What a gravity wave is and is not

Astrophysics Magnetic wave energy fluxes for late-type stars

www.ita.uni-heidelberg.de/~ulm/papers/umf2001.pdf - Cached
Key words. methods: numerical – stars: chromospheres – stars: coronae – stars:
magnetic fields – MHD. 1. Introduction. It has become clear in recent years that …

NASA identifies magnetic reconnections via flux tubes and the shock waves they produce.


ALL PICTURES AND ASSOCIATED COMMENTARY ARE FROM ANN’S ASTRONOMY
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If Hoag’s Object is not gravity formed but by the event of being in the sight of a perfectly aimed electro-magnetic field that would make it a product of symmetry and not gravity.


http://annesastronomynews.com/pod-archive/may-2012/
May 2012 So-called “classic” ring galaxies are generally formed by the collision of a small galaxy with a larger disk-shaped galaxy. This collision produces a density wave in the disk which leads to a characteristic ring-like appearance. Such an event would have happened at least 2-3 billion years in the past. However, there is no sign of any second galaxy that would have acted as the “bullet”, and the core of Hoag’s Object has a very low velocity relative to the ring, making the typical formation hypothesis quite unlikely.

Monoceros:

May 1, 2012

V838 Monocerotis, a star that experienced a major outburst

V838 Monocerotis (V838 Mon) is a red variable star about 20,000 light-years away in the constellation Monoceros. It spans about 14 light-years, what makes it one of the largest known stars. It did not expel its outer layers; instead it grew enormously in size.
The previously unknown star was observed on January 6, 2002 experiencing a major outburst. The initial light curve resembled that of a typical nova eruption, it was then realized to be something completely different. The reason for the outburst is still uncertain.
V838 Monocerotis reached maximum visual magnitude on February 6, 2002, after which it started to dim rapidly, as expected. However, in early March the star started to brighten again, this time mostly in infrared wavelengths. Yet another brightening in infrared occurred in early April, after which the star returned to near its original brightness before the eruption. The light curve produced by the eruption is unlike anything previously seen.
It appears that the progenitor star is considerably more massive and luminous than the Sun, but at the time of maximum V838 Mon was one of the most luminous stars in the Milky Way. The brightening was caused by an abnormal rapid expansion of the outer layers of the star. The laws of thermodynamics dictate that expanding gas cools. Therefore the star became extremely cool and deep red. In fact, some astronomers argue that the spectra of the star resembled that of L-type brown dwarfs. If that is the case, V838 Monocerotis would be the first known L-type supergiant.
Rapidly brightening objects are known to produce a light echo. The light continues propagating outward through a cloud of dust surrounding the star. The light reflects or “echoes” off the dust and then travels to Earth.
In the case of V838 Monocerotis, the light echo produced was unprecedented. While the photos taken by Hubble appear to depict an expanding spherical shell of debris, they are actually formed by reflecting dust that is mostly ‘behind’ the star, not in ‘front’ of it.
There is strong evidence that the V838 Monocerotis system is very young and still embedded in the nebula from which it formed.
These images are showing the expansion of the light echo, from May 20, 2002 until February 8, 2004.

From 2012: Another enigma:November 20, 2012

NGC 3132, a bright planetary nebula in Vela

Image Credit: NASA, ESA and the Hubble Heritage Team (STScI/AURA)

