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http://www.fas.org/irp/imint/docs/rst/Sect20/A6.html
 
Found this Link while  I was investigating Cygnus.....
and wanted to keep it for reference, as its good to know More about all the awesome SpacePics we are now getting to see ! Alot is looking familiar!
Imagine also, this is happening within you as well as without!     xoxo  annie

"The end result of a collision depends on several factors: 1) whether there is a direct hit or a glancing encounter; 2) the relative size (mass) difference between colliding bodies; 3) the terminal speed of each body. The process can be as brief as an hour; or as long as days to years (this rapid time for completion is one reason while such events have yet to be observed in "real time"). Any two of the 7 density types shown near the top of page 20-5 can experience a collision. In some combinations, such as a white dwarf striking a red giant, the end result is two White Dwarfs (one being the incoming member; the other [Red Giant] dispersing and losing so much of its gas by the interaction that only its core remain which quickly evolves into the new White Dwarf, Or, one star remains relatively intact as the second star is incorporated within it."        <<<<<found this an interesting bit of information   !!!!

 

 
 

 

 
 

 

1‑s2.0‑S0273117707004723‑gr1.jpg
sciencedirect.com
 
378 × 366 - Right-upper: ROSAT HRI image of the entire Cygnus Loop.


 
 

 

 
 

 

AAAAA.jpg
latenightinthemidlands.com
 
640 × 480 - ... satellite and shows an ultraviolet view of the so-called Cygnus

Navigation
Novae, Supernovae; Neutron Stars and Pulsars; Quasars and Black Holes; Gamma Ray Bursts; and Star Collisions.
 

Novae and Supernovae

Periodically, a bright object appears in a galaxy and remains that way for days to months. It is referred to, erroneously, as a new star or nova (Latin for "new"; plural, novae). It is, in fact, a star that for more than one reason experiences a major flare-up that later dies down leaving the star intact but with loss of material. Star V838 in the Monoceras constellation underwent such a flare-up of a blue star, releasing considerable material as it reached a luminosity of ~600000 times that of the Sun.
 
Nova developing in star V838.
Soon after its discovery, this nova has been examined in close detail by the HST, yielding this dramatic sequence of images:
 
Sequential images, made by the HST, of clouds of dust and gas moving outward from the V838 nova.
Recently, a new hypothesis about its effects on possible planets orbiting it contends that the flare-up consumed these planets. There is, of course, no direct evidence that there were any planets around this star. But the spectra obtained for the nova phase of V838 show a strong enrichment in Li, Al, Mg and other elements that could have been concentrated in planetary bodies that were caught up in and destroyed by the expanding shell of gases in the flare-up. This is the predicted fate for most planetary systems as the parent star expands its gaseous envelope. Our Solar System will likely be destroyed by such a process in about 5 billion years hence (see page 20-11).
Novae are common events in individual galaxies. One way in which these occur is as follows: What in fact is being observed is a binary star system, one member of which is a White Dwarf and the other a Red Dwarf or even more massive Main Sequence or Red Giant stars. The process involves stripping off of hydrogen from the larger companion star which streams toward and is added as an accretion disk to the White Dwarf, whose gravity controls the activity. This artist's concept in the right illustration below shows what happens (in reality, the material being removed is often not be luminous which is why the actual process is not observed around such star pairs). On the left is an actual case, in which Chandra has produced an X-ray image of star Mira B, a White Dwarf, receiving material pulled from its companion, Mira A, a Red Giant.:
 
Artist's conception (right) of gaseous hydrogen and other materials being removed from a Red Giant onto a White Dwarf; an actual example (left) is the streaming of material from Star Mira A to Star Mira B.
 
This accretion process causes a buildup of hydrogen gas around the White Dwarf until compression under the strong gravity raises the temperature to 107 °K, at which condition nuclear fusion occurs. This causes a sudden brightness of the White Dwarf and a rapid consumption of the accreted hydrogen some of which also may be expelled. The process repeats through a number of cycles, at time scales of 1000s to 10000s of years per flare-up. Novae are therefore recurring events, without star destruction at each occurrence, in distinction to the supernovae described below. The illustration below shows a nova near its peak brightness; the specks around it are ejected hydrogen (the star near the bottom may [?] be the source of the accreted material):
 
Supernova in the galaxy T Pyxidis
This star, normally a small ordinary type in the Milky Way about 20000 light years from Earth, is an eruptive variable in which the hydrogen-burning undergoes a significant flare-up, enlarging the star somewhat but not directly shredding off or expelling significant mass. At its peak, the star had about 600,000 times the energy output as the Sun but in time settled back to its prior state. What is observed above in the sequence left-right top-bottom is the outward driving of dust clouds made luminescent by the energy release.
More massive stars, originally with 8 to 50+ solar masses, burn their gaseous fuel (in the plasma state [atoms are ionized]) much more rapidly until nuclear processes force the gases away at high velocities from the core in an explosion whose early stage may be seen from Earth for a few years as a hugely luminous event called a supernova. One such very bright event was imaged by HST on April 28, 1998 in the spiral galaxy NGC3982; the supernova is the large blue-white object in an arm off the galactic center. Supernovae occur, on average, about once every 30-50 years in a galaxy.
 
1998 Supernova in galaxy NGC3982.
Credit: H. Dahle
The rapid rise and decrease of luminosity during a supernova event (labelled "transect") was captured visually through a telescope looking at GRB 011121 (a gamma-ray-burst source; see below):
 
Time-sequenced observations of the supernova associate with a GRB event.
 
In February, 1987 the brightest supernova in nearly 500 years, SN1987A (located in the Large Magellanic Cloud), was discovered in the southern hemisphere skies from an Observatory in Chile. Here is a before-after image made by a telescope at the Anglo-Australian University:
 
Optical telescope image of stars in the Large Magellanic Cloud (left), one of which (arrow) became a large, brilliant supernova in 1987.
Since 1987, it is being continuously monitored both from Earth and from the HST, providing a "stellar" example of the self-destruction of a star by catastrophic explosion. It appears to still be in a declining luminosity phase going into the 21st Century.
 
Sequential observations of SN1987A in which variations in luminosity have been density-sliced to showing its gradual decline in brilliance; in this rendition blue has been assigned to highest luminosity and red to lowest.
This next image is one of the most spectacular views of 1987A yet acquired by the HST. The single large bright light is a star beyond the supernova environs. Around the central supernova is a single ring but associated with the expansion of expelled gases are also a pair of rings further away that stand out when imaged at a wavelength that screens out much of this bright light.
 
A pair of distant rings around SN1987A; a brighter continuous ring closer to the star's remnants is discussed below.
Visual changes around the star remnant and its surroundings have since been observed over the last 15+ years, as shown in this sequence made with the Wide Field Camera on HST
 
Sequence of WFC HST images of the inner right around SN1987A
The most recent image (lower right) is here enlarged to show detail (upon first seeing just this image, the writer was so astounded that he thought the scene was an artist's rendition).
 
