Limitations of the force field equation to describe cosmic ray modulation

By R. Caballero-Lopez, H. Moraal. 2004

241 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/21f16bdff28873087e6420b28d730b3a9b9ac3ff

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. Paul Charbonneau
4. J. Beer
5. R. Muscheler
6. M. Vonmoos
7. N. Lifton
8. S. Solanki

In Atmospheric Science

1. I. Usoskin
2. G. Kovaltsov
3. R. Muscheler
4. Paul Charbonneau
5. M. Vonmoos
6. J. Beer
7. N. Lifton
8. Adam A. Scaife

Citations in the corpus

• A phenomenological study of the long-term cosmic ray modulation, 850-1958 AD (2004, methodology): “Nevertheless, Caballero-Lopez and Moraal [2004] have shown that the modulation in the outer heliosphere only makes a minor contribution to the modulation observed near Earth for E > 300 MeV/nucleon.”
• A History of Solar Activity over Millennia (2008, methodology): “Reconstruction of the HMF from Be data has been performed by Caballero-Lopez and Moraal (2004), using a model of CR modulation in the heliosphere and a Be production model by Webber and Higbie (2003).”
• Heliospheric modulation of cosmic rays: Monthly reconstruction for 1951–2004 (2005, methodology): “The modulation varies with the varying solar activity and is often described in terms of the so-called force field model [Gleeson and Axford, 1968; Caballero-Lopez and Moraal, 2004; McCracken et al., 2004a]. The only explicit parameter of this model is the modulation potential f whose value is given”
• Solar activity during the last 1000 yr inferred from radionuclide records (2007, methodology): “This method gives a good approximation for the cosmic ray spectrum in the inner heliosphere, which is the cosmic ray spectrum impinging on the Earth’s atmosphere (Caballero-Lopez and Moraal, 2004).”
• EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, background): “…cosmic ray fluxes will formally experience an energy dependent radial gradient in wind modulation efficiency that can vary by a factor of a few between distances of D = 1 AU to 80 AU (Caballero-Lopez & Moraal 2004; Langner & Potgieter 2005; Manuel et al. 2011; Manuel 2011), see also Section 5.2.”
• Scaling in situ cosmogenic nuclide production rates using analytical approximations to atmospheric cosmic-ray fluxes (2014, background): “Above that altitude, the LSD model flux tends to underestimate slightly the neutron monitor intensities measured by Sandström (1958), but it agrees well with the intensities measured by Carmichael et al. (1969a). The difference between the measurements of those studies (taken with different neutron ”
• Cosmic ray induced ionization in the atmosphere: Full modeling and practical applications (2006, background): “2.3. Cosmic Ray Spectrum [11] It is common for various applications to parameterize the differential energy spectrum of galactic cosmic rays at the Earth’s orbit by the so-called force field model [Gleeson and Axford, 1968; Caballero-Lopez and Moraal, 2004; McCracken et al., 2004a], where the spec”
• A History of Solar Activity over Millennia (2008, unknown): “However, it is only a formal spectral index whose physical interpretation is not straightforward, especially on short timescales and during active periods of the sun (Caballero-Lopez and Moraal, 2004).”
• Solar Forcing for CMIP6 (v3.1) (2016, methodology): “so-called force-field model (Caballero-Lopez and Moraal, 2004) parameterized via the time-variable modulation potential φ and the fixed shape of the local interstellar spectrum (see, e.”
• Large variations in Holocene solar activity: Constraints from 10Be in the Greenland Ice Core Project ice core (2006, methodology): “However, Figure 1 shows that the difference to our work [Cini Castagnoli and Lal, 1980; Masarik and Beer, 1999] is smaller than 10% in the energy range where the 10Be response to GCR is largest (gray bar in Figure 1) [McCracken, 2001, 2004; Webber and Higbie, 2003].”