NGC 3132 (also known as the Eight-Burst Nebula because of its figure-8 appearance through small telescopes, or the Southern Ring Nebula) is a very bright, asymmetric planetary nebula of approximately 0.4 light-year across, located about 2,000 light-years away in the southern constellation Vela. It is moving away from us at 49 kilometers per second.
Despite their name, planetary nebulae have nothing to do with planets. The name of planetary nebulae arose because of the visual similarity between some round planetary nebulae and the planets Uranus and Neptune when viewed through early telescopes.
When a star with a mass up to eight times that of the Sun approaches the end of its life, it blows off its outer shells and begins to lose mass. This allows the hot, inner core of the star to radiate strongly, causing this outward-moving cocoon of gas to glow brightly as a planetary nebula.
Over the next several thousand years, the nebula will gradually disperse into space, and then the star will cool and fade away for billions of years as a white dwarf. Our own Sun is expected to undergo a similar fate, but fortunately this will not occur until some 5 billion years from now.
There are two stars close together — a binary system — in the center of NGC 3132, one of 10th magnitude, the other 16th. It’s the dim star, not the bright one, near the center that caused multiple outbursts and originated the intricate, somewhat concentric structure of the nebula. This hot central star is a white dwarf of about 100,000 K that has now blown off its layers and is making the nebula fluoresce brightly from the emission of its intense ultraviolet radiation.
This expanding cloud of gas is one of the nearest known planetary nebulae. The gases are expanding away from the central star at a speed of about 14.4 kilometers per second. Neither the unusual shape of the surrounding cooler shell nor the structure and placements of the cool filamentary dust lanes running across NGC 3132 are well understood.
This image is taken with the Wide Field Planetary Camera 2 onboard the Hubble Space Telescope using three different color filters. North is to the bottom left hand corner of this image.

Just Right formation: Champagne: November 10, 2012

Holmberg II, a dwarf irregular galaxy in Ursa Major

Image Credit: NASA & ESA

Holmberg II (also known as Arp 268 and UGC 4305) is a very bright dwarf irregular galaxy located only about 9.8 million light-years away in the constellation Ursa Major. It is a member of the M81 Group of galaxies, and one of the few that isn’t distracted by gravity from other nearby galaxies.
This small galaxy is a patchwork of dense star-forming regions and extensive barren areas with less material, which can stretch across thousands of light-years.
Holmberg II is dominated by giant bubbles of glowing gas – the largest about 5,500 light-years wide – which are regions of old star formation. The cavities are blown by high-mass stars (as these stars form in dense regions of gas and dust, they expel strong stellar winds that blow away the surrounding material) and of gas by the shock waves produced in supernovae (the violent explosions that mark the end of the lives of massive stars).
As a dwarf galaxy, it has neither the spiral arms of galaxies like the Milky Way nor the dense nucleus of an elliptical galaxy of which the gravitational pull would destroy the fragile bubbles. This makes Holmberg II a gentle haven where these fragile structures can hold their shape.
New star birth is also taking place, but not in the same areas as the bubbles because these are drained now of gas or dust. The star formation regions in Holmberg II appear as massive, disorganized patches filled with hundreds of young, blue stars, that occupy a relatively large fraction of the disk. One region in particular has almost as many young stars as the famous Tarantula Nebula in the Large Magellanic Cloud.
Holmberg II is the perfect example of the “champagne” model of starbirth – where new stars create even newer ones. It works like this: when a bubble is created by stellar winds, it moves outwards until it reaches the edge of the molecular cloud that spawned it. At the exterior edge, dust and gas have been compressed and form a nodule similar to a blister. Here another new star forms.. and triggers again… and triggers again… similar to the chain reaction which happens when you open a bottle of champagne.
The galaxy also hosts an ultraluminous X-ray source in the middle of three gas bubbles in the top right of the image. There are competing theories as to what causes this powerful radiation — one intriguing possibility is an intermediate-mass black hole which is pulling in material from its surroundings.
Holmberg II enables astronomers to study star birth in an environment that isn’t disturbed by density waves (as happens in larger galaxies such as the Milky Way) or by deformation caused by the pull of another galaxy, and that is conveniently close.
This image was captured by the NASA/ESA Hubble Space Telescope. It is a composite of visible and near-infrared exposures taken using the Wide Field Channel of Hubble’s Advanced Camera for Surveys.