Close-up view of the most recent SN1987A image; the central supernova is now a faint glow.
This supernova is also expressive as a concentrated source of x-ray, UV radiation, and radio waves. Here is the first Chandra X-ray image of SN1987A:
 
Chandra image of SN1987A
The next figure shows SN1987A seen in the optical range by HST (upper left), by an Australian Radio Telescope (upper right), and by Chandra on two dates (lower left: Oct 1999; lower right: Jan 2000):
 
Images of SN1987A, as described in the above paragraph.
The SN event began about 167,000 years ago, based on distance measurements but its light burst is only now arriving at Earth. The star 20000 years earlier first cast off an envelope of gases as it expanded to a Red Giant. As its core collapsed, it finally exploded violently in seconds, pushing away exterior gases driven by shock waves, and releasing a huge burst of neutrinos as the core protons and electrons were squeezed into neutrons. It is heating of the gases in the ring by these shock waves that has now been producing first a few, then more, of the bright light spots in the ring. In time, it is predicted that the spots will merge and the whole ring will become bright.
A recent estimate of supernova formation rate in the Milky Way galaxy predicts a new one will occur on average about once every 50 years.
Supernovae in our galaxy and others nearby can appear as very bright light sources sometimes visible to the naked eye. One of the most famed in history is known familiarly as Supernova Kepler, named after the great astronomer who first observed it on August 8, 1604. In celebration of the 400th anniversary of its sudden appearance as a "new star" brighter than any of the planets, astronomers have produced this composite of Chandra, Hubble, and Spitzer Space Telescope images (the one on the right is recording mainly (in red) the dust in the supernova:
 
Supernova Kepler.
Another prime example of a bright, long-lasting supernova is this Palomar telescope view of the Crab Nebula (left), with an HST Wide Field Camera view of the volume within the square shown on the right). Below this image pair is an HST image of this Crab Nebula - a marvelous example of the aesthetic nature of many stellar displays.
 
Image pair of the Crab Nebula showing an image from the Palomar telescope and an enlarged section of the nebula taken by the Hubble Space Telescope.
 
Lets take a closer look at this nebula - perhaps the most studied by astronomers to day - by first showing a ground telescope view made by the CFHT and then an HST view. Both show remarkable detail, once again proving that for closer astronomical objects ground telescopes can compete with the excellence achieved by the Hubble Space Telescope.
 
 
CFHT telescope image of the Crab Nebula.
 
HST image of the Crab Nebula.
The Crab Nebula is famous in history. It was first observed on July 4, 1054 A.D. by Chinese astronomers as a suddenly appearing bright light, seemingly within the Taurus constellation, which remained intense enough so that for a few years it could be seen even during the day. Modern telescope views show that filaments are streaming from the explosion center at speeds up to half that of light. This supernova is, like others in general, an extremely energetic event, radiating from short wavelengths (gamma rays) through the visible and into the long wave radio region. A pulsar-neutron star (see below), rotating 30 times a second, has been detected in its central region. (Recall that the Crab nebula was imaged in four spectral regions, as displayed on page I-3 in the Introduction).
The Crab Nebula has a notably different shape when imaged with x-ray radiation by the Chandra Telescope. We show that below, and beneath it is a striking image made by combining this x-ray image with a visible light image made by the HST. A ring structure emerges and a jetlike protuberance extends roughly perpendicular to the ring.
 
Chandra x-ray image of the Crab Nebula; a Pulsar is located within this nebula.
 
A composite image of the Crab Nebula made by combining the above image with a visible light image made by the HST.
Recently, the HST returned images of the Crab nebula that show the details of the excited gaseous filaments now extending far out into space from the neutron star core. The principal element in many of these filaments is identified by its (process-determined) color: hydrogen = orange; nitrogen = red; sulfur = pink; oxygen = greenish.
 
Gaseous filaments within the Crab Nebula in an excited state rendering them luminous as seen in this HST image.
 
Another detailed view of the Crab Nebula's filaments.
 
Supernovae are also quite impressive when rendered as images using x-radiation. Witness this Chandra view of Cassiopeia A:
 
Cassiopeia A, a supernova visualized here by coloring x-ray levels as determined by the Chandra X-Ray Telescope.
This next image demonstrates how long exposure times can bring out much more detail in a distant astronomical object. Again, Chandra has looked at Cassiopeia A, but with an exposure time of 11.5 days. X-ray wavelengths bring out the distribution of Fe and Si, along with other elements. Of special note are the red jets emanating from the still expanding gaseous matter. The surviving neutron star is not evident in the image.
 
Long-time exposure of x-radiation around Cassiopeia A, imaged by Chandra.
An HST image shows the filamentous structure of the Cassiopeia A supernova. The star that blew up in this constellation was about 10000 light years away. The event took place at that star around 10000 years ago. Historical records note a bright star appearance in the 1600s. In this rendition, oxygen-rich clouds of gas/particles are blue; sulphur is red.
 
The Cassiopeia A supernova.
The Spitzer Space Telescope has examined Cassiopeia A in the near IR. This image of the gaseous matter around the burst star looks much like a fireball as we would see an aerial bomb burst on Earth:
 
Near IR Spitzer image of the Cassiopeia A supernova.
 
However, a surprise greeted investigators when this burst was imaged using a combination of IR bands. Observe this image.
 
Longer wave infrared image of Cassiopeia A, obtained through the Spitzer telescope.
 
One of the bands used to make the image is centered on 24µm. The excited gaseous material making up the glowing filaments was determined to be moving near the speed of light, so that pictures taken a year apart show distinct positional differences. This does not fit a simple growth of the explosion nebula that began 324 years ago. The tentative interpretation: the neutron star that remains after the supernova can produce "echoes" by repeating blasts that re-energize the gaseous material. Calculations indicate a neutron star event about 50 years ago that sent a blast wave through the outwardly progressing gas. A mechanism to cause this neutron star activity is still speculative.
Another supernova with "strings" of gas and matter debris that occupy various orientations is seen in this HST image:
 
Supernova with distorted bands of gas that form a series of strands and loops.
Individual filaments have been examined in detail. Here is part of the Cygnus loop, part of a supernova, seen in visible (top) and in an image produced from gamma radiation:
 
A filament in the Cygnus loop, seen by HST in visible light.
 
