Manual Fine Structure of Solar Radio Bursts: 375 (Astrophysics and Space Science Library)

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Contents:
  1. Imaging spectroscopy of solar radio burst fine structures | Nature Communications
  2. Fine Structure of Solar Radio Bursts - Gennady P. Chernov - Google книги
  3. MLSO Publications

If the address matches an existing account you will receive an email with instructions to retrieve your username. Open access. Space Weather Early View. Research Article Open Access. Sato Corresponding Author E-mail address: hiroatsu. Sato, E-mail address: hiroatsu. Tools Request permission Export citation Add to favorites Track citation. Share Give access Share full text access. Share full text access. Please review our Terms and Conditions of Use and check box below to share full-text version of article.

Figure 1 Open in figure viewer PowerPoint. The values at UT are set as the reference. Figure 2 Open in figure viewer PowerPoint. Solar radio observation on the 6 September The flat curves after UT correspond to the saturation levels of the solar radio frequencies. The dotted line indicates 2, solar flux unit SFU level for comparison with Ondrejov data.

Figure 3 Open in figure viewer PowerPoint. Figure 4 Open in figure viewer PowerPoint. Figure 5 Open in figure viewer PowerPoint. The Ondrejov solar radio intensity of corresponding frequencies is shown by green curve.

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Imaging spectroscopy of solar radio burst fine structures | Nature Communications

Figure 6 Open in figure viewer PowerPoint. Figure 7 Open in figure viewer PowerPoint. The deviation from the reference coordinates is computed for east, north, and height in meters. The PPP processing was started at 00 UT in order to achieve sufficient convergence before solar extreme ultraviolet and radio burst events. Berdermann, J. Google Scholar. Crossref Google Scholar. Figures References Related Information. Close Figure Viewer.


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Bakunin, L. Barta, M. Benz, A. Berney, M.

Fine Structure of Solar Radio Bursts - Gennady P. Chernov - Google книги

Bernold, T. Bespalov, P. Plasma Phys. Such structures would affect the migration of dust grains and could produce dust rings and gaps. MHD processes have received an increasing interest after realizing that for perfectly ionized Keplerian disks, arbitrarily weak magnetic fields could trigger a linear instability, the magneto-rotational instability MRI Balbus and Hawley , saturating in a turbulent state. In weakly ionized plasmas, this instability can be damped Jin ; Kunz and Balbus or modified in nature Balbus and Terquem ; Kunz The transport of magnetic field in weakly ionized disks can be described via a modified induction equation:.

Ohmic and ambipolar diffusions are indeed dissipative terms, respectively caused by collisions of electrons and ions. The Hall term is not a dissipative one: it describes the collisionless drift between electrons and ions and can only transport magnetic energy via whistler waves. Retaining only the ideal and Hall terms amounts to neglecting the ion dynamics, following the induction of magnetic field by electrons only.

In this limit, a linear instability remains that could sustain the turbulent transport of angular momentum in accretion disks Wardle Early simulations including the Hall term showed that the Hall-MRI would still saturate in a turbulent state Sano and Stone a,b , though with varying effective viscosities. However, the Hall term might largely dominate the ideal induction term in the midplane of protoplanetary disks Kunz and Balbus In this regime, the Hall-shear instability still operates in Keplerian disks, but with a different outcome Kunz and Lesur After a phase of linear growth, the instability breaks into a non-linear and disordered regime.

From this turbulent phase, high magnetic flux regions progressively merge together, ultimately separating contiguous regions of strong magnetic field from regions devoid of magnetic flux. This behavior can be understood as follows. The linear instability requires a magnetic field that is sufficiently weak, such that the shear rate of the flow is larger than the whistler waves frequency at a given scale.

Retaining only the Hall term, Eq. Projected on the direction normal to the disk, this equation implies that magnetic flux is transported away from stress maxima, and this opens a route to self-organization. In the limit of weak magnetic flux, the linear instability has accordingly small growth rates and does not generate a significant stress. In the limit of strong magnetic flux, whistler waves can propagate despite the strong shear, when the Keplerian flow becomes linearly stable.

For intermediate intensities of the magnetic flux, the instability generates a magnetic stress that effectively pushes magnetic flux away. If the magnetic flux locally increases, the flow can be stabilized, the magnetic stress becomes locally minimal, and therefore the stabilized region becomes a sink for magnetic flux. Eventually, these magnetic concentrations grow and spread in the azimuthal direction.

If something tries to spread the magnetic flux radially, this will decrease its intensity down to the point where the linear instability is triggered again; as a feedback, the instability generates magnetic stress, thus confining magnetic flux again. Given the total magnetic flux through the disk, the turbulent and ordered phases are two available outcomes for the flow. The Hall effect, when strong enough, allows a spontaneous transition from the turbulent phase to an ordered equilibrium featuring large-scale and long-lived structures. Its relevance to astrophysical disks is uncertain though.

The main caveat of these studies is the neglect of vertical stratification, i.

MLSO Publications

Results from numerical simulations Fig. Still, striped structures have been observed in stratified simulations of strongly magnetized disks Moll ; axisymmetric magnetic accumulations could be a generic feature of MHD turbulent disks Bai and Stone ; Ruge et al. At the moment, this behavior lacks a robust explanation.

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Critical Assessment: The argument of a self-organization process in the evolution of a protopoanetary disk is mostly made in terms of the spatially emerging order S , which starts from random-like turbulent flows with a complex fine structure and ends up in almost equidistantly ordered rings. Jupiter exhibits a stable Great Red Spot since years or possibly since years , which indicates a high-pressure zone of a persistent anticyclonic storm Fig.

Why can such an ordered, stable, long-lived structure exist in the randomly turbulent atmosphere of a gas giant? Why would it not decay into similar turbulent structures as observed in the surroundings? A geostrophic wind or current results from the balance between pressure gradients and Coriolis forces. One theoretical explanation that was put forward is the self-organization of vorticity in turbulence: The Jovian vortices reflect the behavior of quasi-geostrophic vortices embedded in an east-west wind with bands of uniform potential vorticity Marcus Numerical simulations based on the quasi-geostrophic equations for a Boussinesq fluid in a uniformly rotating and stably stratified environment indicated the self-organization of the flow into a large population of coherent vortices McWilliams et al.