Papillon in the LMC:
of the Day: The Papillon Nebula
Anne's Picture of the Day
nov 242012

November 24, 2012

The Papillon Nebula, a compact H II “blob” in the LMC

Image Credit: M. Heydari-Malayeri (Paris Observatory) et al., ESA and NASA

The Papillon Nebula (N159-5) is a butterfly-shaped High Excitation Blob (HEB) of less than 2 light-years across within the nebula N159, a turbulent star-forming region of more than 150 light-years across. It is located in the Large Magellanic Cloud, about 170,000 light-years away in the constellation of Dorado.
High Excitation Blobs (HEBs) are compact H II regions, a rare class of ionized nebulae in the Magellanic Clouds. They are characterized by high excitation, small size, high density, and large extinction compared to typical Magellanic Cloud H II regions. These objects are tightly linked to the early stages of massive star formation, when the stars begin to hatch from their parental molecular clouds.
This compact ionized “blob” is buried in the center of the maelstrom of glowing gases and dark dust in N159. This image shows unprecedented details of the structure and internal morphology of the Papillon nebula (“Papillon” is French for “butterfly”).
A possible explanation of its bipolar shape is the outflow of gas by strong stellar winds from newborn massive stars (over 10 times the mass of our Sun), hidden in the central absorption zone. Such stars are so hot that their radiation pressure halts the infall of gas and directs it away from the stars in two opposite directions. Presumably, a dense equatorial disk formed by matter still trying to fall in onto the stars focuses the outstreaming matter into the bipolar directions.
It is rather rare that we can see massive stars so early after their birth.
This image was taken on September 5, 1998 with the Wide Field Planetary Camera 2 onboard the Hubble Space Telescope.



A galaxy with closed lobes: The Cheeseburger:

Anne’s Picture of the Day: The Cheeseburger Nebula

Anne's Picture of the Day
dec 102012

December 10, 2012

The Cheeseburger Nebula, a planetary nebula in Cygnus

Image Credit: ESA/Hubble & NASA; Acknowledgement: Linda Morgan-O’Connor

The Cheeseburger Nebula (NGC 7026) is a very bright bipolar planetary nebula of a little over one light-year across at its longest dimension, located about 6,000 light-years away in the constellation of Cygnus (The Swan). It is approaching us at approximately 40.6 kilometers per second.
Despite their name, planetary nebulae have nothing to do with planets. The name of planetary nebulae arose because of the visual similarity between some round planetary nebulae and the planets Uranus and Neptune when viewed through early telescopes.
A planetary nebula represents the final stage in the evolution of a star similar to our Sun. Only a few thousand years ago, the star at the center of The Cheeseburger nebula was a red giant, but when it ran out its nuclear fuel, it ejected its outer layers into space to form this glowing, expanding nebula, while leaving behind its hot stellar core in the center.
Over the next several thousand years, this cloud of glowing gas and dust will gradually disperse into space, and then the star will cool and fade away for billions of years as a white dwarf. Our own Sun is expected to undergo a similar fate, but fortunately this will not occur until some 5 billion years from now.
The Cheeseburger has two big closed lobes — filled with very hot gas that emits X-rays — that are roughly butterfly-shaped, and a bright equatorial waist that contains large amounts of molecular gas and dust with the hot central white dwarf star right in the middle. Because the stellar winds that form the lobes are still plowing into the surrounding material, and because the lobes are closed, the hot gas hasn’t been able to escape.
Which could mean that eventually all that material may blow out of the lobes, popping them. When that happens – in what’s called a “blowout” – the gas will escape and it’ll probably form long, weird, filaments.
This image was produced by the Wide Field and Planetary Camera 2 aboard the Hubble Space Telescope. It shows the vivid colors that are produced by the mix of gases present in NGC 7026: starlight in green, light from glowing nitrogen gas in red, and light from oxygen in blue (in reality, this appears green, but the colour in this image has been shifted to increase the contrast).



The articles and beautiful astronomy pictures are from Ann’s Astronomy website.