Same segment as above, but imaged from gamma radiation detected by Chandra.
From the preceding images, it should be obvious that supernovae are the "spectacular fireworks show" that delights both astronomers and the public alike when the resulting images are widely displayed. In recent years, astronomers have become quite adept at spotting a supernova soon after it explodes and then training a variety of sensors - both ground- and spaceborne - to preserve the high moments of the event's expansion. Here is still another "sensation", SN49, in the Large Magellanic Cloud; the elements associated with particular colors are identified in the caption:
 
SN49 in the LMC; reds denote hydrogen excitation, green = oxygen; blue = sulphur.
Also in the Large Magellanic Cloud is Supernova N312D. It is 163000 light years away. The image below, made as a composite of HST and Chandra images, shows the extent to which it has expanded and dispersed after 3000 years. By this time the excited gases are diffuse so that the visual stage of the supernova is no longer dominant. :
 
Supernova N132D; pink denotes Hydrogen excitation; purple is from Oxygen excitation; blue associates with high temperature X-ray excitation.
 
Another supernova example is Eta Carinae, in the 19th Century the second-brightest star in the sky (southern hemisphere) but today is too faint to be seen with the naked eye. Here is a Hubble Space Telescope view of the nebula-like appearance of this exploding star:
 
Full view of the supernova Eta Carinae; HST.
When processed using a combination of red and UV filter images from HST, the central part appears as an apparent "cloud" of matter which is actually mainly a light burst from this supernova, now some 10 billion miles across, that resulted from the explosion of a star 150x more massive than our Sun.
 
Enlargement of the central gaseous dumbell shaped envelope around Eta Carinae, as imaged through red and ultraviolet filters on the HST camera.
The Red Giant, TTCygni (in the constellation Cygnus), is a carbon-rich star which as it explodes expels carbon monoxide (CO) in a discrete ring that has now advanced to about 0.25 light years from the central Giant.
 
A ring of excited CO gas around the late stage Red Giant TTCygni.
A variant of the gas distribution around a supernova is sometimes referred to as "a stellar geode", (the term "geode" is an analogy to rocks which contain cavities, usually lined with crystals). N44G, in the Large Magellanic Cloud (160000 l.y. away), is a star which acts like a supernova to drive surrounding gases into a "bubble" using stellar wind and UV radiation. This HST view uses a red filter to detect hydrogen and a blue filter to respond to sulphur excitation. The cavity is presently about 35 l.y. in diameter. More than one explosion is suspected (perhaps several supernovae). This cavitation process is relatively rare.
 
A massive bubble created by stellar wind/UV radiation, possibly powered by a supernova explosion.
Once a supernova is spotted, its rather short history can be monitored in terms of changes in luminosity over time. The graphs below plot brightness variations for several supernovae of recent vintage and for older supernova whose remnants are still visible.
 
Changes in supernovae brightness over time (age in years back from the present, plotted on a log scale.
Astronomers have distinguished between two general types of supernovae, separated by the intensity of the luminosity and by the pattern of decreasing light output over time. These are simply labeled: Type I and Type II supernova. The latter has proved particularly useful as another "standard candle" - any class of stellar or galactic objects whose (known) intrinsic luminosity (total power output) remains fairly constant at a specific time in their evolutionary history - in the quest to determine distances to far away stars/galaxies and to relate these to rates of expansion. The two types are shown here in this generalized plot:
 
Changes in luminosity with time for the two general types of supernovae.
A variant of Type I, now referred to as the Ia type supernova, has become center stage in the recent recognition that the Universe is now accelerating rather than slowing down (see page 20-10 where the behavior of this type is considered in detail). Type 1a results when a White Dwarf has grabbed so much matter from a neighboring star (with which it is paired; see top of this page) that it undergoes an implosion followed by a sudden explosion. This event is accompanied by a characteristic spectrum. Type 1a's are less common than the Types I and II; a 1a occurs on average about once every three years in a galaxy.
A somewhat different mode of destruction of a massive star involves violent, chaotic expansion of red-glowing (in the visible) gases from a star type known as a Wolf-Rayet star, as shown below, here seen in an early stage of expansion around the still-intact central Giant (about 40-50 solar masses).
 
 
Image of a Wolf-Rayet star in a state of chaotic expansion.
A star close to the Sun that explodes as a supernova (or hypernova; see below) can send shock waves and high-speed particles to distances that could envelop the Earth. This is very unlikely at any given time, such as NOW. But, statistically it is finitely possible, and could be one cause of mass extinctions of life on our planet. A group of astronomers have pointed out that a large number of O and B stars occur in a nearby cluster positioned in the sky near the meeting of the Scorpio and Centaurus constellations. Some once in this cluster may have passed through supernovae stages. That Earth may have been affected is implicated by evidence of a deficiency of interstellar matter (including gas) in the so-called "Local Bubble" within which the Sun lies. A consequence of this is that there is less material in our neighborhood that absorbs or impedes light from more distant parts of the Universe; this improves viewing conditions of those cosmic sources. There may be geologic evidence for supernovae material having reached the Earth: marine deposits dated at 2 and 5 million years are enriched in an iron isotope that would be expelled during a supernova explosion.
In December, 1997, astronomers observed a localized event in deep space which released more gamma ray energy at that point than has been calculated to emanate from the entire Universe under a normal state. Because of their similarity to the short-lived, bright supernovae, such events have been termed hypernovae, which produce a least several orders of magnitude more energy (1053 -1054 ergs) than associated with a supernova (~1051 ergs), but they seemingly form by a different mechanism. The initial flare-up may take only a few seconds to actuate but the effects can last for weeks to months. Some hypernovae seem related to Gamma Ray bursts, described below. Hypernovae were most common in the early Universe when very massive stars underwent rapid burning of their hydrogen fuel to heavier elements and finally exploded with fusionable fuel was expended.
In November of 2004, a group of British scientists announced the results of a sophisticated study of a supernova that exploded about 1000 years ago which is shedding new insight into the ubiquitous cosmic radiation that permeates space. This event is still growing in the region near our Sun so that its effects have been now carefully documented. The detection system is known as H.E.S.S., for High Energy Stereoscopic System. As presently configured, four Chernkov telescopes located in the mountains of Namibia are tied together in an array. Together, these provide high definition of a form of blue-colored radiation (the Cherenkov effect) caused by the cosmic rays interacting with atoms in the upper atmosphere. This supernova has proved to be a major source of very energetic cosmic rays (short wave gamma rays). This strongly suggests the one predominant mechanism for production of such high speed particles is part of the supernova explosion process. Here is a plot of the large area (about twice the diameter of the Moon, but, of course, invisible to the eye) of the expanded radiation field as picked up by the H.E.S.S. observation system:
 
Plot of Cherenkov radiation (a by-product of cosmic radiation exciting gaseous atoms in the Earth's upper atmosphere) detected by the H.E.S.S. array that correlates with the remnants of an expanding supernova.
 

