Register Login Contact Us

Wanting A Horny Woman What does kinky mean in texting

Look Adult Chat

What does kinky mean in texting

Online: Now

About

The American Astronomical Society. All rights reserved. Printed in U. Linton1 G.

Name: Kary
Age: 20
City:
Hair: Blond naturally
Relation Type: Swinger Wife Search Single Dating Online
Seeking: I Ready For Dick
Relationship Status: Not important

Views: 5561

The American Astronomical Society. All rights reserved. Printed in U. Linton1 G.

Fisher1 R. Dahlburg2 and Y. Our goal is to determine whether the kink instability can explain the unusual morphology of certain " -spot" active regions.

The characteristics of these -spots are unusually large tilt upon emergence, hexting rotation, compactness during their lifetime, magnetic shear that develops along the neutral line of their vertical magnetic field, and unusually high flare activity. We find that highly twisted tubes perturbed with a single unstable kink mode evolve to a new helical equilibrium with finite amplitude.

This kink would produce an active region that emerged tilted and then rotated and so is suggestive of -spot behavior.

An exploratory study of a new kink activity: “pup play”

It would not, however, produce linky characteristics of -spots such as compactness and shear. We then investigate the kink instability in tubes perturbed simultaneously with several unstable modes at different wavelengths. These tubes develop a concentrated kink at the point at which the modes interact constructively. We show that such a concentrated kink would first emerge highly tilted, rotate during its subsequent emergence while remaining compact, and develop strong shear along its magnetic neutral line, in agreement with -spot observations.

In addition we find that very strong concentrated kinks develop a current sheet at which the magnetic field reconnects, causing field lines near the center of the tube to become knotted.

Kinky is a gigantic umbrella, the vastness of which most of us can’t comprehend.

This reconnection could be related to the high flare activity of -spots. They are typically tens of thousands of kilometers in diameter and consist of a dark region, or umbra, with magnetic field of several kilogauss surrounded by a brighter penumbra of somewhat lower magnetic field. Both the umbra and penumbra are darker in white light than the quiet photosphere, and the field strengths in the umbra and penumbra are typically 2 orders of magnitude higher than the average field strengths in the quiet photosphere.

Sunspots often emerge into the photosphere as small pairs of opposite magnetic polarity spots that grow over the course of several days into a full-sized sunspot group. A fully developed spot group typically consists of one or more "leading" polarity spots, with several "following" spots of the opposite polarity trailing behind, in that sense of the Sun's rotation. Together with the coronal magnetic loops that connect them and other associated magnetic features, these are called "active regions.

In addition, for a given solar cycle and a given hemisphere north or souththe polarity of the leading portion of the spot group tends to be the same for most active regions, as first noted by Hale et al. The special class of active regions called -spot active regions are an exception to these rules.

What does kinky mean?

In addition they are often observed to rotate about one another as they evolve Leka et al. These active regions are of particular interest because they are known to be much more flare active than normal active regions. In this paper we study a possible mechanism, the current driven kink instability, for the formation of "island -spots," that is, regions that emerge as -spots rather than being created from the collision of ly emerged umbrae.

An active region is believed to be the manifestation whay and above the photosphere of the apex of a magnetic flux tube that arches into the corona from the convection zone. The two opposite polarities of a bipolar active region are created by the intersection with the photosphere of the two legs of this arched flux tube.

I wants real woman

The fact that the two polarities are made up of a of separate spots is likely due to the fact that the emerged portion of the flux tube has fragmented. As the flux tube first emerges, a normal active region appears as two close, small regions of opposite polarity. As the tube emerges further, the spots coalesce and grow until they encompass the whole cross section of tube, and the magnetic polarities separate as more of the arch emerges into the corona.

The usual explanation for the Hale-Nicholson law is that iin source of the flux tubes, likely to be at the base of the convection zone, consists of a magnetic text parallel to the equator that breaks off into flux tubes and rises to the surface, with the flux tubes keeping approximately the same orientation what to the equator during their rise and emergence. The morphology of -spots suggests that the flux tubes that create these active regions have undergone some change during their rise konky that they do not evolve as normal spot groups do.

Mwan does have been distorted so that their apex does not emerge parallel to the equator and so that the sunspot pairs they create do not ,ean as the tube emerges, resulting in a rotated, compact active region. This, together with observations of -spots rotating during their evolution, indicates txting the legs, rather than forming a simple arch, are wrapped or knotted around each other. In Linton et al. We found the kink distorts the tubes studied kinku a helical equilibrium with amplitude large enough to generate moderate tilt in an active region.

Our goal in this paper is to continue our study of the kink instability as it applies to rising convection zone flux tubes and to continue exploring how the emergence of a kinked flux tube relates to the formation and evolution kjnky a -spot kinky region. We present our conclusions about the evolution of a rising, kinking convection zone flux tube and compare these conclusions with the simulations of Fan et al. The linear stability of various flux tube profiles has been widely studied in both nuclear fusion see, e.

Tubes with magnetic field r ,Bz r ] in cylindrical coordinates become kink unstable when the twist becomes larger than some critical value qcr. The fact that k and q have opposite s has the mean implication that the helical sense of the kink right- or left-handed is determined by the of the twist.

Eurocall2012.eu | english to somali dictionary

We plot several dispersion relations in Figure 1calculated as in Linton et al. The texhing forces in these non force-free configurations are balanced by radial pressure gradients. Note that this has a very important implication if the tube expands homologously as it rises through the convection zone, meaning that the field profile scales so that only the values of R and B0 change in equation 3.

Thus simply meaan expanding, tube A will become more kink unstable. Note that for highly twisted tubes the unstable range in k space also expands approximately as predicted by relation 2 and therefore eventually extends to k 0.

What is the abbreviation for twisted kinky sex machine?

This resonance phenomenon is important in non uniform-twist tubes. The marginally stable point in the dispersion relation then manifests itself as a marginally stable surface in the tube, called the mode resonant surface, where the local twist exactly equals the wave jinky the kink. In this case, the kink is an "internal kink" that occurs within this cylindrical surface, initially leaving the tube outside the surface undisturbed.

The nonlinear evolution of the internal kink has been extensively studied in two and three dimensions in the tokamak literature see Waddell et al. These studies find that the helical deformation of the kink pushes the tube into the mode resonant surface, where a current sheet develops. In the convection zone, it is possible that these internal or resistive kinks will be suppressed by the whah resistivity of the convection zone.

If they do occur, however, we expect that they will cause cylindrically symmetric twisted flux tubes with non uniform-twist profiles to tend toward cylindrically symmetric uniform-twist tubes, as in equation 3. In either case, the tubes will then be unstable to the external kink, which we study here with uniform-twist tubes. As shown in Linton et al.

Recently it has become possible to simulate the kink instability in three dimensions numerically see, e. We numerically simulated single-mode wavelength instabilities in twisted tubes embedded in a high plasma- environment, meant to represent convection zone conditions. We focused on modes near the peak of the dispersion relation, max, arguing that modes with the highest growth rate were the best candidates for producing large kinks.

Secret sexting codes you need to know to protect your child - do you know what lmirl means?

The growth rates of the kinks studied agreed very well with those predicted by the linear theory in Linton et al. We concluded that such a helical flux tube would generate a spot region which would emerge tilted knky from the east-west direction and then rotate, as a -spot does.

Our goal here is to extend our study of the kink instability to other regions of k-space. We simulate kinks at longer wavelengths and then simulate the interaction of multiple kink modes in a tube. We then study how this affects the kink amplitude and morphology and how this relates to -spot characteristics.