precisely determining the energy dependence of λ.

In this regard, a team of international researchers, led by Professor Emeritus Shoji Torii from Waseda University, Japan, has now extended the measurements of secondary CR in the tera electronvolts/nucleon (TeV/n) region with high statistics and reduced systematic uncertainties. Their work, published in Physical Review Letters on December 16, 2022, involved contributions from Dr. Paolo Maestro from the University of Siena, Italy, and Dr. Yosui Akaike from Waseda University.

Akaike briefly discusses the fundamental contribution of their study. "Our research presents new direct measurements of the energy spectrum of B and the B/C flux ratio in the energy range 8.4 GeV/n to 3.8 TeV/n, based on the data collected by the CALorimetric Electron Telescope (CALET) from October 13, 2015, to February 28, 2022 aboard the International Space Station. The C energy spectrum has also been updated. The measurements indicate excellent charge identification, accurate tracking, and good energy sampling of the CR particles up to the TeV region," he says.

By analyzing the CALET data, the researchers observed that B shows a different energy spectrum from C in terms of its spectral index value: -3.047 for low energies. The index seems to harden (by 0.25) more than it does for C (by 0.19), albeit with low statistical significance, at a transition energy of around 200 GeV/n. The B/C ratio can be fitted with a single power law function with a spectral index of -0.366, even at high energies.

Further, due to the slight difference in the hardening between B and C, the researchers tried to fit a "leaky-box model" of CR propagation in the galaxy to the B/C ratio. In this approach, the CR were modeled as "leaking" from the galaxy. Their results pointed to the possibility of a non-zero residual value of λ. Physically, this implies that the primary CR cross a column density of matter within the acceleration region. They then produce new secondary B nuclei near the CR source, hardening the ratio.

"The presented results could significantly contribute to our understanding of cosmic ray propagation mechanism in supernova remnants and our galaxy. More importantly, however, pure science research can stimulate an intellectual curiosity about our universe and help us better comprehend what life might look like at places like the Moon and Mars," concludes Akaike.

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Reference

DOI: https://doi.org/10.1103/PhysRevLett.129.251103

Authors: O. Adriani,^1,2 Y. Akaike,^3,4 K. Asano,⁵ Y. Asaoka,⁵ E. Berti,^1,2 G. Bigongiari,^6,7 W. R. Binns,⁸ M. Bongi,^1,2 P. Brogi,^6,7 A. Bruno,⁹ J. H. Buckley,⁸ N. Cannady,^10,11,12 G. Castellini,¹³ C. Checchia,^6,7 M. L. Cherry,¹⁴ G. Collazuol,^15,16 G. A. de Nolfo,⁹ K. Ebisawa,¹⁷ A. W. Ficklin,¹⁴ H. Fuke,¹⁷ S. Gonzi,^1,2 T. G. Guzik,¹⁴ T. Hams,¹⁰ K. Hibino,¹⁸ M. Ichimura,¹⁹ K. Ioka,²⁰ W. Ishizaki,⁵ M. H. Israel,⁸ K. Kasahara,²¹ J. Kataoka,²² R. Kataoka,²³ Y. Katayose,²⁴ C. Kato,²⁵ N. Kawanaka,²⁰ Y. Kawakubo,¹⁴ K. Kobayashi,^3,4 K. Kohri,²⁶ H. S. Krawczynski,⁸ J. F. Krizmanic,¹¹ P. Maestro ,^6,7 P. S. Marrocchesi,^6,7 A. M. Messineo,^27,7 J. W. Mitchell,¹¹ S. Miyake,²⁸ A. A. Moiseev,^29,11,12 M. Mori,³⁰ N. Mori,² H. M. Motz,³¹ K. Munakata,²⁵ S. Nakahira,¹⁷ J. Nishimura,¹⁷ S. Okuno,¹⁸ J. F. Ormes,³² S. Ozawa,³³ L. Pacini,^1,13,2 P. Papini,² B. F. Rauch,⁸ S. B. Ricciarini,^13,2 K. Sakai,^10,11,12 T. Sakamoto,³⁴ M. Sasaki,^29,11,12 Y. Shimizu,¹⁸ A. Shiomi,³⁵ P. Spillantini,¹ F. Stolzi,^6,7 S. Sugita,³⁴ A. Sulaj,^6,7 M. Takita,⁵ T. Tamura,¹⁸ T. Terasawa,⁵ S. Torii,³ Y. Tsunesada,^36,37 Y. Uchihori,³⁸ E. Vannuccini,² J. P. Wefel,¹⁴ K. Yamaoka,³⁹ S. Yanagita,⁴⁰ A. Yoshida,³⁴ K. Yoshida,²¹ and W. V. Zober⁸