This article:

http://voxcharta.org/2012/10/14/discovery-of-multiple-dust-shells-beyond-1-arcmin-in-the-circumste

says multiple shell remnants have been discovered. I suggest these are the residues of controlled novas. This would leave ‘dust’ and this dust then becomes rings. This also would indicate that controlled novas are the majority and not the minority; our fascination beautiful expanded hot gas nova phenomena is due to the fact that it is currently the tip of our technological progress.


Getting Closer: a star of red giant size is discovered to not have ‘come back to life’ but had a small companion that could not absorb the amount of cosmic wind offloading from the giant and went boom. The scientists know this as there WAS NO GAS SHELL PRODUCED.
I speculate that our Sol went nova as O Manuel says in Iron Sun, but the gas shell was not allowed to escape and instead was recaptured and layered on the controlled nova product that was a high magnetic body and in doing so created a lighter magnetic shell producing a LOH (low magnetic field over high) star.
Here: http://www.newscientist.com/article/dn22448-astrophile-bornagain-star-faked-its-death-scene.html
NSV 11749 is a symbiotic nova. Tho in similar red giant rebirths (only 4 known) there is a gap that shows when the shock wave impacts and that indicates the white dwarf erased the cosmic wind in the immediate vicinity of itself.
There are endless variations of solar formation and a twin system in a bubble shell emprisoned by massive magnetism would force this energy inward, creating a massive magnetic body overlaid with a lightly magnetized charged gas envelope. Sol.

This may be what occurred ½ billion years ago. This might explain the small LT starbit I propose returns to visit the Oort shell, the place of its birth, on its nearest orbital point, before looping outward toward Centauri A&B.

Note that the LMC is fraught with gaseous bubbles. A complete and semi bubble appear in astronomical recordings. One might conjecture this gas would normally be compressed magnetically into a central trap. That has not been done and the gas roams at will within the cloud being compressed by roving bands of current sponsored magnetism. I propose this cloud must be saturated with electro magnetism and the gas freely available for star-forming.



Now the question is does this substantiate my theory of black hole aging and the regurgitation of the gas? As it is unknown if the LMC ever hosted a black hole, and the cloud shows no sign of former spiraling that would indicate a previous life, I propose the cloud never acquired a central electro-magnetic trap. There is evidence of a papillon shape which may be indicative of a Birkeland current pinch providing star forming. Could it be that stars form without the aid of a gravity disc rotation?

Would a disc have to be more massive that the LMC could produce for it to acquire a LT electromagnetic body? Would the BC s have to collimate? I suggest the aging of a LT central body would be intimately connected to the decreasing pressure so the growth of the LT star body would have to be connected to increasing pressure supplied not by gravity but by electromagnetism.

How large do gas clouds exist? Is there a size that always falls to forming a central LT body?
Would gas clouds too small to acquire a LT star body be a preferential home for life?




Gravity waves are not compression waves, pressure waves, etc. All of those actions exist within our small galaxy. Gravity waves are conjectured to exist when proposed black holes trajectories cross paths. This phenomena of gravity waves is associated with black holes because both are GRAVITY descriptions of galactic proportions.

I depict LT starbodies as primarily electromagnetic traps whose function as light mazes depends on massive gas pressure; the kind generated by massive magnetic fields. Hence when this particular magnetic pressure is not able to be generated the LT starbody cannot hold the gas inside and exhausts it into the galaxy in spite of the fact it still resides at the center of a gravity galaxy. Thus we see swollen galactic centers claimed to be massive black holes where they are exhausted gases from the LT starbody. This hot gas streams outward expanding and cooling.

The gas becomes cold; the galaxy disappears from visible to invisible. The material in this now cold gas becomes disorganized and loosely focused. It may even degrade into a cloud or lesser. How a LT starbody degrades after being emptied of gas could be as simple as becoming a clump of stars.