Dynamics of the Interplanetary Gas and Magnetic Fields.

Parker, E. N.

doi:10.1086/146579

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“…Parker (1958), who proposed the existence of the solar wind, already noted that this wind would cause a retardation of solar rotation on a long time scale. It was soon recognised that this phenomenon also applied to other stars and the associated angular momentum loss was linked to the existence of a surface convection zone (Schatzman 1962).…”

Section: Discussionmentioning

confidence: 99%

X-ray emission regimes and rotation sequences in M 35

Gondoin

2013

A&A

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Context. Late-type stars in young open clusters show two kinds of dependence of their X-ray emission on rotation. They also tend to group into two main sub-populations that lie on narrow sequences in diagrams where their rotation periods are plotted against their (B − V) colour indices. A correlation between these two regimes of X-ray emission and the rotation sequences has been recently observed in the M 34 open cluster. Sun-like M 34 stars also show a drop of their X-ray to bolometric luminosity ratio by about one order of magnitude at a Rossby number of about 0.3. Aims. The present study looks for similar connections between X-ray activity and rotation in an other open cluster. The aim is to consolidate a model of X-ray activity evolution on the main sequence and to provide observational constraints on dynamo processes in the interiors of late-type stars. Methods. The paper compares XMM-Newton measurements of X-ray stellar emission in M 35 with X-ray luminosity distributions derived from rotation period measurements assuming either an X-ray regime transition at a critical Rossby number or a correlation between X-ray emission regimes and rotation sequences. Results. This second hypothesis could account for the low number of M 35 stars detected in X-rays. A model of X-ray activity evolution is proposed based on the correlation. One major output is that the transition from saturated to non-saturated X-ray emission occurs at Rossby numbers between about 0.13 and 0.4 for each star depending on its mass and initial period of rotation on the ZAMS. This prediction agrees with observations of stellar X-ray emission in M 34. It explains the large range of X-ray luminosities observed among Sun-like stars in young open clusters. Conclusions. I conclude that the correlation between X-ray emission regimes and rotation sequences could be a fundamental property of the early evolution of stellar magnetic activity on the main sequence. I argue that the angular momentum redistribution mechanism(s) responsible for the transition between rotation sequences could result in a changing mixture of dynamo processes occurring side by side, possibly including a turbulent dynamo at high rotation rate and an interface-type dynamo whose efficiency decreases progressively at later stage of stellar evolution when rotation dies away.

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Section: Discussionmentioning

confidence: 99%

X-ray emission regimes and rotation sequences in M 35

Gondoin

2013

A&A

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“…The results can be compared with measured interplanetary fields extrapolated toward the sun or by extrapolation of the coronal field outward (Schatten, 1968;Stenflo, 1971) using the assumption of transport of the field by a radially flowing plasma. The radial gradients of the I field components used are those predicted by the spherically-symmetric model of Parker (1958). Thus a comparison of experimentally-determined IEF gradients with the Parker model predictions is of interest to such coronal field studies, as well as to the construction of solar wind models.…”

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“…The initial formulation' for the IMF in terms of a reference field B(E, 0o ) at a heliocentric radial distance r = b, latitude 6 and azimuth 00 was given (Parker, 1958) in the form…”

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Heliocentric distance dependence of the interplanetary magnetic field

Behannon

1978

Reviews of Geophysics

129

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“…In addition, the IMF has a prevailing global structure across the heliosphere which is controlled by the solar rotation. The combination of this rotation and the radially flowing solar wind gives an average distribution of the equatorial IMF in the shape of an Archimedean spiral, known as the Parker spiral [Parker, 1958]. Within this plane (see Figure 2.2), the Parker spiral makes an average angle of ~45° near Earth which becomes increasingly azimuthal to ~87° at…”

Section: Properties At 10 Aumentioning

confidence: 99%

The Near-Saturn Magnetic Field Environment

Sulaiman

2017

Springer Theses

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Shock waves exist throughout the universe and are fundamental to understanding the nature of collisionless plasmas. The complex coupling between charged particles and electromagnetic fields in plasmas give rise to a whole host of mechanisms for dissipation and heating across shock waves, particularly at high Mach numbers. While ongoing studies have investigated these process extensively both theoretically and via simulations, their observations remain few and far between. This thesis presents a study of very high Mach number shocks in a parameter space that has been poorly explored and identifies reformation using in situ magnetic field observations from the This non-axisymmetry is revealed to have an impact in the rotation of the magnetic field and is significant enough to influence the magnetic shear at the magnetopause.

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Dynamics of the Interplanetary Gas and Magnetic Fields.

Cited by 3,320 publications

References 0 publications

X-ray emission regimes and rotation sequences in M 35

X-ray emission regimes and rotation sequences in M 35

Heliocentric distance dependence of the interplanetary magnetic field

The Near-Saturn Magnetic Field Environment

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