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Analysis of Forbush Decreases Observed Using a Muon Telescope in Antarctica Starting on 21 June 2015 * Chinese Physics C Vol. 42, No. 12 (2018) 125001 Analysis of Forbush decreases observed using a muon telescope in Antarctica starting on 21 June 2015 * De-Hong Huang(黄德宏)1;1) Hong-Qiao Hu(胡红桥)1 Ji-Long Zhang(张吉龙)2;2) Hong Lu(卢红)2 Da-Li Zhang(张大力)2 Bin-Shen Xue(薛炳森)3 Jing-Tian Lu(吕景天)3 1 SOA Key Laboratory for Polar Science, Polar Research Institute of China, Shanghai 200136, China 2 Institute of High Energy Physics (IHEP), Chinese Academy of Sciences (CAS), Beijing 100049, China 3 Key Laboratory of Space Weather, National Center for Space Weather, China Meteorological Administration, Beijing 10081, China Abstract: A cosmic-ray muon telescope has been collecting data since the end of 2014, which was shortly after the telescope was built in the Zhongshan Station of Antarctica. The telescope is the first observation device to be built by Chinese scientists in Antarctica. The pressure change is very strong in Zhongshan station. The count rate of the pressure correction results shows that the large variations in the count rate are likely caused by pressure fluctuations. During the period from 18 June to 22 June 2015, four halo coronal mass ejections (CMEs) were ejected from the Sun. These CMEs initiated a series of Forbush decreases (FD) when they reached the Earth. We conducted a comprehensive study of the intensity fluctuations of galactic cosmic rays recorded during FDs. The intensity fluctuations used in this study were collected by cosmic ray detectors of multiple stations (Zhongshan, McMurdo, South Polar, and Nagoya), and the solar wind measurements were collected by ACE and WIND. The profile of the FD of 22 June demonstrated a four-step decrease. The traditional one- or two-step FD classification method does not adequately explain the FD profile results. The interaction between the faster CME that occurred on 21 June 2015 and the two slow CMEs of the earlier few days should be considered. The cosmic ray intensities of the South Pole, McMurdo, and Zhongshan stations have similar hourly variations, whereas the galactic cosmic rays recorded between polar and non-polar locations are distinct. The FD pre-increase of 22 June 2015 for the Nagoya muon telescope (non-polar location) lags those of the McMurdo and Zhongshan stations (polar locations) by 1 h. The FD onset of 22 June 2015 for the Nagoya muon telescope lags those of the polar locations by 1 h. Keywords: cosmic ray, muon telescope, neutron monitor, CME, Forbush decrease PACS: 95.55.Vj , 96.40.Cd, 96.60.Wh DOI: 10.1088/1674-1137/42/12/125001 1 Introduction recorded not only from the Earth but also from space. The galactic cosmic ray (GCR) intensity measurements The cosmic ray intensity decreased during the mag- collected from the Pioneer V spacecraft show that the netic storm that occurred during April 25{30, 1937. This FD was due to the Sun and was unrelated to the Earth event was reported by Forbush [1], and it came to be re- and its magnetic field [6]. After PAMELA was launched ferred to as the Forbush decrease (FD) in the 1950s. Hess in 2006, GCR spectra were measured directly with suffi- and Demmelmair confirmed the cosmic ray decrease phe- cient statistics to observe FDs [7]. nomenon [2]. To explain the FD, Chapman assumed that Interplanetary coronal mass ejections (ICMEs), the the magnetic field of the equatorial ring-current protects interplanetary counterparts of coronal mass ejections the Earth from the approaching cosmic ray via shielding (CMEs), are large magnetized clouds of plasma, ejected [3]. More detailed calculations showed that the influ- by the Sun and expelled into heliosphere. If the speed of ence of enhanced ring-current will lead to an increase in the ICME exceeds that of the ambient solar wind by an cosmic ray intensity, rather than to its decrease [4]. Us- amount greater than the fast magnetosonic wave speed, a ing neutron monitors (NMs), Simpson showed that the shock wavefront and a magnetic sheath region are formed FD is not produced by geomagnetic field variations [5]. between the shock and the ICME leading edge. FDs Since the first years of the space era, FDs have been caused by the ICMEs are sporadic (non-recurrent) and Received 6 November 2017, Revised 25 August 2018, Published online 25 October 2018 ∗ Supported by NSFC (11575204) 1) E-mail: [email protected] 2) E-mail: [email protected] ©2018 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd 125001-1 Chinese Physics C Vol. 42, No. 12 (2018) 125001 are characterized by fast decreases. FDs can drop to the the alpha magnetic spectrometer onboard ISS measures minimum within approximately a day, but their