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Balogh, A.; Smith, Edward J.

doi:10.1023/a:1011854901760

Cited by 25 publications

(10 citation statements)

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“…A small warp in the HCS would have been sufficient to produce the observations described while most of the sheet had actually tipped past the south pole, although it is almost certain that the HCS inclination was near its maximum. Balogh et al, [30] explained by, the two-sector structure observed during this period was consistent with a single HCS tilted at high inclination. An initial overview of the HMF polarity at Ulysses around solar maximum was presented by [31] and this period is represented in the Figure 3.…”

Section: The Polarity Reversal In Ulysses Second Orbitsupporting

confidence: 74%

Fluctuations of Solar Wind Parameters During Polar Reversal

Sobia¹

2015

AJAA

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Abstract:Around the time of polarity reversal in 2000 -2001, the solar wind plasma parameters and interplanetary magnetic field fluctuations are studied for an interval of time that corresponds to Ulysses in-situ measurements of high-latitude heliospheric magnetic field. This study has been done by investigating solar wind speed, density, temperature and solar magnetic field using Ulysses magnetometer and SWOOPS instrument. The sun's magnetic field reverses polarity approximately in every 11 year and it creates a peak in each solar cycle. This study gives a brief understanding of solar wind parameters in the heliosphere during polar reversal in solar cycle 23. The solar magnetic field completely reorganizes during the polar reversal phase, hence the distribution of solar wind parameters changes accordingly. By studying the variation of solar wind parameters, it is possible to understand the polar reversal phenomenon. The photospheric polarity reversal is completed in more active Northern Hemisphere in late 2000 and then in the Southern Hemisphere in 2001. The reversal of the magnetic field at the solar wind source surface is inferred to have occurred between late 2000 and 2001, with the most likely time of reversal being early within that period.

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Section: The Polarity Reversal In Ulysses Second Orbitsupporting

confidence: 74%

Fluctuations of Solar Wind Parameters During Polar Reversal

Sobia¹

2015

AJAA

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“…As a result, no ''pure'' fast solar wind, as we have defined in this paper, can be observed. The heliospheric medium is dominated by a mix of CMEs and short-lived interaction regions [Balogh and Smith, 2001;Gosling et al, 2001]. Despite the presence of the occasional high-speed stream, we expect that the turbulence properties of the solar wind may be close to those we have derived for the slow streams and ''pure'' slow wind.…”

Section: Solar Activitymentioning

confidence: 60%

Turbulence and intermittency in the heliospheric magnetic field in fast and slow solar wind

et al. 2009

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We study the nonuniform solar wind turbulence using high‐resolution Ulysses magnetic field data measured at different solar activity level, heliospheric latitudes, and distance. We define several types of solar wind dependent of the coronal region of origin and also of the dynamical behavior of the different streams, namely, “pure” fast wind, fast streams, “pure” slow wind, and slow streams. The turbulent properties of the solar wind types were investigated in terms of their scaling properties and spatial inhomogeneity. A clear trend in the power spectrum of the solar wind magnetic field magnitude is observed: the “pure” fast wind has a slope ∼−1.33 (1/f‐like), the fast streams ∼−1.48 (Kraichnan‐like), the “pure” slow wind ∼−1.67 (Kolmogorov‐like), and the slow streams ∼−1.72. We find that the “pure” fast wind in the polar heliolatitudes is less intermittent than the other types: “pure” slow wind and both slow and fast streams, which is because of the absence of dynamical interactions between streams with different speeds. On the other hand, fast streams are more intermittent than the “pure” fast wind, and slow streams are less intermittent than the “pure” slow winds. A clear radial and latitudinal evolution of the intermittency is observed only for the “pure” fast wind, while in the equatorial plane, the fast streams, the “pure” slow wind, and the slow streams do not show evolution either in heliolatitude or in heliocentric distance.

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“…A single current sheet, separating two regions of opposite polarity, is observed throughout the solar cycle (Smith et al, 1995;Balogh and Smith, 2001;Jones and Balogh, 2003). At solar minimum, the current sheet resides at low heliographic latitudes.…”

Section: Introductionmentioning

confidence: 99%

Understanding the Behavior of the Heliospheric Magnetic Field and the Solar Wind During the Unusual Solar Minimum Between Cycles 23 and 24

Zhao

Fisk

2011

Sol Phys

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The properties of the heliospheric magnetic field and the solar wind were substantially different in the unusual solar minimum between Cycles 23 and 24: the magnetic-field strength was substantially reduced, as were the flow properties of the solar wind, such as the mass flux. Explanations for these changes are offered that do not require any substantial reconsideration of the general understandings of the behavior of the heliospheric magnetic field and the solar wind that were developed in the minimum of Cycle 22 -23. Solar-wind composition data are used to demonstrate that there are two distinct regions of solar wind: solar wind likely to originate from the stalk of the streamer belt (the highly elongated loops that underlie the heliospheric current sheet), and solar wind from outside this region. The region outside the streamer-stalk region is noticeably larger in the minimum of Cycle 23 -24; however, the increased area can account for the reduction in the heliospheric magnetic-field strength in this minimum. Thus, the total magnetic flux contained in this region is the same in the two minima. Various correlations among the solar-wind mass flux and coronal electron temperature inferred from solar-wind charge states were developed for the Cycle 22 -23 solar minimum. The data for the minimum of Cycle 23 -24 suggest that the correlations still hold, and thus the basic acceleration mechanism is unchanged in this minimum.

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Cited by 25 publications

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Fluctuations of Solar Wind Parameters During Polar Reversal

Fluctuations of Solar Wind Parameters During Polar Reversal

Turbulence and intermittency in the heliospheric magnetic field in fast and slow solar wind

Understanding the Behavior of the Heliospheric Magnetic Field and the Solar Wind During the Unusual Solar Minimum Between Cycles 23 and 24

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