"All the World's a Stage We Pass Through" R. Ayana

Thursday 22 March 2012

Plasma Tubes Connect Dark Spherical Body to Our Sun

Plasma Tubes Connect Dark Spherical Body to Our Sun

 Plasma Ball ObjectWhilst the web has been buzzing with expectation of several potential big events… out in space an incredible event has been silently brewing at the centre of our solar system. Something very weird has been happening to our Sun.

I say silently brewing, but actually in the last four days [in early March] whilst this phenomenon was under-way we have been somewhat distracted away from it due to our focus being drawn to several major solar flares and coronal mass ejections, including three X-class flares and two M-class flares. This activity in itself has been quite astonishing.

The real show however can be seen by going to the SOHO website and running the dates 08-03-2012 to 12-03-2012 into the various camera feeds available. The best for this purpose is EIT-171, though I suggest you run the dates on all feeds. Just what exactly it is that has been discovered by two Youtube channel hosts 'Sunsflare' and 'MrMBB333' remains to be concluded, however what we see with our eyes is enough to be mind blowing.

The pictures below with embedded links to original sources show us several compelling details. Then the video from Sunsflare gives us an increased level of clarity of the 'object'.

Giant Plasma Sphere Attached to Sun
This first image shows us that what appears to be an enormous black sphere is connected to the Sun by a number of plasma tubes. If you go through the different video source option over at SOHO you find that this 'plasma object' is there from at least 09-03-12 and seemingly comes around from the other side of the sun. There are at least 4 plasma tubes 'feeding' it on 10-03-12, which makes sense as plasma tubes tend to manifest in pairs, then we find that the tubes seem to merge into just one on 11-03-12 though this may just be our viewing angle.

Giant CME March 2012
Then on 12-03-2012 an enormous energy event, seemingly a massive CME, blasts out from that precise region we are monitoring, and the object and tube both vanish from the location. Whatever it is, it then 'seems' to have been thrown away from the sun as part of the stellar eruption, appearing as the white mass with twisting tendrils shooting out before it. Note too the loop of energy ahead of it rather like some kind of stargate vortex opening. The SOHO EIT304 has another image of the eruption.

Current Sunspots
To add to the mystery we can see that the current image for the position of sunspots shows nothing in the area from which the CME type event occurs, extremely peculiar. This makes no sense at all, we should be looking at a huge sunspot here to produce a CME of this enormous and massive nature. If indeed it even is a CME as we understand them.  

Following on from the events of the 11th and 12th we have been blind-sided by yet another bizarre solar happening. This time we are seeing an enormous pyramidal coronal hole covering much of the surface of our sun. We are informed by www.spaceweather.com that wind pouring out from this region will hit our planet around the 17th. What they do not mention is the sheer weirdness of the phenomena itself…

Giant Solar Pyramid Hole
 Something else that we need to make note of is the deafening silence from mainstream media and even mainstream astrology media such as spaceweather.com regarding the Jupiter sized sphere that emerged from the solar disk on the 12th and the ensuing M-class eruption that followed it. We can categorically say they have ignored this now, as today we had a report of a M-Class flare from sunspot 1429 dated 13/03/12, thus making it clear no report was to be made of the one we have all seen the images for here that occurred on the 12th!

In recent psychic contacts myself and my partner were informed that March would show some enormous events which would be capable of waking the world up to the fact something is indeed shifting in our reality. We were also informed that there was a strong chance of a large natural catastrophe such as a quake or volcano in the same month, and that by some time in April an alien vessel would make contact with our planet, under false pretences. Seeing this major March event has given me more courage to have faith in the information source!

By Bruce Fenton

Excerpted from 2012 Rising @ http://2012rising.com/article/jupiter-size-plasma-sphere-feeding-from-sun-separates-in-giant-cme-12-03-2012-is-this-the-anticipated-march-global-shift-event

Sun Spheres: A new look at a polar crown cavity

A new look at a polar crown cavity as observed by SDO/AIA

by KiPnews

Context: The Solar Dynamics Observatory (SDO) was launched in February 2010 and is now providing an unprecedented view of the solar activity at high spatial resolution and high cadence covering a broad range of temperature layers of the atmosphere.

Aims: We aim at dening the structure of a polar crown cavity and describing its evolution during the erupting process.

Methods: We use high cadence time series of SDO/AIA observations at 304Å (50000 K) and 171Å (0.6 MK) to determine the structure of the polar crown cavity and its associated plasma as well as the evolution of the cavity during the dierent phases of the eruption.

Results: We observe coronal plasma shaped by magnetic eld lines with a negative curvature (U-shape) sitting at the bottom of a cavity. The cavity is located just above the polar crown lament material.

We thus observe the inner part of the cavity above the lament as depicted in the classical three part Coronal Mass Ejection (CME) model composed of a lament, a cavity and a CME front.

