Secular variation of the Sun's magnetic flux

By S. Solanki, M. Schüssler, M. Fligge. 2002

176 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/880cce44a1a3e1d6eb53eeb5de11001267cb183c

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In Astronomy and Astrophysics

Citations in the corpus

Solar radiative output and its variability: evidence and mechanisms (2004, methodology): “Emphemeral regions are, once again, postulated, as an additional source of open ux to explain why 10Be levels uctuated during the seventeenth century (Solanki et al., 2002b).”
Evolution of the large-scale magnetic field on the solar surface: a parameter study (2004, background): “This result is in agreement with the predictions of the simple model describing the long-term evolution of the Sun’s large-scale magnetic field by Solanki et al. (2000, 2002b) and with the simulations of Schrijver et al. (1997).”
Reconstruction of total and spectral solar irradiance from 1974 to 2013 based on KPVT, SoHO/MDI and SDO/HMI observations (2014, background): “…is presently the most precise version of the SATIRE model whose main assumption is that variations in solar irradiance on timescales of days and longer arise from photospheric magnetism alone (Foukal & Lean 1986; Fligge et al. 2000; Solanki et al. 2002; Preminger et al. 2002; Krivova et al. 2003).”
A phenomenological study of the long-term cosmic ray modulation, 850-1958 AD (2004, methodology): “[54] Solanki et al. [2000, 2002] have modeled the evolution of the Sun’s large-scale magnetic field since the Maunder minimum using sunspot numbers as a proxy for the flux emerging from large active regions and from small ephemeral regions.”
Reconstruction of solar total irradiance since 1700 from the surface magnetic flux (2007, methodology): “A set of three coupled ordinary differential equations has been shown to describe the evolution of the three flux components (Solanki et al. 2002): dφact dt = εact(t) − φact τact − φact τta , (1) dφeph dt = εeph(t) − φeph τeph − φeph τte , (2) dφopen dt = φact τta + φeph τte − φopen τopen ·…”
Modeling the Sun’s Magnetic Field and Irradiance since 1713 (2005, background): “Solanki et al. (2002) have presented a model for the evolution of the Sun’s total and open magnetic flux since 1700.”
SUPERFLARES ON SOLAR-TYPE STARS OBSERVED WITH KEPLER. I. STATISTICAL PROPERTIES OF SUPERFLARES (2013, background): “about 1024 Mx and 1023 Mx (e.g., Solanki et al. 2002; Vieira & Solanki 2010), the total magnetic flux in the most active Sun-like stars may be estimated to be 3 × 1024 ∼ 1025 Mx.”
A History of Solar Activity over Millennia (2008, unknown): “Modern physics-based models allows one to calculate the open solar magnetic flux from data of solar observation, in particular sunspots (Solanki et al., 2000, 2002; Krivova et al., 2007).”
The Maunder minimum (1645–1715) was indeed a grand minimum: A reassessment of multiple datasets (2015, methodology): “Finally, Vieira et al. (2011) adapted the models by Solanki et al. (2002) and Krivova et al. (2007) for use with 14 C data (red colour tones).”
A physical reconstruction of cosmic ray intensity since 1610 (2002, methodology): “[3] In this paper we suggest a physical model for longterm cosmic ray calculation which is a combination of the solar magnetic flux model [Solanki et al., 2000, 2002] and a spherically symmetric heliospheric model [Gervasi et al., 1999; Usoskin et al., 2002].”
Solar modulation parameter for cosmic rays since 1936 reconstructed from ground-based neutron monitors and ionization chambers (2011, result): “This is consistent with the lower solar open magnetic flux in earlier 20th century suggested by many studies [cf. Lockwood et al., 1999, 2009; Solanki et al., 2002; Usoskin et al., 2002a; McCracken, 2007; Vieira and Solanki, 2010].”