Solar neutron and proton production during the 1990 May 24 cosmic-ray flare increases

Debrunner, H.; Lockwood, J. A.; Ryan, J. M.

doi:10.1086/172712

Cited by 52 publications

(38 citation statements)

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“…Besides prominent microwave ) and hard X-ray (HXR; Pelaez et al 1992) emission, this renowned X9/1B flare simultaneously produced energetic neutrons, protons, and γ -rays, and has since been studied extensively (Shea et al 1991;Debrunner et al 1992Debrunner et al , 1993Debrunner et al , 1997Kocharov et al 1994Kocharov et al , 1996Torsti et al 1996;Vilmer et al 2003). The γ -ray lightcurve up to 95 MeV measured by the PHEBUS detector on the GRANAT spacecraft shows two peaks at 20:48:12 and 20:48:36 UT, respectively (Debrunner et al 1997).…”

Section: Observation and Analysismentioning

confidence: 99%

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

Liu

et al. 2013

ApJ

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Using Big Bear Solar Observatory film data recently digitized at NJIT, we investigate a Moreton wave associated with an X9 flare on 1990 May 24, as well as its interactions with four filaments F1-F4 located close to the flaring region. The interaction yields interesting insight into physical properties of both the wave and the filaments. The first clear Moreton wavefront appears at the flaring-region periphery at approximately the same time as the peak of a microwave burst and the first of two γ -ray peaks. The wavefront propagates at different speeds ranging from 1500-2600 km s −1 in different directions, reaching as far as 600 Mm away from the flaring site. Sequential chromospheric brightenings are observed ahead of the Moreton wavefront. A slower diffuse front at 300-600 km s −1 is observed to trail the fast Moreton wavefront about one minute after the onset. The Moreton wave decelerates to ∼550 km s −1 as it sweeps through F1. The wave passage results in F1's oscillation which is featured by ∼1 mHz signals with coherent Fourier phases over the filament, the activation of F3 and F4 followed by gradual recovery, but no disturbance in F2. Different height and magnetic environment together may account for the distinct responses of the filaments to the wave passage. The wavefront bulges at F4, whose spine is oriented perpendicular to the upcoming wavefront. The deformation of the wavefront is suggested to be due to both the forward inclination of the wavefront and the enhancement of the local Alfvén speed within the filament channel.

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Section: Observation and Analysismentioning

confidence: 99%

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

Liu

et al. 2013

ApJ

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“…The value of the solar zenith angle varied from 29 to 65 for different stations located at different altitudes from the sea level to 680 g/cm 2 (see Table 1). Debrunner et al (1993) and Kovaltsov et al (1993) noted that the observations of this event disagreed with Eq. (5), which can only be used when the Sun is near zenith i.e.…”

Section: The Dependence Of the Response Of Nm To Solar Neutrons On Obmentioning

confidence: 81%

“…Thus, the nucleons scattered into large angles play a significant role as well. Debrunner et al (1993) showed that the observations of the 24 May 1990 SNE can be fitted by calculations of S n (Debrunner et al, 1990) within the limits of both observational and Monte Carlo statistical errors. Kovaltsov et al (1993), on the basis of the data analysis, suggested a new approximate empirical expression which can be used for a wide range of the solar zenith angles :…”

Section: The Dependence Of the Response Of Nm To Solar Neutrons On Obmentioning

confidence: 99%

“…A comparison of the calculated response of an NM with the actual response allows one to obtain possible values of the parameters of an a priori assumption model of the neutron injection. For instance, such an approach has been used by Chupp et al (1987) for the analysis of the 3 June 1982 SNE as well as by Debrunner et al (1993) and Kocharov et al (1994) for the analysis of the 24 May 1990 SNE. However, this approach can be applied only for strong neutron events for which the time-profile of the NM response can be obtained.…”

Section: Deduction Of the Number Of Solar Neutrons From Nm Responsementioning

confidence: 99%

“…Today, about ten reliably detected solar-neutron events (SNEs) are known. Two of the events were observed by several NMs during the solar flares of 3 June 1982 (Debrunner et al, 1983;Efimov et al, 1983;Iucci et al, 1984) and 24 May 1990 (Shea et al, 1991;Debrunner et al, 1993;Kovaltsov et al, 1993).…”

Section: Introductionmentioning

confidence: 99%

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The World Neutron Monitor Network as a tool for the study of solar neutrons

et al. 1997

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Abstract. The use of the World Neutron Monitor Network to detect high-energy solar neutrons is discussed in detail. It is shown that the existing network can be used for the routine detection of intense sporadic solar-neutron events whenever they occur. A technique is suggested involving the weighted summation of responses of separate monitors to solar neutrons. It is demonstrated that the use of this method improves the significance of solar-neutron event detection. Different results of the simulation of the neutron-monitor sensitivity to solar neutrons have been tested with respect to their application for practical use. It is shown that the total number of neutrons with energy above 300 MeV injected from the Sun during a solar flare can be estimated directly from the time-integrated neutronmonitor response to solar neutrons without any model assumptions. The estimation technique has been developed.

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Neutron monitor yield function for solar neutrons: A new computation

et al. 2016

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A new yield function of a standard neutron monitor 6NM64 for solar neutrons is presented and tabulated in the attached lookup tables. It corresponds to a wide range of altitudes of the neutron monitor locations and angles of incidence for neutrons entering the Earth's atmosphere. The computations were made by Monte Carlo using the GEANT4‐based PLANETOCOSMICS tool. The yield function was validated against the measured data for solar neutron events of 3 June 1982 and 24 May 1990, and good agreement was found within a wide range of the altitudes of the neutron monitor location and angles of incidence of solar neutron arrival. The sensitivity of the world neutron monitor network for registration of solar neutron events was reassessed. The neutron monitor network is shown to be, in addition to other methods, a sensitive tool for monitoring of high‐energy solar‐flare neutrons with ≈95% probability to detect statistically significantly (>5σ) a solar neutron event similar to that of 3 June 1982.

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Solar neutron and proton production during the 1990 May 24 cosmic-ray flare increases

Cited by 52 publications

References 0 publications

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

The World Neutron Monitor Network as a tool for the study of solar neutrons

Neutron monitor yield function for solar neutrons: A new computation

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