Rigidity dependence of cosmic ray proton latitudinal gradients measured by the Ulysses spacecraft: Implications for the diffusion tensor

By R. Burger, M. Potgieter, B. Heber. 2000

284 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/4ca32ee5b2d925c2ec36d2ec932094a46d6d8166

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Citations in the corpus

EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, methodology): “The LIS spectrum assumed by Burger et al. (2000) [B00], given in Equation (7), is typically used and is shown in Figure 5.”
Dynamics of the Earth’s Particle Radiation Environment (2009, methodology): “Equation (2) includes also the function JLIS, the exact shape of which is not known (Burger et al. 2000; Garcia-Munoz et al. 1975; Moskalenko et al. 2002; Webber and Higbie 2003).”
A History of Solar Activity over Millennia (2008, methodology): “Presently-used approximations for LIS (e.g., Garcia-Muñoz et al., 1975; Burger et al., 2000; Webber and Higbie, 2003) agree with each other for energies above 20 GeV but may contain uncertainties of up to a factor of 1.”
Long-Term Cosmic-Ray Modulation in the Heliosphere (2004, methodology): “…heliospheric polar regions and similar to what Jokipii & Kóta (1989) used; Dfak ¼ 10:0 in units of (rigidity) 2, which causes drifts to be somewhat reduced at lower rigidities, as explained by Burger et al. (2000); ðKAÞ0 ¼ 1:0, and is the ratio between the particle speed and the speed of light.”
Heliospheric modulation of cosmic rays: Monthly reconstruction for 1951–2004 (2005, methodology): “[30] While our method is based on the local interstellar spectrum by [Burger et al., 2000] (called BPH00; see also equation (2)), some other estimates of LIS can be found in literature.”
A physical reconstruction of cosmic ray intensity since 1610 (2002, unknown): “The model adopts the following local interstellar spectrum of GCR (i.e., outside the heliosphere) as a function of rigidity [Burger et al., 2000]: GLIS Pð Þ ¼ 1:9 104P 2:78; P 7GV GLIS Pð Þ ¼ exp 9:472 1:999 lnP 0:6938 lnPð Þ2þ0:2988 lnPð Þ3 0:04714 lnPð Þ4Þ; P < 7GV ð6Þ where P is expressed in GV,…”
Cosmic ray induced ionization in the atmosphere: Full modeling and practical applications (2006, methodology): “Here we use the LIS for protons according to [ Burger et al., 2000 ]”
Solar modulation parameter for cosmic rays since 1936 reconstructed from ground-based neutron monitors and ionization chambers (2011, methodology): “Here we use, following the procedure described in U05, the proton LIS in the form [Burger et al., 2000]: JLIS Tð Þ ¼ 1:9 10 4 P Tð Þ 2:78 1þ 0:4866P Tð Þ 2:51 ; ð2Þ where P(T) = ffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi T T þ 2Trð Þ p , J and T are expressed in units of…”
A History of Solar Activity over Millennia (2008, unknown): “The differential intensity Ji of the cosmic-ray nuclei of type i with kinetic energy T at 1 AU is given in this case as Ji(T, φ) = JLIS,i(T + Φi) (T )(T + 2Tr) (T + Φ)(T + Φi + 2Tr) , (3) where Φi = (Zie/Ai)φ for a cosmic nuclei of i-th type (charge and mass numbers are Zi and Ai), T and φ are expre”