A ?source surface theory? corollary: The mean solar field-interplanetary field correlation

Schatten, Kenneth H.

doi:10.1007/bf00151854

Cited by 10 publications

(2 citation statements)

References 9 publications

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“…It has been proposed (Wilcox, Sever^iy, and Co?.burn, 1969) that the interplanetary field is not generate^9 by the magnetic !M elds associated with solar • active rc^ions, bur rather by the large scale magnetic f^_eld of the sun. Schatten (1970) has shown qua.^^titatively that these observations are in agreement ^vith, the potential field models of Altschuler anu Newkirk (1969) and Schatten,Wilcox and Ness (19F9) Sakurai (1966a, 1966b) in considering the relationships between solar active longitudes and the polarity distribution of the interplanetary magnetic fields, found that the roots of the sector• boundaries are located just east of the associated active longitudes. Furthermore, it was shown ti^at these active longitudes, from which the sunspot groups effective for the production of solar proton flares are generated, persist for long periods of time, of the order ' of a few years .…”

supporting

confidence: 63%

Active solar radio regions at metric frequencies and the interplanetary sector structures

Sakurai

Stone

1971

Sol Phys

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supporting

confidence: 63%

Active solar radio regions at metric frequencies and the interplanetary sector structures

Sakurai

Stone

1971

Sol Phys

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“…While the Sun's MMF is often taken to be an indirect measure of the IMF, being essentially proportional to B (Severny et al 1970;Schatten 1970), the similarity between equations (1) and…”

Section: Measurements Of the Solar Wind In The Ecliptic Planementioning

confidence: 99%

A Floor in the Solar Wind Magnetic Field

Svalgaard¹,

Cliver

2007

ApJ

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Long-term (∼130 years) reconstruction of the interplanetary magnetic field (IMF) based on geomagnetic indices indicates that the solar wind magnetic field strength has a "floor," a baseline value in annual averages that it approaches at each 11 yr solar minimum. In the ecliptic plane at 1 AU, the IMF floor is ∼4.6 nT, a value substantiated by direct solar wind measurements and cosmogenic nuclei data. At high heliolatitudes, Ulysses measured a constant radial field with a magnitude (normalized to 1 AU) of ∼3.2 nT during solar minimum conditions in ∼1995 when the observed solar polar fields were ∼100 mT and in 2006 when the polar fields were ∼60 mT, as well as for solar maximum conditions in 2001 when the polar fields were close to zero. We identify the floor with a constant (over centuries) baseline open magnetic flux at 1 AU of ∼ Wb, corresponding 14 4 # 10 to a constant strength (∼10 11 A) of the heliospheric current. Solar cycle variations of the IMF strength ride on top of the floor. The floor has implications for (1) the solar wind during grand minima-we are given a glimpse of Maunder minimum conditions at every 11 yr minimum; (2) current models of the solar wind-both source surface and MHD models are based on the assumption, invalidated by Ulysses, that the largest scale fields determine the magnitude of the IMF; consequently, these models are unable to reproduce the high-latitude observations; and (3) the use of geomagnetic input data for precursor-type predictions of the coming sunspot maximum-this common practice is rendered doubtful by the observed disconnect between solar polar field strength and heliospheric field strength.

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Stellar Winds and Spindown in Solar Type Stars

Roxburgh¹

1983

Solar and Stellar Magnetic Fields: Origins and Coronal Effects

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A ?source surface theory? corollary: The mean solar field-interplanetary field correlation

Cited by 10 publications

References 9 publications

Active solar radio regions at metric frequencies and the interplanetary sector structures

Active solar radio regions at metric frequencies and the interplanetary sector structures

A Floor in the Solar Wind Magnetic Field

Stellar Winds and Spindown in Solar Type Stars

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