<p>Large Forbush decreases (FDs) in the Galactic cosmic ray flux were observed by the paired neutron monitor (SNM) and the vertical channel of the muon detector (SMDV) at the Antarctic Syowa Station in May and October, 2024. The maximum count rate depressions in SNM and SMDV are <InlineEquation ID="IEq1"> <EquationSource Format="TEX">$\sim$</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>10% and <InlineEquation ID="IEq2"> <EquationSource Format="TEX">$\sim$</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>5% in the May FD, respectively. In the October FD, the observed count rates decreased in two steps following two successive interplanetary shocks. The maximum count rate depression recorded by SNM (SMDV) is <InlineEquation ID="IEq3"> <EquationSource Format="TEX">$\sim$</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>7% (<InlineEquation ID="IEq4"> <EquationSource Format="TEX">$\sim$</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>3%) in the first step, while it is <InlineEquation ID="IEq5"> <EquationSource Format="TEX">$\sim$</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>8% (<InlineEquation ID="IEq6"> <EquationSource Format="TEX">$\sim$</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>5%) in the second step. It is demonstrated that the SNM count rate fraction relative to the total count rate in SNM and SMDV (<InlineEquation ID="IEq7"> <EquationSource Format="TEX">$F_n$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi>F</mi> <mi>n</mi> </msub> </math></EquationSource> </InlineEquation>) is a good real-time indicator of the temporal variation of the cosmic ray rigidity spectrum (<InlineEquation ID="IEq8"> <EquationSource Format="TEX">$\Delta \Gamma (P,t)$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi mathvariant="normal">Δ</mi> <mi mathvariant="normal">Γ</mi> <mo stretchy="false">(</mo> <mi>P</mi> <mo>,</mo> <mi>t</mi> <mo stretchy="false">)</mo> </mrow> </math></EquationSource> </InlineEquation>), which is an important parameter for identifying the physical processes responsible for FD effects. It is verified that the variation of <InlineEquation ID="IEq9"> <EquationSource Format="TEX">$F_n$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi>F</mi> <mi>n</mi> </msub> </math></EquationSource> </InlineEquation> is consistent with <InlineEquation ID="IEq10"> <EquationSource Format="TEX">$\Delta \Gamma (P,t)$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi mathvariant="normal">Δ</mi> <mi mathvariant="normal">Γ</mi> <mo stretchy="false">(</mo> <mi>P</mi> <mo>,</mo> <mi>t</mi> <mo stretchy="false">)</mo> </mrow> </math></EquationSource> </InlineEquation> calculated from the Global Fitting Analysis (GFA) at the Syowa Station. <InlineEquation ID="IEq11"> <EquationSource Format="TEX">$F_n$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi>F</mi> <mi>n</mi> </msub> </math></EquationSource> </InlineEquation> also shows a significant increase of <InlineEquation ID="IEq12"> <EquationSource Format="TEX">$\Delta \Gamma (P,t)$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi mathvariant="normal">Δ</mi> <mi mathvariant="normal">Γ</mi> <mo stretchy="false">(</mo> <mi>P</mi> <mo>,</mo> <mi>t</mi> <mo stretchy="false">)</mo> </mrow> </math></EquationSource> </InlineEquation> during the ground-level enhancement (GLE) due to solar energetic particles on May 11 superposed on the FD recovery phase, implying that the total (Galactic + solar) cosmic ray spectrum is softened due to the contribution from GLE intensity steeply increasing with decreasing rigidity. This implies that <InlineEquation ID="IEq13"> <EquationSource Format="TEX">$F_n$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mi>F</mi> <mi>n</mi> </msub> </math></EquationSource> </InlineEquation> can be also a good indicator of small GLEs which are sometimes difficult to identify in the count rate variation when masked by an FD and the associated diurnal anisotropy.</p> Graphic Abstract <p></p>

Real-time monitoring of the rigidity spectrum of large Forbush decreases in May and October 2024 with the paired neutron monitor and muon detector at the Antarctic Syowa Station

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2026年3月3日

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Yuki Hayashi,
Kazuoki Munakata,
Masayoshi Kozai,
Ryuho Kataoka,
Akira Kadokura,
Chihiro Kato,
Naoko Miyashita,
Shoko Miyake,
Kiyoka Murase,
Marcus L. Duldig,
David Ruffolo,
Warit Mitthumsiri,
Pradiphat Muangha,
Alejandro Sáiz,
Surujdheo Seunarine,
Paul A. Evenson,
Pierre-Simon Mangeard,
Kazumasa Iwai,
Hiroaki Menjo,
Ezequiel Echer,
Alisson Dal Lago,
Marlos Rockenbach,
Nelson Jorge Schuch,
Jose V. Bageston,
Carlos Roberto Braga,
Hala Khalid Al Jassar,
Madan Mohan Sharma,
Naser Burahmah,
Fahad Zaman,
Ismail Sabbah,
Takao Kuwabara,
Ding Chen,
Jing Huang

摘要

Large Forbush decreases (FDs) in the Galactic cosmic ray flux were observed by the paired neutron monitor (SNM) and the vertical channel of the muon detector (SMDV) at the Antarctic Syowa Station in May and October, 2024. The maximum count rate depressions in SNM and SMDV are $\sim$ $\sim$ 10% and $\sim$ $\sim$ 5% in the May FD, respectively. In the October FD, the observed count rates decreased in two steps following two successive interplanetary shocks. The maximum count rate depression recorded by SNM (SMDV) is $\sim$ $\sim$ 7% ( $\sim$ $\sim$ 3%) in the first step, while it is $\sim$ $\sim$ 8% ( $\sim$ $\sim$ 5%) in the second step. It is demonstrated that the SNM count rate fraction relative to the total count rate in SNM and SMDV ( $F_n$ $F_{n}$ ) is a good real-time indicator of the temporal variation of the cosmic ray rigidity spectrum ( $\Delta \Gamma (P,t)$ $Δ Γ (P, t)$ ), which is an important parameter for identifying the physical processes responsible for FD effects. It is verified that the variation of $F_n$ $F_{n}$ is consistent with $\Delta \Gamma (P,t)$ $Δ Γ (P, t)$ calculated from the Global Fitting Analysis (GFA) at the Syowa Station. $F_n$ $F_{n}$ also shows a significant increase of $\Delta \Gamma (P,t)$ $Δ Γ (P, t)$ during the ground-level enhancement (GLE) due to solar energetic particles on May 11 superposed on the FD recovery phase, implying that the total (Galactic + solar) cosmic ray spectrum is softened due to the contribution from GLE intensity steeply increasing with decreasing rigidity. This implies that $F_n$ $F_{n}$ can be also a good indicator of small GLEs which are sometimes difficult to identify in the count rate variation when masked by an FD and the associated diurnal anisotropy.

Graphic Abstract