The lament (in this case a polar crown lament) is part of the cavity and makes a continuous structuring from the lament to the CME front depicted by concentric ellipses (in a 2D cartoon).

Conclusions: We propose to dene a polar crown cavity as a density depletion sitting above denser polar crown lament plasma drained down the cavity due to gravity. As part of the polar crown lament, plasma at dierent temperatures (ranging from 50000K to 0.6 MK) is observed at the same location on the cavity dips and sustained by a competition between the gravity and the curvature of magnetic eld lines.

The eruption of the polar crown cavity as a solid body can be decomposed into two phases: a slow rise at a speed of 0.6 km·s
1 , and an acceleration phase at a mean speed of 25 km·s1.

Launched in February 2010, the Solar Dynamics Observatory (SDO) is the rst NASA Living With a Star mission.

SDO has on board three dierent instruments dedicated to study the magnetic and plasma evolution of the solar corona, its associated eruptive events and their consequences on the Earth.

Here we analyse observations from the Atmospheric Imager Assembly (AIA) with high time cadence ( 12s) and spatial resolution (′′ ) which provide much more detail of the corona on the limb than other comparable instruments such as SOHO/EIT and STEREO/SECCHI/EUVI.

Especially it has been shown that SDO/AIA has the sensitivity to observe far more o-limb structures than never before (Lemen et al. 2011).

Here we report on one of these structures: a cavity observed on 13 June 2010 associated with an erupting polar crown lament/prominence leading to a propagating Coronal Mass Ejection (CME) at a speed of about 300-

Send o
print requests to: S. R´egnier 350 km·s 1 (as reported in the SOHO/LASCO CME catalog, http://cdaw.gsfc.nasa.gov/CME list/ ).

Typically CMEs are observed in white light coronograph with a three part structure: the bright core related to the lament material, the cavity surrounding the core and the bright front of the CME marking the transition between the CME and the ambient corona (see e.g., Illing & Hundhausen 1986).

In a recent paper by Gibson et al. (2010), the authors studied in detail the structure, shape and evolution (mostly due to the solar rotation) of a stable cavity observed by SOHO/EIT in the wavelength lter at 195Å.

They found that, based on a forward modelling approach, the cavity is darker than the surrounding due to the depletion in density by a factor of about

2. It is clear in their study that the prominence cavity analysed corresponds to the classical cavity as dened in the three-part CME model mentioned above.

 Fig. 1. O-limb close-up on the cavity structure as observed by SDO/AIA at 304Å (left) and at 171Å (right) at 03:24:12 UT (negative images).

The formation and instability of cavities associated with a CME have been extensively modelled (see reviews by
Lin 2002; Forbes et al. 2006).

The structure often contains a twisted ux tube able to accumulate magnetic energy and  mass within it which thus can be destabilised by catastrophicmechanisms and/or external triggers.

Despite several studies of the thermal structures of cavities especially from whitelight coronographs, eclipse observations, EUV and soft X-ray imaging (e.g., Hudson et al.

1999; Hudson & Schwenn 2000; Gibson et al. 2006; Habbal et al. 2010), there is to our knowledge no observational evidence of a long time series and high cadence obsevations of cavity at dierent temperatures as provided by SDO/AIA data able to (i) clearly demonstrate the thermal structure of both the prominence and cavity material, and (ii) describe how the plasma of a polar-crown lament evolves before and during the eruption.

Thus, the observations described here focus for the rst time on the dynamics of the inner part of the cavity above the polar crown lament/prominence material and its evolution during the eruptive phase. 

We rst describe the multithermal structure of the polar crown lament/cavity (Section 2) and then the evolution of the plasma during the eruption in two dierent wavelengths (Section 3).

In Section 4, we propose a denition for a polar crown cavity and discuss the implications of our study on eruptive lament models.

2. Multithermal observations of the cavity

The event was observed on 13 June 2010 between 00:00 and 12:00 UT on the North-West limb. We focus only on the data provided by the SDO/AIA instrument using the full spatial resolution and a reduced time cadence of 3 minutes (instead of the nominal 12s).

The SDO/AIA data are processed at level 1 (test series) which includes removal of bad pixels and spikes.

The time series were corrected for pointing and jitter eects. The image calibration corresponds to a rst approximation but does not inuence our study.

An overview of the structures observed by SDO/AIA is given in Fig. 1 at dierent temperatures: (a) HeII at 304Å at
about 50000 K, (b) FeIX at 171Å at about 0.6 MK, (c) FeXII at 193Å  at about 1.6 MK (with a hot contribution of FeXXIV at 2 MK) and (d) FeXIV at 211Å at about 2 MK.

The single temperature associated with each channel corresponds to the main peak of emission in the temperature response functions provided by the SDO/AIA team (Lemen et al. 2011).