Neutron Stars and Pulsars

The end product of a supernova event associated with stars greater than about 8-10 solar masses is a Neutron star, with such strong internal pressures that neutrons are formed by intense squeezing together of protons and electrons (remember: p + e ---> n); these neutrons are also degenerate. (Degenerate matter describes a condition in which the pressures exerted by the mass [as in a gaseous state] no longer depend on temperature but only on the [high] density reached at this stage; the matter is said to no longer obey the classical laws of physics). During the formation of a neutron star, the prior state star (which may have a core as heavy as iron) develops a degeneration pressure that rises until it is capable of halting further gravity-driven collapse down to a remarkably tiny size.
This class of stars winds up as small objects only a few kilometers wide but containing matter equivalent to 4-5 solar masses. Their densities can exceed 1014 gm/cc (or 107 denser than White Dwarfs). (A feel for this extreme density is gained from this comparison: A volume equivalent to a lump of sugar would contain 100 million metric tons [as measured on Earth] of neutron star matter.) These stars can be detected by telescopes that gather gamma-ray, x-ray, and radio radiation. Obviously, being of such small size neutron stars are very hard to find by optical telescope, even though they can glow with intense radiance, unless they are very near to Earth within the M.W. galaxy. The HST has now provided the first-ever look in visible light, shown below, coming a Neutron star. It is shining just in front of a nebular dust mass whose distance is just 400 light years away. (The light is produced by processes involving photon escape from a surface whose temperature exceeds 10000°K; the surface area is quite small in keeping with the miniscule size of the star.) The size of this object has been estimated to be only 28 km (16.8 miles) making it the second smallest intrinsically radiating object beyond our Solar System discovered to date by visual means.
 
A tiny neutron star (arrow), the first ever detected by the HST.
 
The XMM-Newton satellite has produced a strong image of a neutron star just 500 light years beyond the Solar System, as shown here:
 
Geminga, a nearby neutron star that is the second brightest source of gamma rays in the sky.
This smallest imaged star, Geminga, is about 20 km (12 miles) in diameter and has a mass 1.5 times that of the Sun. It rotates at a speed of 4 revolutions per second. Its hot surface exudes strong x-rays and gamma rays, some extending out as filaments (tails), being driven by its huge magnetic field. Electrons and positrons are also a part of the filament, part of the electric field built by the rotation of the star within its magnetic field. The electrons accelerate outward but some evidence shows that the positrons are coaxed back to the star to settle into hot spots.
Some Neutron stars, called Pulsars, are known to have intense magnetic fields and to emit directional beams of strong pulses, best observed by radio astronomy but also very evident in the X-ray region, in extremely regular intervals (with periods from about 1/1000th of a second to several seconds) whose cyclical nature is related to their (often rapid) rotation; the Earth must lie within the beam's solid angle in order to detect this Pulsar action (the pulses therefore are bursts of radiation from a constant beam detected intermittently from Earth, much like a searchlight's beam, while sweeping continuously, appears to the viewer only when aligned momentarily as it passes through its cycle). This is illustrated by this diagram:
 
Pulsar diagram.
Pulsars are formed by the neutron star's immense gravity pulling gas from supernova debris (most pulsars seem associated with Type II supernovae), such that this gas is accelerated to a third or more of the speed of light (thus approaching relativistic speeds [those near light speed] and "detonates" when it strikes the neutron star surface. The magnetic field tends to funnel the fast-moving gas and particles onto narrow parts of the neutron star's surface which become "hot spots. This releases great quantities of energy extending in the spectrum from radio to x-ray regions. There are thousands of bursts of energy that rise from the surface many times each second giving rise to the periodicity detected by radio telescopes and by x-ray observatories such as Chandra.
One of the pulsars that has been extensively studied lies in the heart of the Crab Nebula which we have examined earlier. It shows the development of a pair of short jets of very hot gases that radiate strongly in the x-ray region of the spectrum.
 
Optical (right) and X-ray (left) images of the Crab pulsar.
This pulsar is shown as a close-up enlargement:
 
The Crab pulsar colored orange in this rendition.
There is a very strong pulsar in the Vega constellation. Here is a Chandra view of this feature, expanded in an inset:
 
A pulsar (bright yellow ball) in x-ray excited gases in the Vega constellation
And once again, as seen in more detail.
 
Enlargement of the Vega pulsar, with its second arcuate shock wave excitation in the x-ray region.
The jet (about 0.5 light years in length) around the Vega pulsar continually shifts its position and shape, as monitored over many months by Chandra. This bespeaks of a significant variation in the configuration of its driving magnetic field.
 
Four views on different dates of one of the pulsar jets around the Vega pulsar; Chandra image.
Pulsars can be irregular in shape (mainly the result of x-ray excited gas around the central neutron star. This is evident in PSR B1509-38
 
A pulsar with irregular surrounding gas and a less well developed pair of directed beams.
Here is an X-ray image of the pulsar 3C58 as observed by the Chandra Observatory. It's initiating supernova event was first observed in 1158 A.D. The neutron star at the center of the pulsar source is rotating at 15 times a second. Its radiation excites the cloud of particles surrounding it.
 
The pulsar 3C58.
Some pulsars leave a distinctive trail of excited particles behind them, resembling patterns seen in wind tunnel experiments. These are, in fact, dubbed "Wind Pulsars". The best documented example so faar is the Mouse Pulsar, moving at a speed of 1.3 million mph through space. This image combines data from Chandra and a radio telescope:/p>
 
The Mouse Pulsar.
Most neutron stars have very strong magnetic fields up to 1012 gauss (a normal star's field has a strength of around 100 gauss). A rare subclass of neutron stars (only 10 have been found so far) is called a Magnetar, or more formally, an AXP (Anomalous X-ray Pulsar). An AXP has a magnetic field measuring around 1014 Gauss (the current record holder, at 1015 Gauss, is SGR 1806-20, about 1000 times greater than a typical neutron star and a million billion times that of the Sun's 5 Gauss. A magnetar is similar to an SGR (Soft Gamma-ray Repeaters), another neutron star variant that undergoes periodic variations in energy output. Both AXPs and SGRs are detected by their pronounced X-ray signals. The Rossi Explorer satellite is used to study neutron stars. One magnetar, N 39, has been imaged by the HST and appears in the visible as a collection of filamentous strands formed from shock waves released when a giant star exploded some thousands of years ago.
 
A Magmetar pulsar, N 39, a strong x-ray and gamma-ray emitting neutron star (8 second spin rate), with its nebular material arranged in strands; shown here is the HST visible-near IR image.
 

