An improved solar neutron telescope installed at a very high altitude in México

Galicia, J. F. Valdés; Muraki, Y.; Tsujihara, H.; Sako, T.; Musalém, O.; Hurtado, A.; González, L. X.; Matsubara, Y.; Watanabe, Kyoko; Hirano, N.; Tateiwa, N.; Shibata, S.; Sakai, Takehiro

doi:10.1016/j.nima.2004.06.148

Cited by 26 publications

(8 citation statements)

References 10 publications

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“…Because all of the data could not be fitted with a single power Ϫ1 sr law, we fitted only the data between 17:40 and 17:47 UT, which is the interval corresponding to 100 MeV-400 MeV neutrons. Interestingly, in an independent analysis using a different attenuation model (Dorman et al 1999) and efficiency calculation (Valdés-Galicia et al 2004), the Mexico SNT data give a quite consistent result of . This 27 Ϫ4.0 Ϫ1 Ϫ1…”

Section: Analysis and Discussionmentioning

confidence: 79%

“…At the GOES soft X-ray peak time of the flare (17:40 UT), Mexico and Bolivia were suitable places to observe solar neutrons in the SNT network (Tsuchiya et al 2001;Valdés-Galicia et al 2004). At Sierra Negra (E262Њ .7, N19Њ .0; 4580 m above sea level [a.s.l.])…”

Section: Observationsmentioning

confidence: 99%

“…Below the scintillators, 4 layers of proportional counters are also aligned to measure the direction and energy of the recoil particles. Details of the detector and its performance are described in Valdés-Galicia et al (2004). The Bolivia SNT is simpler.…”

Section: Observationsmentioning

confidence: 99%

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Long-lived Solar Neutron Emission in Comparison with Electron-produced Radiation in the 2005 September 7 Solar Flare

Sako

Watanabe

Muraki

et al. 2006

ApJ

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Strong signals of neutral emissions were detected in association with a solar flare that occurred on 2005 September 7. They were produced by both relativistic ions and electrons. In particular, relativistic neutrons were observed with the solar neutron telescopes (SNTs) located at Mount Chacaltaya in Bolivia and Mount Sierra Negra in Mexico and with neutron monitors (NMs) at Chacaltaya and Mexico City with high statistical significances. At the same time, hard X-rays and g-rays, which were predominantly emitted by high-energy electrons, were detected by the Geotail and the INTEGRAL satellites. We found that a model of the impulsive neutron emission at the time of the X-ray/ g-ray peak can explain the main peaks of all the detected neutron signals, but failed to explain the long tailed decaying phase. An alternative model, in which the neutron emission follows the X-ray/g-ray profile, also failed to explain the long tail. These results indicate that the acceleration of ions began at the same time as the electrons but that ions were continuously accelerated or trapped longer than the electrons in the emission site. We also demonstrate that the neutron data observed by multienergy channels of SNTs put constraints on the neutron spectrum.

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Section: Analysis and Discussionmentioning

confidence: 79%

Section: Observationsmentioning

confidence: 99%

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Long-lived Solar Neutron Emission in Comparison with Electron-produced Radiation in the 2005 September 7 Solar Flare

Sako

Watanabe

Muraki

et al. 2006

ApJ

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“…The SNT includes a set of proportional counters to determine the arrival direction of entrance particles, which is why it is called a Solar Neutron Telescope (SNT). Technical details of the SNT are available in [2][3][4][5].…”

Section: Solar Neutron Telescope (Snt) At Mt Sierra Negramentioning

confidence: 99%

Simultaneous Observation of Solar Neutrons from the ISS and High Mountain Observatories in association with a flare on July 8

Muraki

López

Koga

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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An M6.5-class flare was observed at N12E56 of the solar surface at 16:06 UT on July 8, 2014. In association with this flare, solar neutron detectors located on two high mountains, Mt. Sierra Negra and Chacaltaya and at the space station observed enhancements in the neutral channel. The authors analysed these data and a possible scenario of enhancements produced by high-energy protons and neutrons is proposed, using the data from continuous observation of a solar surface by the ultraviolet telescope onboard the Solar Dynamical Observatory (SDO). IntroductionOn July 8, 2014, a solar flare occurred on the solar surface at N12E56. According to the GOES observation, the flare started at 16:06 UT and peaked at 16:20 UT, with a flare intensity of M6.5. In association with this flare, hard X-rays were detected by the GBM instrument onboard the FERMI satellite. The intensity of the hard X-rays peaked at 16:13 at around 400 photons/detector/sec within the range 100-300 keV. The solar flare was continuously monitored before the flare by the ultraviolet telescope onboard the Solar Dynamical Observatory (SDO).

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“…Sierra Negra (about 4,600 m) in Mexico. The hut of the SciCRT is neighboring to that of Mexico SNT [14]. The SciCRT aims to observe highenergy solar neutrons to contribute to elucidate the acceleration mechanism of ions by solar flares and muons for studying the transport of galactic cosmic rays in the heliosphere and space weather.…”

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confidence: 99%

Sensitivity of the SciBar Cosmic Ray Telescope (SciCRT) to solar neutrons

Sasai¹,

Matsubara²,

Itow³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The SciBar Cosmic Ray Telescope (SciCRT) is aimed to help elucidate the acceleration mechanism of high-energy ions that may produce neutrons at the Sun. It is a fully active scintillator tracker which consists of 14,848 plastic scintillator bars, originally constructed for accelerator neutrino oscillation experiments. The SciCRT; it has a huge detector volume compared with conventional Solar Neutron Telescopes (SNTs), e.g. 15 times larger than Mexico SNT. Furthermore, the SciCRT can measure the energy deposition of each particle as neutron ADC data which have not been registered before. Neutron ADC data provide us with a precise measurement of energies deposited at the detector. The SciCRT was deployed at the summit of Mt. Sierra Negra (4,600 m) and began to acquire data in September 2013. Then we partially upgraded the DAQ system developed originally for an accelerator experiment, as the readout rate of the DAQ system was significantly limited for our experiment. This paper highlights sensitivity numerical studies of solar neutrons that the SciCRT is able to register. At first, we focus in the accuracy to determine the spectrum power-law index, assuming an instantaneous emission of solar neutrons. This is required to determine the power-law index within an error of ±1.0 in order to discuss the efficiency of the acceleration. Then in the case of the fixed power-law index, we discuss the capability of discriminating three different lengths of emission times: 0 min, 5 min, and 8 min. Finally we evaluate whether it is possible to discriminate a different combination of these two parameters simultaneously. Thus, we show that data from the SciCRT will unlock the degeneracy problem amid the emission time and the energy spectrum of solar neutrons.35th International Cosmic Ray Conference

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An improved solar neutron telescope installed at a very high altitude in México

Cited by 26 publications

References 10 publications

Long-lived Solar Neutron Emission in Comparison with Electron-produced Radiation in the 2005 September 7 Solar Flare

Long-lived Solar Neutron Emission in Comparison with Electron-produced Radiation in the 2005 September 7 Solar Flare

Simultaneous Observation of Solar Neutrons from the ISS and High Mountain Observatories in association with a flare on July 8

Sensitivity of the SciBar Cosmic Ray Telescope (SciCRT) to solar neutrons

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