The study of the SDO/AIA channel thermal response performed by O’Dwyer et al. (2010) shows the properties of the dierent SDO/AIA broadband channels in dierent regions of the Sun (active region, quiet Sun and coronal hole).

The prominence and cavity material is supposed to be at or near the temperatures mentioned above.

The observed structures are:

(i) cool and hot plasma o the limb which are parts of a polar crown lament (see Fig. 1a, b). The plasma is conned in
an area with a characteristic height of 100 Mm and width of 80 Mm (at the start of the time series);
(ii) a dark cavity seen as a complete ellispe in the 193Å and 211Å channels (see Fig. 1c, d);
(iii) elongated barbs seen as dark material in the hot channels and connecting the photosphere/chromosphere regions to the cavity (and/or the bottom of the cavity) to supply or  evacuate mass from the

We will not discuss the dynamics of the barbs and their implications in the eruption

process in this letter.

Figs. 1a, b evidence the co-spatiality of the polar-crown material in both the 304Å and 171 Å channels .

These snapshots highlight:
- the upward (U-shaped) bending of magnetic
eld lines at the bottom of the inner cavity,
- the accumulation of prominence material along these
eld lines suggesting that a magnetohydrostatic equilibrium is in place with the magnetic eld curvature acting against the gravity.

The latter assumption is also supported by the fact that the cavity has been stable for several hours before the eruption.

Even if the location is similar, the U-shaped eld lines in both channels are not lled by the corresponding plasma in the same manner: in the 171 Å channel the length along the U-shaped eld lines lled by the coronal plasma appears longer than in the 304Å channel.

It is important to remember here that the observed structure is integrated along the line-of-sight.

Therefore limited three dimensional depth information can be derived on the polar crown lament solely from this SDO/AIA dataset only

S. R´egnier et al.: A new look at a polar crown cavity as observed by SDO/AIA

Fig. 2. Evolution of the polar crown cavity and the associated plasma (left) at 50000 K (304Å) and (right) at 0.6 MK (171Å) at three dierent times: (a) 00:03:12 UT, (b) 03:24:11 UT, (c) 06:51:11 UT and (d) 09:00:11 UT. The white arrows indicate the direction of the plasma motions. The lines parallel to the solar limb divide the dierent parts of plasma involved in the eruption (see text).

3. Evolution of the cavity

In order to study the dynamics of the eruption, we rst look at several snapshots of the cavity to describe the motions and structures of the polar crown lament.

We restrict the dynamical study to the 304Å and 171 Å channels in which the Ushaped structures are clearly seen and also for which there is  a minimum of confusion with the background emission (seeFig. 1c, d).

Fig. 2 outlines a series of images at four characteristic times of the cavity evolution: (a) at 00:03 UT when the cavity is stable at a height of 100 Mm above the surface (projection on the plane of the sky), (b) at 03:24 UT in the early phase of the eruption, (c) at 06:51 UT towards the end of cavity eruption within the SDO/AIA eld-of-view, (d) at 09:00 UT, a couple of hours after the cavity has moved into the higher part of the corona, and the plasma and magnetic eld lines are still in the process of reorganisation and relaxation.

The polar crown material is divided into two parts, namely P1 and P2, that are not distinguishable at rst (Fig. 2a) but can be dierentiated in the following frames (Fig. 2b-c by the solid line parallel to the limb).

P1 corresponds to the main part of the eruptive cavity.

In Fig. 2b, the plasma contained in U-shaped ed lines starts to move upwards (as indicated by the left arrow) whilst the plasma on the right-hand side exhibits upwards ows along eld lines (right arrow).

P2 remains stable. In Fig. 2c, the plasma in P1 is detached and thus ejected into the high corona. P2 starts to rise.

In Fig. 2d, only the plasma in P2 remains at this height in the corona whilst P1 continues its way out of the corona.

The plasma in P2 is owing down towards the low corona following the eld lines in both channels (see arrows).

From this time series, it is important to notice that the plasma in both EUV channels are located at the same place below the polar crown cavity, and this is only during the eruptive phase that the decoupling between the two is observed.

Second, we examine the radial evolution of the cavity at three dierent locations along the width of the cavity by plotting three adjacent time slices (Figs. 3 and 4): the middle location (2) corresponds to the minimum height of the cavity above the surface at the beginning of the time series, whilst locations (1) and (3) are symmetrically on both sides of the minimum height.

The cavity appears in the top left corner of the time slices and the bottom of the cavity is rst located at about 90 Mm at 304Å and 100 Mm at 171Å.

Even if the motion of the cavity is not entirely in the radial direction, the three time slices show the behaviour of a large portion of the cavity during the eruption: the similar evolution in all three slices supports the assumption that the cavity evolves as a solid body.

We notethat the cavity leaves the eld-of-view (250 Mm high) at aboutthe same time in both wavelengths (around 07:00 UT).