Black Holes and Quasars

As seen in the star evolution diagram on page 20-5, when gases and other matter of 50 or greater solar masses gravitationally contract into small, compact bodies, the result is a Black Hole (B.H.), so called because the gravity associated with its extremely dense mass (for the mass in our Sun, collapse into a Black Hole would yield a density of about 1022 grams per cubic meter; larger stars would produce densities several orders of magnitude greater) prevents all detectable radiation from within from escaping beyond its event horizon (sphere of influence). The distance from a B.H.'s center to the horizon is known as the Schwartzchild radius . Since the B.H. is itself invisible (black), its existence must usually be inferred from its gravitational effect on surrounding stars and interstellar matter. Before their observational discovery, Black Holes were predicated to exist from General Relativity considerations. A Black Hole generally is so small that its spacetime expression produces a curvature so pronounced that all internal energy and radiation is seemingly trapped beneath the B.H. (within its horizon).
An exception may be Hawking radiation (named after Stephen Hawking who devised the theory) consisting of particles created by quantum processes and driven by the gravitational energy within and around the Hole. The mechanism by which this process takes place is an excellent example of "quantum weirdness". In the 'empty' space just outside the B.H.'s event horizon, virtual particles and antiparticles are constantly created (as happens in general in this environment throughout the Universe. Under the strong gravity field around the B.H., one of these particles, the one with positive energy, is likely to be propelled away while the other is captured and dragged into the B.H. Antiparticles have negative energy and those brought into the B.H. react with B.H. particles to reduce the mass of the Hole and thereby lower its gravitational field. This B.H. gravitational field, in turn, loses the energy it provided to make the virtual pair. The escaping particles constitute the Hawking radiation, which is too "faint" to be detected from Earth but nevertheless causes the B.H to slowly "evaporate".
This escaping (emitted) radiation is most effective for tiny Black Holes and provides a means by which they can dissipate over extremely long times through this evaporation. While based on sound theoretical reasoning, Hawking radiation has not yet been directly detected. But if it is proved to exist, it provides a mechanism by which countless numbers of small primordial B.H.'s that formed at the outset of the Universe, because gravity was so intense then, have since vanished. At the present time, astrophysicists are learning more about B.H.'s by computer modeling and simulating their behavior.
Black Holes are also capable of ejecting matter in jets or streams of particles moving in beams almost at the speed of light. (Jets also occur during star formation and during late stages of star death). Here is an HST view of the well-known galaxy, M87, in which its billions of stars are not resolved so as to appear as a yellow glow. The central "star" is actually light emitted from the exterior around a B.H., probably as a quasar (third paragraph below).
 
Jet of high speed luminous particles from a central Black Hole in the M87 galaxy.
Below are three more views of the jet streamer from M87; the top is imaged by Chandra in the X-ray region; the center is visible light; and the bottom from radio waves. The origin of such streamers, found also associated with other galaxies, is still imperfectly known. But, the Black Hole(s) causing this ejection of gas and particles are the source of strong, directional electromagnetic fields. The gases may be excited by synchrotron radiation, causing the radiation that extends over most of the electromagnetic spectrum.
 
A long jet of particles and gas emanating from the galaxy M-87.
Still another example of a jet associated with the presumed central black hole in a galaxy is Centaurus A (NGC5128) located some 11 million l.y. from Earth. On one side the jet is obvious but it has a faint companion on the other side. This jet pair lines up with the axis of rotation of the galaxy. The image, made by Chandra, is converted to a visible view using data sensed in the x-ray region of the spectrum:
 
Jet(s) associated with the Centaurus A galaxy; Chandra x-ray image.
This jet, which follows magnetic lines, is even more splendidly displayed with an HST image is combined with a Chandra image, as shown below, with the strongest x-ray signals shown in blue:
 
Composite HST-Chandra images displaying the Centaurus-A jet, emanating from a Black Hole.
Probably the best image to date of a paired jet associated with a supermassive Black Hole is that recently captured by HST as it trained on Quasar 3C120; the jet, composed of x-rays and electrons, follows strong magnetic lines:
 
Jets emanating from the quasar ring 3C120.
These jets may be the same phenomena commonly detected by radio astronomy, as illustrated near the bottom of page 20-3.
Galaxies are thought to have multiple Black Holes, most of which are relatively small. Evidence is growing that most spiral galaxies, at least, have one or more Black Holes in their central regions. Such B.H.'s seem to serve as a stabilizing influence on the evolution of a galaxy, causing stars and stellar gas and dust to migrate inward and be dragged into the Hole. The first case in which two supermassive B.H.'s occur in the central core of a galaxy has been found in NGC6240. This irregular galaxy is shown in visible light in the left HST image below; the Chandra image on the right indicates a pair of Black Holes, which create a strong x-ray signal (in blue; weaker x-rays in red and yellow) as infalling material is heated to very high temperatures. Astronomers predict that these B.H.'s will eventually merge by collision.
 
 Chandra X-ray satellite image, with a pair of Black Holes at the centers of the blue high intensity X-ray emissions.
The amount of gas and dust surrounding a central black hole can be much greater than farther out in a galaxy. In NGC 1068 (also known as Messier 77), the HST image on the left of this next figure shows reflected light from the dust in blue, ionized Oxygen gas in yellow, and ionized Hydrogen gas in red; on the right is a Chandra image of its center in which the orange-red corresponds to highly energized material around the immediate B.H. that is emitting x-rays.
 
HST and Chandra images of NGC 1068
Chandra has now established that the central region of the Milky Way galaxy has a moderate-sized Black Hole (located in the celestial hemisphere at a point close to Sagittarius A); perhaps there is more than one in this inner part. The image below shows not the invisible hole itself, but the radiation emitted from excitation of gases and other matter drawn into the B.H. During this continuous exposure over 164 hours, the glowing gases underwent periodic flare-ups that combine in this composite pattern:
 
The effects of the Black Hole at the center of the Milky Way, causing excitation of gases to temperatures at which strong x-rays are emitted and detected by Chandra.
The size of M.W.'s Black Hole has been hard to determine because of this masking matter. It mass has been estimated to be about 3.2 to 4 million solar masses. Early estimates placed the diamter of a sphere to its event horizon at about 23 million kilometers (14 million miles). Recently, studies done by penetrating radio waves, using radio telescopes, has shed light on its dimensions, summarized in this diagram:
 
The geometry of the M.W. central Black Hole, using radio wave data.Courtest Space.com.
The radio wave results have changed this size to about 300 million kilometers (186 million miles)(for reference, recall that the M.W. center is about 26 l.y. from Earth). This may not actually pin down the more meaningful event horizon size, here referred to as the Black Hole shadow; the radio wave horizon may measure the outer extent of excited matter associated with the Black Hole. The shadow size may eventually be determined using gravitational lensing effects extractable from a Very Long Baseline Array of radio telescopes.
In principle, Black Holes should sometimes collide (but the consequences are not yet defined theoretically), especially when two galaxies collide with the B.H's at their centers then interacting. Evidence for this is sparse. However, such an event is postulated for the observations by the Wide Field Camera on HST of NGC326. In the main view below is the pattern of jet lobes from that galaxy seen a few years ago. In the offset second image is a more recent observation in which the orientation of the principal jets has now shifted more than 90°. The favored explanation is that two Black Holes have now interacted causing the spin axis of one to shift notably.
 
