2000
DOI: 10.1038/35044027
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Evolution of the Sun's large-scale magnetic field since the Maunder minimum

Abstract: The most striking feature of the Sun's magnetic field is its cyclic behaviour. The number of sunspots, which are dark regions of strong magnetic field on the Sun's surface, varies with a period of about 11 years. Superposed on this cycle are secular changes that occur on timescales of centuries and events like the Maunder minimum in the second half of the seventeenth century, when there were very few sunspots. A part of the Sun's magnetic field reaches out from the surface into interplanetary space, and it was… Show more

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Cited by 258 publications
(275 citation statements)
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“…The more detailed similarities between the two, however, imply that the open magnetic flux in some way quantifies both the spectrum of flux tube dimensions and the total flux of magnetic flux tubes threading the photosphere. Solanki et al (2000) obtained a good match to both the open flux variation derived by Lockwood et al (1999a) and to the cosmic ray flux variation inferred from the 10 Be cosmogenic isotope (Beer et al 2000;Lockwood 2001;McCracken & McDonald 2001) using a simple model of open flux emergence in active regions and its subsequent decay. Recently, Solanki et al (2001) have extended this modelling to include flux emergence in ephemeral regions and to estimate the total photospheric flux.…”
Section: Discussionmentioning
confidence: 75%
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“…The more detailed similarities between the two, however, imply that the open magnetic flux in some way quantifies both the spectrum of flux tube dimensions and the total flux of magnetic flux tubes threading the photosphere. Solanki et al (2000) obtained a good match to both the open flux variation derived by Lockwood et al (1999a) and to the cosmic ray flux variation inferred from the 10 Be cosmogenic isotope (Beer et al 2000;Lockwood 2001;McCracken & McDonald 2001) using a simple model of open flux emergence in active regions and its subsequent decay. Recently, Solanki et al (2001) have extended this modelling to include flux emergence in ephemeral regions and to estimate the total photospheric flux.…”
Section: Discussionmentioning
confidence: 75%
“…The correlation is expected to be poorer on shorter scales because individual photospheric magnetic features, such as for example a sunspot group, can grow and fade on timescales equivalent to, or shorter than, the 1-month averaging intervals used here and so produce rapid variations in I TS . On the other hand, open flux variations change on longer time scales associated with open flux emergence and decay (Solanki et al 2000). Significant anticorrelations are found with cosmic rays for the full range of geomagnetic rigidity cut-offs (2.4-13 GV).…”
Section: Discussionmentioning
confidence: 81%
“…It must always be remembered that sunspot numbers have applications only because they are an approximate proxy indicator of the total magnetic flux threading the photosphere and hence can be used to estimate and reconstruct terrestrial influences such as the received shortwave Total Solar Irradiance (TSI) and UV irradiance (Krivova, Balmaceda, and Solanki, 2007;Krivova et al, 2009, respectively), the open solar magnetic flux (Solanki, Schüssler, and Fligge, 2000;Lockwood and Owens, 2014a), and hence also the near-Earth solar-wind speed (Lockwood and Owens, 2014b), mass flux (Webb and Howard, 1994), and interplanetary magnetic-field strength (Lockwood and Owens, 2014a). Sunspot numbers also provide an indication of the occurrence frequency of transient events, in particular coronal mass ejections (Webb and Howard, 1994;Owens and Lockwood, 2012), and the phase of the decadal-scale sunspot cycle is used to quantify the tilt of the heliospheric current sheet (Altschuler and Newkirk, 1969;Owens and Lockwood, 2012) and hence the occurrence of fast solar-wind streams and co-rotating interaction regions (Smith and Wolf, 1976;Gazis, 1996).…”
Section: Definitions Of Sunspot Numbersmentioning
confidence: 99%
“…In brief, the OSF is modelled as a continuity equation (Solanki, Schüssler & Fligge 2000), with the source term, S, set by an empirical relation to SN using the data for the recent decades. The loss term, L, varies with the heliospheric current sheet inclination, which is assumed to be invariant between solar cycles (Asvestari & Usoskin 2016).…”
Section: The Magnetic Osfmentioning
confidence: 99%