In Fig. 3, the time slices evidence the evolution of the cool plasma at 304Å during the eruption process: the slow rise of
the cavity during 4-5 hours and then the eruption.

The plasma of the cavity observed at 304Å does not reach heights above 250 Mm. During the eruption process most of the plasma is drained back down along magnetic structures as highlighted in Fig. 2.

From Fig. 4, we dene the initial and nal stages of the eruption as observed at 171Å from the asymptotic behaviour
of the time slice (2) as indicated by the straight white lines.

At the start, the cavity is stable justifying why we started our study at 00:00 UT. The rst phase is a slow rise of the cavity with a characteristic speed of 0.6 km·s 1 .

The cavity follows this trend until 03:00 UT. The second phase of the eruption is the fastermotion of the cavity with a characteristic speed of 25 km·s 1.

Even if this speed is far less than local Alfv´en or sound speeds,this is comparable to the speed of plasmoid ejection as reportedby Tsuneta (1997).

4. Discussion and Conclusions

We propose to dene a polar crown cavity as a density depletion at the bottom of which the polar crown lament material sits indicating the existence of a magnetohydrostatic equilibrium.

The lament material is drained down along the polar crown cavity by gravity and sustained by the action of the upward-directed magnetic eld curvature force.

This fact as well as the long, steady observations of the polar crown cavity indicate that the cavity is in a magnetohydrostatic equilibrium.

The cold and hot coronal plasma are located at a similar location along the same eld lines.

The observations of the cavity structure and plasma spatial distribution are consistent with the classical 2D cartoon of a cavity depicted by concentric ellipses.

For instance, in the classical CSHKP model (Carmichael 1964; Sturrock 1968; Hirayama 1974; Kopp & Pneuman 1976), the eruptive structure is composed of a twisted ux tube at the bottom of which the plasma is concentrated.

Contrary to the cartoon proposed by Cliver et al. (1986) placing the lament material at the centre of the cavity, the lament material is located at the bottom of the cavity which is more consistent with the model of Martens & Kuin (1989).

S. R´egnier et al.: A new look at a polar crown cavity as observed by SDO/AIA

 Fig. 3. Time slices of the eruptive cavity as observed in 304Å on 13 June 2010 by SDO/AIA. The image on the left has been taken at 03:24:12 UT in log scale to highlight the cavity. On the right, the time slices are plotted along three dierent radial directions: (1) and (3) are on the sides of the cavity, (2) is at the minimum of the cavity. The three location are chosen at the beginning of the time series running from 00:00 UT to 12:00 UT. The vertical axis represents the distance in Mm from the bottom (on the disc) of the time slices. The white vertical line indicates the time of the image on the left. The movie is provided as online material.

In the observations reported here, magnetic curvature compensates gravity to create an equilibrium state in which the density is considerably increased at the bottom of the cavity.

We also show that the ows along eld lines and varying from one wavelength to an other are important for the initiation (Fig. 2b) and relaxation (Fig. 2d) phases of the eruption.

We also note that the rise of the cavity (divided in two stages) is similar to the plasmoid eruption initiated by an impulsive are as reported by Ohyama et al. (1997) (see also Shibata 1998).

Fig. 4. Same as Fig. 3 for the 171Å channel. The asymptotic behaviour is indicated by the straight white lines. The estimated speeds are also indicated. The movie is provided as online material

This preliminary study describes the structure and evolution of a polar crown lament and its cavity projected onto the plane of the sky and, in any case, gives a full picture of the eruption process.

In a forthcoming paper, we will discuss the possible triggers of the cavity eruption of concomitant external (ares, CMEs) and internal (kink/torus instability, mass loading) phenomena by combining SDO/AIA and STEREO/SECCHI/EUVI images which give us a more realistic 3D representation of the event.

Acknowledgments. We thank the referee for his/her useful commentshelping to improve the letter. The SDO/AIA data have been obtained through the University of Central Lancashire database.

The data used are provided courtesy of NASA/SDO and the AIA science team.
CEA acknowledges the support of the STFC studentship programme.

The SOHO/LASCO CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University ofAmerica in cooperation with the Naval Research Laboratory.

SOHO is a project of international cooperation between ESA and NASA.

A new look at a polar crown cavity as observed by SDO-AIA .S. R´egnier et al.: A new look at a polar crown cavity as observed by SDO/AIApdf Structures and dynamics

This is the Video that went Viral on the Internet Pretending there was a Alien like spherical structure aside the Sun:

From Knowledge Is Power @ http://www.kipnews.org/2012/03/12/sun-spheres-a-new-look-at-a-polar-crown-cavity/


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  1. A "U" shape is not the same as a "spherical" shape. U and O are not alike. The U looks like a normal coronal cavity, however the spherical one we see, does not.

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