A physical reconstruction of cosmic ray intensity since 1610
By I. Usoskin, K. Mursula, S. Solanki, M. Schüssler, G. Kovaltsov. 2002
140 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Molecular Biology
View Paper: https://www.semanticscholar.org/paper/b4eab984c4a40a8bb668bd04a8c723764313bb3e
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Citations in the corpus
- Cosmic ray induced ionization in the atmosphere: Full modeling and practical applications (2006, background): “Several possible mechanisms have been suggested, which can be responsible for the observed relation between the solar variability and the climate: via the changing solar irradiance [Fro¨hlich and Lean, 2004; Soon, 2005]; by the UV heating of the stratosphere and consequent changes in the circulation”
- Evolution of the solar irradiance during the Holocene (2011, methodology): “Using a standard theory of cosmic ray transport in the Heliosphere one can relate the modulation potentialΦ to the open magnetic flux assuming a constant 11-yr averaged solar wind speed (e.g. Usoskin et al. 2002).”
- A phenomenological study of the long-term cosmic ray modulation, 850-1958 AD (2004, methodology): “ Usoskin et al. [2002] recognized that the low values of the 10 Be concentration at the”
- The Maunder minimum (1645–1715) was indeed a grand minimum: A reassessment of multiple datasets (2015, background): “The OSF is the main driver of the heliospheric modulation of cosmic rays on timescales of decades to centuries (e.g., Usoskin et al. 2002), with additional variability defined by the heliospheric current sheet (HCS) tilt and the large scale polarity of the heliospheric magnetic field (Alanko-Huotari…”
- Grand minima and maxima of solar activity: new observational constraints (2007, background): “Most directly related to the 14C production in the atmosphere is the modulation potential φ (e.g., Castagnoli & Lal 1980, Masarik & Beer 1999, Usoskin et al. 2002) whose variations are shown in panel A.”
- A History of Solar Activity over Millennia (2008, unknown): “It has been shown, using a theoretical model of the heliospheric transport of cosmic rays (e.g., Usoskin et al., 2002b), that on the long-term scale (beyond the 11-year solar cycle) the modulation potential φ is closely related to the open solar magnetic flux Fo, which is a physical quantity…”
- Solar Irradiance Variability and Climate (2013, background): “Therefore Steinhilber, Beer & Fröhlich (2009) and Vieira et al. (2011) first employ physical models to calculate the solar open magnetic flux from Φ (see also Solanki et al. 2004, Usoskin et al. 2002, 2003a).”
- The New Sunspot Number: Assembling All Corrections (2015, background): “riginal GN series, this \Grand Maximum" concept rests primarily on an unusually high maximum in the mid-20th century found in time series of cosmogenic isotopes and attributed to a solar origin (Usoskin et al., 2002; Usoskin, 2013). We note however that all studies do not agree on this interpre”
- Solar modulation parameter for cosmic rays since 1936 reconstructed from ground-based neutron monitors and ionization chambers (2011, background): “…spectrum of CR. Count rate of such a detector is defined as an integral, above the threshold energy corresponding to the local geomagnetic rigidity cutoff, of a product of the CR energy spectrum and a specific yield function of the detector [see, e.g., Clem and Dorman, 2000; Usoskin et al., 2002b].”
- An Antarctic view of Beryllium-10 and solar activity for the past millennium (2011, background): “On the other hand, physical models are able to simulate various quantities related to the open magnetic flux: the modulation parameter, sunspot number, GCR, and cosmogenic isotope production (e.g., Usoskin et al. 2002).”