Neutron Monitor Response Functions

By J. Clem, L. Dorman. 2000

286 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9dd5908decc184cce85538090c32d6dfd145ea3c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. I. Usoskin
2. G. Kovaltsov
3. S. Solanki
4. Galina Bazilevskaya
5. K. Mursula
6. M. Schüssler
7. N. Krivova
8. Katja Alanko-Huotari

In Nuclear and High Energy Physics

1. I. Usoskin
2. G. Kovaltsov
3. Galina Bazilevskaya
4. J. Clem
5. S. Solanki
6. F. Joos
7. R. Roth
8. Eugene V. Rozanov

Citations in the corpus

• A physical reconstruction of cosmic ray intensity since 1610 (2002, background): “…P; xð Þ dP; ð7Þ where x and Pc are the atmospheric depth and the geomagnetic rigidity cutoff of the NM location, and Y(P, x) is the specific yield function which accounts for the propagation of GCR particles in the Earth’s atmosphere and the detection of secondary nucleons [Clem and Dorman, 2000].”
• A History of Solar Activity over Millennia (2008, background): “Panel A): Yield functions of the globally averaged and polar Be production (Webber and Higbie, 2003), global C production (Castagnoli and Lal, 1980), polar neutron monitor (Clem and Dorman, 2000) as well as the energy spectrum of galactic cosmic protons for medium modulation (φ = 550 MV).”
• A History of Solar Activity over Millennia (2008, unknown): “Panel A): Yield functions of the globally averaged and polar (10)Be production (Webber and Higbie, 2003), global (14)C production (Castagnoli and Lal, 1980), polar neutron monitor (Clem and Dorman, 2000) as well as the energy spectrum of galactic cosmic protons for medium modulation (φ = 550 MV).”
• RECORD-SETTING COSMIC-RAY INTENSITIES IN 2009 AND 2010 (2010, background): “In contrast, the response of sea-level, high-latitude neutron monitors (Clem & Dorman 2000) begins at ∼1 GV (∼433 MeV for protons) with a median response 10 GV (Ahluwalia & Fikani 2007).”
• Solar modulation parameter for cosmic rays since 1936 reconstructed from ground-based neutron monitors and ionization chambers (2011, methodology): “, 1982], CD00 [Clem and Dorman, 2000], and M09 [Matthiä, 2009; Matthiä et al.”
• Measurement of the flux and energy spectrum of cosmic-ray induced neutrons on the ground (2004, methodology): “Here we give the values for the parameters in (5), the scaling function for geomagnetic cutoff, determined by Belov, Struminsky, and Yanke (BSY) at solar minimum and maximum, and [35], [36], normalized so that their mean, , is 1 at NYC at standard sea-level pressure.”
• Heliospheric modulation of cosmic rays: Monthly reconstruction for 1951–2004 (2005, background): “[1982] and Clem and Dorman [2000], denoting the corresponding values by indices ‘‘DFL82’’ and ‘‘CD00.”
• Cosmic ray induced ionization in the atmosphere: Full modeling and practical applications (2006, background): “It detects mostly superthermal neutrons [Clem and Dorman, 2000], which correspond to the hadronic component of the atmospheric cascade, while the muon component dominates in the tropospheric CRII, especially at high energies (see Figure 1).”