A rapid change in orientation of jets from galaxy(ies) NGC326, possible caused by two central Black Holes colliding.
A Black Hole's incredible gravity pulls in particles from outside the event horizon until their velocities are accelerated to nearly the speed of light. Matter is literally torn apart upon entering the Black Hole. As these particles close in, monstrous energy releases produce continuous bursts of energy outside the horizon, a process believed responsible for most Quasars (a contractive term for "quasi-stellar" to describe a star-like appearance even though the observed feature is not a single star). Quasars are extremely bright objects (very high luminosity, comparable or even exceeding that of an entire typical galaxy), being considered by most astronomers to be the glow of radiation bursts ("hot spots" of gamma radiation, x-rays and visible light) from both stellar and interstellar matter continuously infalling into the central regions of active galaxies, whose cores are probably supermassive Black Holes. While the majority of quasars are located at or near a galaxy center, some occur in the spiral galaxy arms or in the regions beyond an elliptical galaxy's core. They were initially discovered as intense radio wave sources detected by radio telescopes. Now it is known that most quasars are not accompanied by radio waves (less than 2% are dominantly radio sources, in which that wavelength region marks energy developed by synchrotron radiation) but are instead sources of more intense, shorter wavelength radiation. Here is an optical image of one (and possibly several) quasar(s) acquired by the HST:
 
Quasar PKS 2349, imaged by the Wide Field Camera on HST.
And here is a very bright central core of a Seyfert Galaxy, NGC 3516, with a quasar producing a huge light emission (but probably being "intensified" by gravitational lensing) associated with infall to a massive Black Hole:
 
The very luminous central core of Seyfert Galaxy NGC 3516; HST image.
A quasar in M1000, as imaged from variations in x-radiation monitored by the Chandra X-ray Observatory, appears thusly:
 
A quasar in galaxy M1000, with density-slice levels of x-radiation as picked up by the Chandra X-Ray Observatory.
A quasar with an associated Black Hole seems to be pulling in material from regions beyond. Quasar HE 1013-2136 at a distance of 10 billion l.y., imaged by an ESO telescope on a Chilean mountaintop, seems to be drawing gases from a galaxy to the left:
 
Quasar HE 1013.
This pair of images shows a quasar in visible (bright in the blue) and infra-red light.
 
Visible and infrared images of a quasar.
The powerful quasar qso 1 Zw 1, as seen in the infrared, is also a strong radio source (contours superimposed).
 
Quasar qso 1 Zw 1, imaged in the infrared by the HST; radio contours based on data obtained by the Plateau de Bure radio telescope in the High Alps.
Most quasars are so far away (but some more recent ones are nearby) that light arriving at Earth left the quasar source when the young Universe was only about 1/4 to 1/6 its present size. Thus, most (estimates in excess of 75%) quasars formed early in Universe history and many, particularly the larger ones, have since become either greatly diminished ("dormant", with occasional flare-ups) or are now extinguished in today's time frame. This generalized (smooth) plot of quasar history, both in terms of time since the Big Bang and when the numbers of galaxies relative to the expansion size of the Universe are normalized to 1 (maximum), illustrates these points:
Plot of quasar occurrence in cosmic time and at the stages where the number of galaxies per unit volume of expansion are indicated by the 'relative space density'.
But since Black Holes can still form in young cosmological time, i.e., recently, throughout the Universe, conceivably they are giving rise (usually after only millions of years) to new quasars. Quasars are made visible because of emission of light resulting from energy conversion as stars and interstellar gases are gravitationally sucked into supermassive Black Holes. HST has observed such events, which may be the case in this image of the elliptical galaxy NGC4261, in which the ring seemingly surrounds such a Black Hole.
 
HST image of an apparent Black Hole in the elliptical galaxy NGC4261; the ring is associated with a quasar.

Black Holes that occur outside galaxies, or in a star-sparse region within a galaxy, do not attract enough material to become readily visible by virtue of the excitation of incoming matter. But their presence is often suspected where an x-ray or gammma-ray source is observed without a corresponding visible body. Black Holes can vary in dimensions, the smallest in the general class being much less than a kilometer in diameter but packing mass equivalent to about 3 solar masses. (Theory indicates that mini-Black Holes can be as small as a few centimeters or even microscopic in size.) Humongous B.H.s can contain masses derived from billions of infalling stars and galactic matter, attaining sizes exceeding that of our Solar System. Massive to Supermassive Black Holes may be the customary state at the center of spiral and other galaxy types, having built up from millions stars and other matter converging inward as though moving to a drain. The HST view of NGC7742, a Seyfert type 2 active galaxy, shows a large glowing central region, within which a supermassive Black Hole is postulated. Its bright center probably represents a quiescent quasar state, resulting from energy release when stars spiral past the B.H. horizon into its interior; note the ring of bright hot, largely younger stars beyond and the faint spiral arms further out.
 
HST image of galaxy NGC7742, with an intense broad central region of high luminosity which may be caused by emissions as matter is drawn into a Black Hole.
Recently, Black Holes have been detected in Globular Clusters by analyzing the patterns of movement and velocities of stars that can be resolved in the assemblages making up the clusters. These B.H.'s have estimated masses intermediate between the small isolated ones mentioned above and the Supermassive ones described in the previous paragraph. Although the numbers of points in the following plot relating B.H. mass to stellar assemblage mass are still few, a general trend that fits size to a straight line is evident:
 
Relation between Black Hole mass and the mass of the stellar assemblages (from star clusters to Elliptical galaxies); note that the mass of a Black Hole (a very large number) is nevertheless only about 0.1 of a percent of all the mass in the stellar grouping.
In the early years after first postulated and then discovered, Black Holes were treated almost as a curiosity, without any special importance in the initial phases of the Universe's history. But, with the discovery that most (if not all) galaxies have B.H's in their core, there is a growing belief among astronomers that they are the necessary starting point in the formation of a galaxy, serving as the nucleus or core that attracts the matter that eventually organizes into a galaxy. Recent reports of both observational and theoretical studies now offer two important ideas: 1) both Black Holes and Neutron stars are more abundant in the inner or central part of a galaxy - a fact related to the idea that massive stars tend to form more readily in the core region; and 2) in early cosmological time Black Holes had a definite symbiotic relation to the processes that form and develop galaxies, i.e., massive B.H.'s can serve either as a nucleus for a growing galaxy or at the least aid in gathering matter into organized gas clumps that evolve into primitive galaxies.
Some Black Holes are thought to be the sole surviving remnants of galaxies that have been completely swept into them. Other Black Holes may have formed during the first seconds of the Big Bang. There are increasing indications that supermassive Black Holes were in existence within the first billion years of the Universe. Many of these are either relics of the B.B. or remnants of early supernovae. In some respects, Black Holes are an approximation to the supersingularity postulated as the starting point of the Big Bang except that they have finite dimensions of meters to several kilometers and even much larger for those in galactic centers depending on their amounts of mass (can be equivalent to the cumulate mass of hundreds of millions to billions of Suns). One theoretical class of Black Holes represent extreme densities concentrated in "points" as small as 10-15 meters.
Speculatively, one future outcome for the Universe (depending on the ultimate mode of expansion [see page 20-8]), after 50 b.y. or so, could be a collection of billions of Black Holes that eventually converge upon themselves to coalesce into a single ultra-dense Black Hole that ultimately would become the singularity for the next Universe (in this model, any number of successive Universes, exploding and contracting cyclically, is feasible). Such a concept of repeating Universes (treated in more detail on page 20-10) is referred to as the "Big Crunch", or even more colloquially, as the "Bounce" in reference to the repetition of an explosion after total collapse to the B.H. singularity.
 

