Model of the magnetic field in the inner heliosphere with regard to radial field strength leveling in the solar corona

Veselovsky, I. S.; Lukashenko, A. T.

doi:10.1134/s003809461201008x

Cited by 2 publications

(3 citation statements)

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“…The latitudinal IMF dependence as well as effects discussed in [11,12,20] contribute to the "flux excess" effect. Discarding of the B r and B increase in low heliolatitudes inevitably reduces a quality of even very competent models (such as [29] and [30]), as they are based on slightly simplified views on the large-scale IMF picture in the inner heliosphere, assuming a constant B r at any distance with a sharp [29] or more gradual [30] change of the B r sign at the ecliptic plane.…”

Section: The «Magnetic Flux Excess» (F S ) Is Mainly a Consequence Ofmentioning

confidence: 99%

“…Discarding of the B r and B increase in low heliolatitudes inevitably reduces a quality of even very competent models (such as [29] and [30]), as they are based on slightly simplified views on the large-scale IMF picture in the inner heliosphere, assuming a constant B r at any distance with a sharp [29] or more gradual [30] change of the B r sign at the ecliptic plane. This means that in solar activity maximum both B r and the B r internal scatter increase.…”

Section: The Radial Imf Component Depends On Heliolatitudementioning

confidence: 99%

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The interplanetary magnetic field: Radial and latitudinal dependences

Khabarova

2013

Astron. Rep.

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Results of the analysis of spacecraft measurements at 1-5.4 AU are presented within the scope of the large-scale interplanetary magnetic field (IMF) structure investigation. The work is focused on revealing of the radial IMF component (B r ) variations with heliocentric distance and latitude as seen by Ulysses. It was found out that |B r | decreases as ~r −5/3 in the ecliptic plane vicinity (±10° of latitude). This is consistent with the previous results obtained on the basis of five spacecraft in-ecliptic measurements (Khabarova, Obridko, 2012). The difference between the experimentally found (r −5/3 ) and commonly used (r −2 ) radial dependence of B r may lead to mistakes in the IMF recalculations from point to point in the heliosphere. This can be one of the main sources of the "magnetic flux excess" effect, which is exceeding of the distantly measured magnetic flux over the values obtained through the measurements at the Earth orbit. It is shown that the radial IMF component can be considered as independent of heliolatitude in a rough approximation only. More detailed analysis demonstrates an expressed |B r | (as well as the IMF strength) increase in the latitudinal vicinity of ±30° relative to the ecliptic plane. Also, a slight increase of the both parameters is observed in the polar solar wind. The comparison of the B r distributions confirms that, at the same radial distance, B r values are higher in low latitudes than in high ones. The analysis of the latitudinal and radial dependences of the B r distribution's bimodality is performed. The B r bimodality is more expressed in high latitudes than in the low-latitude solar wind, and it is observed farther in high latitudes. The investigation has not revealed any dependence between B r and the solar wind speed V. Meanwhile, the two-peak distribution of the solar wind speed as measured by Ulysses is a consequence of a strong latitudinal and solar cycle dependence of V. It is shown that the solar wind speed in high latitudes (above ±40°) anti-correlates with a solar activity: V is maximal during the solar cycle minima, and it has a minimum at the maximum of solar activity. PACS: 96.50.Bh, 95.85.Sz, 96.60.Vg

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Section: The «Magnetic Flux Excess» (F S ) Is Mainly a Consequence Ofmentioning

confidence: 99%

Section: The Radial Imf Component Depends On Heliolatitudementioning

confidence: 99%

The interplanetary magnetic field: Radial and latitudinal dependences

Khabarova

2013

Astron. Rep.

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“…where only the first harmonic |k| = 1 is taken into account, and δ 1 , δ 2 , δ 3 are the amplitude multipliers of, correspondingly, dipole, quadrupole and octupole components, ψ 1 , ψ 2 , ψ 3 are phase shifts. Our approach is the development of an earlier attempt (Veselovsky and Lukashenko, 2012), made in the framework of a potential model, to describe the magnetic field of the Sun's corona and inner helio-magnetic field in the form of a sum of only dipole and quadrupole fields on the base of Ulysses data.…”

Section: Asymmetry Of Solar Magnetic Field According To Ulysses Datamentioning

confidence: 99%

Migrating Dynamo Waves and Consequences for Stellar Current Sheets

et al. 2022

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We study the relation between stellar dynamo-wave propagation and the structure of the stellar magnetic field. Modeling dynamo waves by the well-known Parker migratory dynamo, we vary the intensity of dynamo drivers in order to obtain activity-wave propagation toward the Equator (as in the solar-activity cycle) or towards the Poles. We match the magnetic field in the dynamo active shell with that in the surrounding stellar material, using a simple dissipativ magnetohydrodynamic system for the transition region. Introducing E. Yushkov

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Model of the magnetic field in the inner heliosphere with regard to radial field strength leveling in the solar corona

Cited by 2 publications

References 1 publication

The interplanetary magnetic field: Radial and latitudinal dependences

The interplanetary magnetic field: Radial and latitudinal dependences

Migrating Dynamo Waves and Consequences for Stellar Current Sheets

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