grad- particles in the GV{TV rigidity range. Thus, it only pro- ual recovery phase can last several days. The magnitude vides high-energy solar energetic particles (SEPs) events of an FD, within the energy range of the NM, varies at ∼1 GV from 2011 to 2016 [16]. The major advan- from a few percent to close to 30% (for example, the FD tage of cosmic ray detectors on the ground is that the of 29 October 2003). Sanderson et al. (1991) have at- detection area is very large. Ground detectors (neutron tempted to measure the effect of turbulence in the post monitor and muon telescope) can provide the intensity shock region by measuring the radial diffusion coefficient of cosmic rays from 500 MeV to 100 GeV with sufficient from the magnetic field data, and relating this to the statistics. The geomagnetic cutoff rigidity of a detec- magnitude of the first-step FD [8]. Lockwood et al. ob- tor determines the cosmic ray energy that reaches each served that an FD is more likely to occur following a observation station. Multiple space and ground observa- shock in which the magnetic field and plasma parame- tions are carried out simultaneously to provide comple- ters are strongly enhanced. Their results indicate that mentary observations. a decrease in cosmic ray intensity may be produced by Since 1951, ground observations have been carried a smaller diffusion coefficient in the region behind the out via NMs around the world. The muon detectors com- shock [9]. A simple model for propagating diffusive bar- plement NMs by monitoring cosmic ray modulations oc- riers was presented by Wibberenz et al. [10]. In this curring at slightly higher energies and provide measure- work, FDs can be interpreted in terms of radially prop- ments of numerous muon arrival directions. The surface agating barriers with a reduced (radial) diffusion coef- muon detectors can detect events with a median primary ficient. Cane (2000) concluded that sporadic FDs can energy of 50{100 GeV, whereas NMs only detect energy be divided into three types: FDs caused by only shocks, of 10{40 GeV. Global muon detector networks (GMDNs) FDs caused by only ICMEs, and FDs caused by both were established in March 2006 to monitor space environ- shocks and ICMEs [11]. The traditional FD model pre- ments. The networks include multidirectional detectors dicts that an ICME and its shock reduce the GCR inten- (36 m2) in Nagoya, Japan, a hodoscope-type cosmic ray sity via a two-step profile. After analyzing 233 ICMEs, detector (9 m2) in Kuwait, a muon detector (36 m2 ) which should have created two-step FDs, Jordan et al. in Sao Martinho, Brazil, and a muon detector (9 m2) in concluded that small-scale interplanetary magnetic field Hobart, Australia [17]. (IMF) structures, which are generally ignored, can con- A new muon-neutron telescope was set up in Yang- tribute to a variety of FD profiles [12]. bajing in 2007 [18]. The Yangbajing Cosmic Ray Obser- An FD caused by corotating interacting regions vatory is located at a latitude of 30.11°N, a longitude of (CIRs) formed by the interaction between a fast solar 90.53°E, and an altitude of 4300 m above sea level. Us- wind from a coronal hole and a slow solar wind can be ing IGRF1995, the vertical cutoff rigidity of cosmic rays recurrent. A recurrent FD has a long decrease phase. is determined to be 14.1 GV. The average duration of the recurrent FDs is approxi- By the end of 2014, a cosmic-ray muon telescope was mately 10{14 days. Generally, the decrease and recovery installed at Zhongshan Station in Antarctica [19]. It is lo- phases of the GCR intensity are symmetric [13]. cated at sea level with a latitude of 69.4°S and a longitude An FD's profile may vary from one event to an- of 76.4°E. Using IGRF1995, the vertical cutoff rigidity of other because the interplanetary medium disturbance is cosmic-ray protons at Zhongshan Station is determined a result of multiple factors. Cosmic-ray-based spectral to be 0.07 GV. The observation data are sent to China variations and anisotropy associated with an FD pro- via a satellite link released through a network. Every vide valuable information to understand the interplane- hour, the raw data of the muon telescope are transmit- tary medium. Prior to the discovery of the solar winds ted from Zhongshan station to Institute of High Energy and IMFs, only FDs were observed in the data. Con- Physics (IHEP) in Beijing. The data are published on sequently, valuable historical information was collected the Internet in real time [20]. but not properly analyzed. Ground-based observations Between 18 and 22 June 2015, four halo CMEs were of cosmic rays are an important aspect of space weather ejected toward the Earth and initiated a series FDs.
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