Gamma Ray Bursts

Black holes almost certainly play a role in what are called Gamma Ray Bursts (GRB). These are the most intense and copious releases of energy observed in the Universe - less than that of the Big Bang itself but much more than given out by supernovae or quasars. GRBs can at their outset release enough energy to give them a luminosity calculated to be 1019 greater than that of the Sun. They are characterized by extreme outputs over very brief periods, measured in seconds to minutes at their peak. At least one GRB is observed each day somewhere in the Universe, so they are rather common events, albeit less frequent than supernovae.
Despite being the largest rapid release high energy events in the Cosmos, GRBs were unknown (sometimes mistaken for ordinary supernovae) before 1967. The manner in which they were discovered is an interesting example of serendipity: Nuclear explosions on Earth release large quantities of gamma ray energy. In the 1960s, the U.S. was seeking ways to detect Soviet nuclear tests, so it built and orbited gamma ray, x-ray, and neutron detectors on military satellites. In the U.S. Air Force Vela program, the Vela-4 satellite detected many gamma ray events, all at times that failed to correlate with any known nuclear blasts on Earth. These gamma ray events were all proved (eventually) to emanate from well beyond Earth. Here is a plot of one of the first records:
 
Energy (counts per second)-time diagram of a detected gamma ray event recorded from a military (Vela program) satellite.
GRBs give off tremendous amounts of energy extending through all wavelengths of the EM spectrum. The diagnostic signature of the GRB that separates it from supernovae is the predominance of high energy gamma rays over very short time periods. GBRs can be subdivided into two types: short burst (around 2 seconds) and long burst (more 2 seconds; initial emissions on the order of 20-30 seconds, with a few extending up to an hour). This time spike has been observed in GRBs detected by more sophisticated sensors that monitored such events. Thus, this example:
 
Energy-time plot for a 1991 GRB event.
These GRBs puzzled astrophysicists. They were first thought to be in the Milky Way. And in fact some were actually located in our galaxy, where they occur on average about once in 10000 years. Afterglow radiation from one such event was observed on February 28, 1997 in the M.W. itself by an Italian X-ray satellite called BeppoSAX:
 
A GRB afterglow associated with an event in the Milky Way, imaged at X-ray wavelength by BeppoSAX.
But, the frequency of occurrence, which as more observations were confirmed indicates at least one GRB every day, suggested that the vast majority of GRBs were located in galaxies well beyond the Milky Way. As more records of these events accumulated, it became evident that GRBs are not concentrated in specific regions of the sky but are distributed at random (isotropic) over the entire sky. GRB's are also randomly distributed in time - occurring anywhere in the Universe (thus over the full extent of time since the first galaxies;(from thousands of light years to 12+ billion l.y.). A large number seem to be distant, near the outer part of the observed Universe, and hence were most common in the early history of the Universe. Here is a map of the sky showing many of the larger GRBs, as detected by the Compton Gamma Ray Observer and BeppoSAX.
 
Full Sky distibution of up to 800 GRBs; larger ones shown as blotches
The BATSE (Burst and Transient Source Experiment) instrument on the Compton Gamma Ray Observatory (CGRO; see page 20-3) was particularly suited to detecting GRBs. Here is one image of an event that occurred several billion light years away:
 
A CGRO BATSE image of GRB980329 that was monitored on April 17, 1997; its peak output lasted 8 seconds.
These GRB events should generate radiation at wavelengths longer than those of gamma rays. As studies of them expanded, traces of individual events were sought by other satellites that monitor at different wavelengths. The problem is that evidence of a GRB diminishes rapidly at shorter wavelengths. However, in time such events were picked up at various wavelengths when alerts were given and the sky locations established. Now, with experience this is the time frame for durations of GRBs over a range of wavelengths:
 
Duration of detectable radiation from a GRB at different wavelengths.
These signs of lower levels of energy at longer wavelengths persisting around a GRB are grouped under the general term "afterglow". X-rays proved useful as GRB signatures provided the searching satellite(s) could check out the source region within a few days. The x-ray emissions persist over periods of hours to days. This is one X-ray image of a presumptive GRB that was located in a galaxy nearby (some has classified this as a hypernova):
 
A hypernova (= GRB ?) event imaged by x-radiation picked up by the Einstein Observatory.
Images acquired by BeppoSAX were especially helpful in the sky survey for GRBs. The top illustration consists of two intensity contoured images typical of X-ray renditions; note the reduction in intensity in just four days between February 28 and March 3. Below it is a pair of BeppoSAX images taken first on December 15, showing the GRB as a bright dot and then on December 16 as the afterglow had faded away.
 
BeppoSAX image pair of X-ray signals from a GRB.
 
Images taken a day apart of a GRB, in which x-radiation monitored by BeppoSAX is rendered like a visible image.
Special attention was given to finding GRBs at visible (optical) wavelengths, since these are especially capable of measuring red shifts by which approximate distance to the source can be estimated. About half the GRBs give off light in the visible for durations of a week or more. The HST and the Keck Observatory in Hawaii were pointed at targets reported by other observing satellites. Here is the HST image of event GRB000301c.
 