Affiliations:

¹Department of Physics Department of Physics, University of Florence, Via Sansone, 1–50019, Sesto Fiorentino, Italy

²INFN Sezione di Florence, Via Sansone, 1–50019, Sesto Fiorentino, Italy

³Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan

⁴JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan

⁵Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan

⁶Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy

⁷INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3–56127 Pisa, Italy

⁸Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA

⁹Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA

¹⁰Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA

¹¹Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA

¹²Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA

¹³Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy

¹⁴Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA

¹⁵Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy

¹⁶INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy

¹⁷Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan

¹⁸Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan

¹⁹Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan

²⁰Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwakecho, Sakyo, Kyoto 606-8502, Japan

²¹Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan

²²Waseda Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan

²³National Institute of Polar Research, 10-3, Midori-cho, Tachikawa, Tokyo 190-8518, Japan

²⁴Faculty of Engineering, Division of Intelligent Systems Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan

²⁵Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan

²⁶Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan

²⁷University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3–56127 Pisa, Italy

²⁸Department of Electrical and Electronic Systems Engineering, National Institute of Technology, Ibaraki College, 866 Nakane, Hitachinaka, Ibaraki 312-8508 Japan

²⁹Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA

³⁰Department of Physical Sciences, College of Science and Engineering, Ritsumeikan University, Shiga 525-8577, Japan

³¹Faculty of Science and Engineering, Global Center for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan

³²Department of Physics and Astronomy, University of Denver, Physics Building, Room 211, 2112 East Wesley Avenue, Denver, Colorado 80208-6900, USA

³³Quantum ICT Advanced Development Center, National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan

³⁴College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan

³⁵College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino, Chiba 275-8575, Japan

³⁶Graduate School of Science, Osaka Metropolitan University, 3-3-138, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan

³⁷Nambu Yoichiro Institute for Theoretical and Experimental Physics, Osaka Metropolitan University, 3-3-138, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan

³⁸National Institutes for Quantum and Radiation Science and Technology, 4-9-1 Anagawa, Inage, Chiba 263-8555, Japan

³⁹Nagoya University, Furo, Chikusa, Nagoya 464-8601, Japan

⁴⁰College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan

About Associate Professor Yosui Akaike

Yosui Akaike is an Associate Professor at the Waseda Research Institute for Science and Engineering at Waseda University, Japan. He has been actively involved in astronomical research for more than 15 years. During this period, he has published over 60 research papers with 200-plus co-authors. His work has been cited nearly 800 times in more than 400 documents. His research interests include cosmos, dark matter, antiprotons, cosmic ray showers, and particle telescopes. He has even worked with the CALorimetric Electron Telescope (CALET) aboard the International Space Station.

About Waseda University

Located in the heart of Tokyo, Waseda University is a leading private research university that has long been dedicated to academic excellence, innovative research, and civic engagement at both the local and global levels since 1882. The University has produced many changemakers in its history, including nine prime ministers and many leaders in business, science and technology, literature, sports, and film. Waseda has strong collaborations with overseas research institutions and is committed to advancing cutting-edge research and developing leaders who can contribute to the resolution of complex, global social issues. The University has set a target of achieving a zero-carbon campus by 2032, in line with the Sustainable Development Goals (SDGs) adopted by the United Nations in 2015.

To learn more about Waseda University, visit https://www.waseda.jp/top/en