The space telescope NINA: results of a beam test calibration

Bidoli, V.; Casolino, M.; Pascale, M. P. De; Morselli, A.; Furano, Gianluca; Picozza, P.; Scoscini, A.; Sparvoli, R.; Barbiellini, G.; Bonvicini, W.; Cirami, R.; Schiavon, P.; Vacchi, A.; Zampa, N.; Ambriola, M.; Bellotti, R.; Cafagna, F.; Ciacio, F.; Castellano, M.; Circella, M.; Marzo, C. De; Bartalucci, S.; Giuntoli, S.; Ricci, M.; Papini, P.; Piccardi, S.; Спиллантини, П.; Bakaldin, A.; Batishev, A.; Galper, A. M.; Koldashov, S. V.; Korotkov, M.; Mikhailov, V. V.; Murashov, A.; Voronov, S. A.; Boezio, M.

doi:10.1016/s0168-9002(98)01196-6

Cited by 18 publications

(11 citation statements)

References 11 publications

(4 reference statements)

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“…In method 1 the charge Z is estimated by means of the product E 1 × E tot , and the mass is evaluated by applying the following formula:

where Δ E is the energy lost by the particle in a thickness Δ x measured starting from the first plane. A precise evaluation of parameters a and b for each atomic species has been obtained both from real and simulated data [ Bidoli et al , 1999].…”

Section: Data Analysis and Observationsmentioning

confidence: 99%

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Geomagnetically trapped light isotopes observed with the detector NINA

et al. 2002

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[1] The detector New Instrument for Nuclear Analysis (NINA) aboard the satellite Resurs-01-N4 detected hydrogen and helium isotopes geomagnetically trapped, while crossing the South Atlantic Anomaly. Deuterium and tritium at L shell < 1.2 were unambiguously recognized. The 3 He and 4 He power law spectra, reconstructed at L shell = 1.2 and B < 0.22 G, have indices equal to 2.30 ± 0.08 in the energy range 12-50 MeV nucleon À1 and 3.4 ± 0.2 in 10-30 MeV nucleon À1 , respectively. The measured 3 He/ 4 He ratio and the reconstructed deuterium profile as a function of L shell bring one to the conclusion that the main source of radiation belt light isotopes at Resurs altitudes ($800 km) and for energy greater than 10 MeV nucleon À1 is the interaction of trapped protons with residual atmospheric helium.

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“…In method 1 the charge Z is estimated by means of the product E 1 × E tot , and the mass is evaluated by applying the following formula:

Section: Data Analysis and Observationsmentioning

confidence: 99%

“…where ÁE is the energy lost by the particle in a thickness Áx measured starting from the first plane. A precise evaluation of parameters a and b for each atomic species has been obtained both from real and simulated data [Bidoli et al, 1999].…”

Section: Data Analysis and Observationsmentioning

confidence: 99%

Geomagnetically trapped light isotopes observed with the detector NINA

et al. 2002

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“…The energy resolution is better than 1 MeV. A detailed description of the instrument and its performance with beam facilities and in orbit are reported in the works by Bakaldin et al (1997); Bidoli et al (1999Bidoli et al ( , 2001). …”

Section: The Silicon Detectormentioning

confidence: 99%

<i>Letter to the Editor</i> Energy spectrum of secondary protons above the atmosphere measured by the instruments NINA and NINA-2

Bidoli¹,

Casolino²,

Pascale³

et al. 2002

Ann. Geophys.

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Abstract. In this paper we report on the energy spectrum of protons of albedo origin measured by the instruments NINA and NINA-2 at different geomagnetic locations, and the behaviour of the proton flux as a function of altitude out of the South Atlantic Anomaly. The instrument NINA was used on board the satellite Resurs-01-N4 between 1998 and 1999, at an altitude of about 830 km. The NINA-2 apparatus, on board the satellite MITA, was put into orbit in July 2000, at an altitude of about 450 km. A detailed understanding of the fluxes of charged particles in near Earth orbit is important to reach an accurate theoretical description of the Earth's magnetic field, but also as input for the calculation of the background for scientific instruments aboard satellites, like the future AGILE and GLAST γ astronomy telescopes.

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“…Further details about the instrument and its performance during a test-beam session can be found in (Bakaldin et al 1997;Bidoli et al 1999).…”

Section: The Nina Instrumentmentioning

confidence: 99%

“…In order to optimize these values we utilized samples of different types of particles, obtained from a beam test session at GSI in 1997 (Bidoli et al 1999), as well as flight data.…”

Section: The Track Selection Algorithmmentioning

confidence: 99%

In‐Orbit Performance of the Space Telescope NINA and Galactic Cosmic‐Ray Flux Measurements

Bidoli

Canestro

Casolino

et al. 2001

ASTROPHYS J SUPPL S

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The NINA apparatus, on board the Russian satellite Resurs-01 n.4, has been in polar orbit since 1998 July 10, at an altitude of 840 km.Its main scientific task is to study the galactic, solar and anomalous components of cosmic rays in the energy interval 10-200 MeV n −1 .In this paper we present a description of the instrument and its basic operating modes. Measurements of Galactic Cosmic Ray spectra will also be shown.

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The space telescope NINA: results of a beam test calibration

Cited by 18 publications

References 11 publications

Geomagnetically trapped light isotopes observed with the detector NINA

Geomagnetically trapped light isotopes observed with the detector NINA

<i>Letter to the Editor</i> Energy spectrum of secondary protons above the atmosphere measured by the instruments NINA and NINA-2

In‐Orbit Performance of the Space Telescope NINA and Galactic Cosmic‐Ray Flux Measurements

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The space telescope NINA: results of a beam test calibration

Cited by 18 publications

References 11 publications

Geomagnetically trapped light isotopes observed with the detector NINA

Geomagnetically trapped light isotopes observed with the detector NINA

&lt;i&gt;Letter to the Editor&lt;/i&gt; Energy spectrum of secondary protons above the atmosphere measured by the instruments NINA and NINA-2

In‐Orbit Performance of the Space Telescope NINA and Galactic Cosmic‐Ray Flux Measurements

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<i>Letter to the Editor</i> Energy spectrum of secondary protons above the atmosphere measured by the instruments NINA and NINA-2