Solar Cycle Dependence of the Diurnal Anisotropy of 0.6 TeV Cosmic-ray Intensity Observed with the Matsushiro Underground Muon Detector

• Published in: The Astrophysical journal Vol. 712; no. 2; pp. 1100 - 1106
• Main Authors: Munakata, K, Mizoguchi, Y, Kato, C, Yasue, S, Mori, S, Takita, M, Kóta, J
• Format: Journal Article
• Language: English
• Published: Bristol IOP Publishing 01.04.2010; IOP
• Subjects: AIR; ANISOTROPY; Astronomy; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ATMOSPHERES; COSMIC MUONS; COSMIC RADIATION; DAILY VARIATIONS; Earth, ocean, space; ELECTRIC FIELDS; ELEMENTARY PARTICLES; ENERGY RANGE; Exact sciences and technology; FERMIONS; FLUIDS; GASES; HELIOSPHERE; INTERPLANETARY MAGNETIC FIELDS; IONIZING RADIATIONS; LEPTONS; LEVELS; MAGNETIC FIELDS; MAIN SEQUENCE STARS; MUONS; ORBITS; RADIATIONS; SECONDARY COSMIC RADIATION; SOLAR ACTIVITY; SOLAR ATMOSPHERE; SOLAR CYCLE; SOLAR WIND; STARS; STARSPOTS; STELLAR ACTIVITY; STELLAR ATMOSPHERES; STELLAR WINDS; SUN; SUNSPOTS; TEV RANGE; UNDERGROUND; VARIATIONS; Heliosphere; cosmic rays; Anisotropy; Intensity; Sun: heliosphere; Solar cycle; Sun: activity; Cosmic radiation; Sun; Muons
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/712/2/1100

We analyze the temporal variation of the diurnal anisotropy of sub-TeV cosmic-ray intensity observed with the Matsushiro (Japan) underground muon detector over two full solar activity cycles in 1985-2008. We find an anisotropy component in the solar diurnal anisotropy superimposed on the Compton-Getting anisotropy due to Earth's orbital motion around the Sun. The phase of this additional anisotropy is almost constant at {approx}15:00 local solar time corresponding to the direction perpendicular to the average interplanetary magnetic field at Earth's orbit, while the amplitude varies between a maximum (0.043% +- 0.002%) and minimum ({approx}0.008% +- 0.002%) in a clear correlation with the solar activity. We find a significant time lag between the temporal variations of the amplitude and the sunspot number (SSN) and obtain the best correlation coefficient of +0.74 with the SSN delayed for 26 months. We suggest that this anisotropy might be interpreted in terms of the energy change due to the solar-wind-induced electric field expected for galactic cosmic rays (GCRs) crossing the wavy neutral sheet. The average amplitude of the sidereal diurnal variation over the entire period is 0.034% +- 0.003%, which is roughly one-third of the amplitude reported from air shower and deep-underground muon experiments monitoring multi-TeV GCR intensity suggesting a significant attenuation of the anisotropy due to the solar modulation. We find, on the other hand, only a weak positive correlation between the sidereal diurnal anisotropy and the solar activity cycle in which the amplitude in the 'active' solar activity epoch is about twice the amplitude in the 'quiet' solar activity epoch. This implies that only one-fourth of the total attenuation varies in correlation with the solar activity cycle and/or the solar magnetic cycle. We finally examine the temporal variation of the 'single-band valley depth' (SBVD) quoted by the Milagro experiment and, in contrast with recent Milagro's report, we find no steady increase in the Matsushiro observations in a seven-year period between 2000 and 2007. We suggest, therefore, that the steady increase of the SBVD reported by the Milagro experiment is not caused by the decreasing solar modulation in the declining phase of the 23rd solar activity cycle.