Spectrometre pour protons solaires et galactiques a bord du satellite iris

Amram, Y.; Axisa, F.; Engelmann, J.; Koch, L.; Schneider, Christian

doi:10.1016/0029-554x(69)90592-8

Cited by 3 publications

(3 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…With the 1.3 ns 10-in. PMT TTS [7] and the intrinsic ASIC time resolution (Table 1), the overall timing resolution is found to be 1.9 ns at 1 pe.…”

Section: Resultsmentioning

confidence: 95%

“…The time-over-threshold information from the ASIC can be used to determine the pulse's charge and time. The contribution of the reconstruction to the charge resolution (20%) is below the PMT intrinsic charge resolution for any application (40% [7]). The peak time is derived from the last crossed threshold allowing a constant 0.5 ns resolution for charges up to 50 pe.…”

Section: Resultsmentioning

confidence: 99%

“…An ANTARES optical module [7], housing a Hamamatsu R7081-20 10-in. PMT was placed in a black box and illuminated with a LED.…”

Section: Time and Charge Reconstruction And Determination Of The Thrementioning

confidence: 99%

See 2 more Smart Citations

SCOTT: A time and amplitude digitizer ASIC for PMT signal processing

Ferry

Guilloux

Anvar

et al. 2013

Nuclear Instruments and Methods in Physics Research Section A:

View full text Add to dashboard Cite

“…With the 1.3 ns 10-in. PMT TTS [7] and the intrinsic ASIC time resolution (Table 1), the overall timing resolution is found to be 1.9 ns at 1 pe.…”

Section: Resultsmentioning

confidence: 95%

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

SCOTT: A time and amplitude digitizer ASIC for PMT signal processing

Ferry

Guilloux

Anvar

et al. 2013

Nuclear Instruments and Methods in Physics Research Section A:

View full text Add to dashboard Cite

Penetration of solar protons over the polar cap during the February 25, 1969, event

Engelmann¹,

Hynds²,

Morfill³

et al. 1971

J. Geophys. Res.

Self Cite

View full text Add to dashboard Cite

During the February 25, 1969, solar proton event, particle measurements from the close‐orbiting satellite Esro 2, and particle and magnetic field measurements outside the magnetosphere from the Heos A1 satellite are available. The Esro 2 data for proton energies from E>27 to E>90 Mev show intensity enhancements in the auroral zone region and in the central polar region relative to the rest of the polar cap. At energies of a few million electron volts such enhancements are significantly less marked. By comparison of observations inside and outside the magnetosphere and by suitable trajectory computations inside the magnetosphere, we explain the auroral zone enhancements at energies >27 Mev in terms of a form of impact zone effect allied to a particle anisotropy outside the magnetosphere. We suggest that the enhancements observed over the polar region may be due to the particle anisotropy outside the magnetosphere plus coupling between the central polar cap lines of force and the interplanetary field lines.

show abstract

Differential energy spectrum of geomagnetically trapped protons with the Esro 2 satellite

Valot¹

1972

J. Geophys. Res.

View full text Add to dashboard Cite

The proton energy spectrum in the inner Van Allen zone was investigated in the range 30 to 300 Mev with a solid state dE/dx telescope aboard the Esro 2 satellite. The B‐L domain covered is 1.3 ≤ L ≤ 2.4 and 0.18 ≤ B ≤ 0.24. It was found that an exponential spectrum f [E] = N0 exp (—E/E0) is a good fit to the data in the range L = 2 to L = 2.4. For L < 2, a composite exponential spectrum is more suitable for describing the observed shape: Between 30 Mev and a ‘knee‐energy’ Ec, f[E] = N1 exp (—E/E1) and for E > Ec, f[E] = N0 exp (—E/E0). From our data, the variations with L of the parameters Ec, E0, E1 were found to be (a) E1 = (148 ± 8) Mev; (b) E0 = (290 ± 20) L−3.3±0.3; and (c) Ec = (400 ± 20) L−3±0.2. We suggest that two injection mechanisms are operating for all of this energy range, and that they give rise to two populations. The first one is the main component at energies lower than 25 Mev. At energies higher than our threshold (30 Mev), the detected fluxes are the addition of a second population (main component) and the high‐energy tail of the first population. The spectrum of this second population appears to have the characteristic shape of a spectrum altered by ionization losses and generated by a continuous source, the slope for energies greater than Ec being E0.

show abstract

Spectrometre pour protons solaires et galactiques a bord du satellite iris

Cited by 3 publications

References 0 publications

SCOTT: A time and amplitude digitizer ASIC for PMT signal processing

SCOTT: A time and amplitude digitizer ASIC for PMT signal processing

Penetration of solar protons over the polar cap during the February 25, 1969, event

Differential energy spectrum of geomagnetically trapped protons with the Esro 2 satellite

Contact Info

Product

Resources

About