Radiation studies in space with nuclear emulsion detectors

Yagoda, Herman

doi:10.1007/bf00240579

Cited by 14 publications

(3 citation statements)

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“…The utility of these exposures for detailed trapped radiation measurements was first realized when emulsions recovered around August 1, 1962, showed over-all blackening due to the artificial electron belts created by the Starfish high-altitude thermonuclear explosion (crude measurements have been reported [Filz and Yagoda, 1961;Yagoda, 1962]). This blackening was not uniformly distributed, however, and varied from emulsion to emulsion and with sition on the ballast plate as well as position to position on a single emulsion sheet.…”

Section: Introductionmentioning

confidence: 99%

Time and altitude dependence of 55-Mev trapped protons, August 1961 to June 1964

Filz¹,

Holeman²

1965

J. Geophys. Res.

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Measurements of 55‐Mev omnidirectional trapped protons detected in a small region of the South Atlantic by nuclear emulsions flown on recoverable oriented Air Force satellites are reported for the period August 1961 to June 1964 between altitudes of 221 and 736 km. During the period August 1961 to June 1962, the data best fit a flux versus altitude curve J = 4.99 × 10−11 H4.792 protons/m2 sec Mev and is in good agreement with the variation of atmospheric density at these altitudes. H is the altitude over the South Atlantic measured in kilometers, and the time is the total time in orbit. No consistent slow increase of flux with time was observed as would be expected as the result of changes in atmospheric density. A sudden increase in flux was observed after the July 9, 1962, high‐altitude nuclear explosion Starfish, which is explained as consistent with a nonadiabatic redistribution of inner‐zone protons with an approximate 3.5° pitch angle change for L = 1.4 at the equator. The proton flux decays as expected on the basis of atmospheric ionization losses only, over a 2‐year period. The values of the trapped proton average atmospheric density that fit the decay are 3×107, 7×106, 2×106, and 1×106 atomic electrons per cm3 for altitudes of 275, 350, 440, and 500 km.

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Section: Introductionmentioning

confidence: 99%

Time and altitude dependence of 55-Mev trapped protons, August 1961 to June 1964

Filz¹,

Holeman²

1965

J. Geophys. Res.

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“…3), a spallation event see e.g. Kowalczyk (2008) and Krasa (2010) and pictures of what was called "star" from the former appearance in photographic plates (Levi Setti and Tomasini 1952) may indeed result in a photographic emulsion, see Yagoda (1962). This is exactly what was noticed during an examination of a movie made from routinely processed C3/LASCO coronagraph observations of the SoHO mission, at 11:30 UTC of 29 Nov. 2015, a time of very low solar activity on the Sun.…”

Section: Observationsmentioning

confidence: 99%

“…The CCD imaging instruments of the SoHO mission (Domingo et al 1995) of ESA and NASA, including the Large Angle and Spectrometric Coronagraphs (LASCO) and the Extreme ultraviolet Imaging Telescope (EIT) imagers, are sensitive to Solar Energetic Particles (SEP) in the MeV up to GeV range. Yagoda (1962), Obayashi (1964) and Roederer (1964) reported that a myriad of impacts is continually recorded at the time of big flares and CMEs. Higher energy particles in the GeV and in the more energetic range up to 10 21 eV are today called cosmic rays (CR), e.g., see Freier et al (1948); Chandrasekhar and Fermi (1953); Fermi (1954); Gaisser (1990) and Dorman (2006), they are primarily made of protons.…”

Section: Introductionmentioning

confidence: 99%

Observation of galactic cosmic ray spallation events from the SoHO mission 20-yr operation of LASCO

Koutchmy

Tavabi

Urtado

2018

Monthly Notices of the Royal Astronomical Society

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A shower of secondary Cosmic Ray (CR) particles is produced at high altitudes in the Earth's atmosphere, so the primordial Galactic Cosmic Rays (GCRs) are never directly measured outside the Earth magnetosphere and atmosphere. They approach the Earth and other planets in the complex pattern of rigidity's dependence, generally excluded by the magnetosphere. GCRs revealed by images of single nuclear reactions also called spallation events are described here. Such an event was seen on Nov. 29, 2015 using a unique LASCO C3 space coronagraph routine image taken during the Solar and Heliospheric Observatory (SoHO) mission observing uninterruptedly at the Lagrangian L1 point. The spallation signature of a GCR identified well outside the Earth's magnetosphere is obtained for the 1 st time. The resulting image includes different diverging linear "tracks" of varying intensity, leading to a single pixel; this frame identifies the site on the silicon CCD chip of the coronagraph camera. There was no solar flare reported at that time, nor Coronal Mass Ejection (CME) and no evidence of optical debris around the spacecraft. More examples of smaller CR events have been discovered through the 20 years of continuous observations from SoHO. This is the first spallation event from a CR, recorded outside the Earth's magnetosphere. We evaluate the probable energy of these events suggesting a plausible galactic source.

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