Optical image of GRB000301c made by the HST.
A ground telescope imaging of another GRB shows the burst as seen in visible light (here the print is a negative) at 21 hours (left) and 8 days (right) after first detection. The rapid fading of the galaxy-sized feature is evident (note arrows)
 
Photo made through the La Palma telescope of a GRB (arrows) at approximately 1 and 8 days after burst.
Although not used a lot for this purpose, radio telescopes have detected and imaged GRBs. Here is one made by the VLA group:
 
VLA radio wavelength image of GRB980329.
One very important GRB event led to some intriguing information that indicates that this phenomenon occurred much more often early in cosmic time (but continues til the present) and helps to confirm the huge amounts of energy involved. Its magnitude is equivalent to 100 million billion solar radiances. On December 14, 1997 the CGRO registered this event. Word was sent to BeppoSAX operators and to the HST and Keck telescopes to look for it as rapidly as possible. All succeeded. This is how the event was imaged by the HST:
 
HST�s optical image showing a huge outburst of gamma rays from a possible hypernova; over a month�s time the output dropped significantly (left).
The image on the right was taken on January 23, 1999 during its maximum. By February 8 (left) this burst (shown at a different scale, in the box) had faded to 1/4 millionth of the visible output.
When a redshift distance measurement was made on the GRB, it was found to be some 12 billion light years from Earth, proving the surmise that GRBs have probably been part of the Universe's history since soon after the Big Bang. It was also the brightest object yet found at that far distance from Earth.
Thus, the pattern found for most GRB events is rapid emission of gamma rays followed, as they fade, by the dominant radiation passing through x-ray, visible, and radio wavelengths, with the whole sequence being over in less than a few months.
GRBs are of such high interest that another dedicated satellite has been placed in orbit to look for these and similar events. This is HETE-2, the High Energy Transient Explorer, launched October 9, 2000 (the first HETE failed to separate from its third stage rocket). It is described at this MIT site. One of its most important discoveries is described four paragraphs down.
The cause(s) of GRBs continues to be uncertain and tantalizing. As an aid to the following discussion, use this Fireball Model to provide a framework for the starting energy, the expansion of the GRB, and the time involved in reaching the afterglow phase:
 
A model for GRB expansion.
 
The early idea of the explosion of material sucked in and around a neutron star (see top illustration on this page for a similar example) has been challenged. But, a variant postulates a role for a binary pair of neutron stars which, if they should collide, produce a huge release of energy. Still others attribute the GRBs to some involvement with quasars. One school holds them to be the outcome of giant supernovae (hypernovae) which generate the most powerful short-time energy release levels known in the Universe. A recent hypothesis takes still a new tack - the GRBs are associated with large clusters of galaxies which together have such a strong gravitational pull that they accelerate matter both within and around the galaxies to high speeds that, upon colliding with intergalactic matter, release energy at the gamma-ray level.
Another hypothesis, known as the Paczynski Model (also known as a collapsar event) and now the most favored explanation, starts with a supermassive (type O) rotating star that collapses to form a black hole that continues to draw more material around it until a critical state is reached that requires an intense supernova-like explosion producing the GRB fireball. Essentially, all the mass involved is suddenly converted to energy in obeyance to the Einstein E = mc2relation. There are indications that this energy release may be directed, something like the beam associated with a pulsar. Calculations show that if such a beam generated from a GRB destruction of a neighboring massive star in the Milky Way were to strike the Earth, the intensity would destroy everything at and above the surface - oceans, vegetation, atmosphere, life (fortunately, the probability of this happening, both in terms of star sizes and of directionality of the beam, is considered quite low).
In fact, until the release of information in June 2004 about a GRB only 35000 l.y. away - either in or just outside the M.W. - no nearby events had ever been confirmed. The image below shows W49B as a color composite made from Chandra X-ray data (blue), and Palomar telescope images taken in the IR (green and red). The estimated initial release of energy over a 1 minute time span is 1013 greater than that of the Sun. The image represent the GRB status soon after the burst; the colors indicate enrichment in iron. The postulated beam associated with collapsar events was not oriented straight at the Earth and hence is not visible here.
 
 J. Keohane, JPL
 
Some of the above information has been extracted from an article in the December 2002 edition of Scientific American, entitled "The Brightest Explosions in the Universe", by N. Gehrels, L. Piro, and P. Leonard. The article contains this illustration that summarizes the authors' ideas on the formation of GRBs:
 
Schematic showing the development and brief history of a typical GRB.
From Scientific American, December 2002
In their model, similar to some others proposed, GRBs are definitely associated explosive processes that will end forming black holes. In one common mechanism, a massive star collapses and explodes as a hypernova, leading to a disk of matter/energy surrounding a black hole; this is a fast process in the sense that at a critical time, the hypernova ensues without anything discernible obviously leading up to it. Alternatively, over a long span of time (millions of years, the same end result could occur as two neutron stars mutually orbiting finally crash into each other. The wedge to the right of the 'Central Engine' conforms to a jet that carries the photons released in the GRB outward at near light-speed. This material moves outward as "blobs" that catch-up and coalesce forming internal shock waves that generate the gamma bursts. With expansion over time, the high energy photons are replaced by those of progressively lower energies represented by x-rays, light, and radio waves as the emissions encounter the galactic/intergalactic medium. The final result is an afterglow that fades over time.
On March 29, 2003, HETE-2 captured a GRB (HETE Burst H2652 is also listed as GRB 030329 and SN2003dh) in a galaxy 2.6 billion light years distant and sent the occurrence of this event back to Earth so quickly that many observatories were alerted quick enough to train their telescopes on it within minutes. Thus, for the first time the earliest stages of a GRB could be monitored. This event proved one of the brightest ever observed. This plot of HETE data shows how brief was the main phase of the event.
 
Energy release/time plot for GRB H2652.
A radio telescope image of this GRB taken on April 22 shows a progressive distribution of decreasing energy moving outward. This seems to confirm the "fireball" model for ejection of matter (an alternate explanation, that material is ejected in huge blobs [the "cannonball" model, is apparently not valid for this observation). The expelled material moves at nearly the speed of light.
 
GRB 030329, imaged at radio frequencies, about 24 days after the initial burst of gamma rays.
Spectrographic data showed that the initial burst of H2652 was rich in excited Silicon and Iron. These elements would be produced in a star whose mass is at least 30x that of the Sun, which would give rise to temperatures and pressures that generate nuclear reactions that fuse nuclei into Si and Fe. These are the conditions that favor a "super-supernova", another way of referring to hypernovae. Astronomers believe this is convincing evidence for that mode of generation of many (perhaps most) GRBs.
As knowledge of the roles of the predominant dark matter and dark energy (see pages 20-9 and 20-10) is increasing, another explanation (Louis Clavelli) - somewhat conjectural - has emerged. This holds that dark energy under the right conditions acts upon ordinary matter to convert it to dark matter. From theory, this should give off intense bursts of energy as the conversion proceeds, witnessed by us as GRBs.
The latest space telescope dedicated to GRB detection is NASA's Swift, launched on November 20, 2004. This spacecraft has three detection systems that can be activated within minutes of the one always on that picks up the gamma-radiation. Swift will be capable of finding and monitoring as many as 2 GRBs per week, far more than previous instruments, and will follow the changes to the stage when Black Holes as the end product is reached. Swift also can "see" back to the early days of the Universe out to almost 15 billion light years away. The spacecraft and its three telescopes are shown here:
 
Artist's sketch of Swift; BAT = Burst Alert Telescope; XRT = X-ray Telescope; UVOT = Ultraviolet Optical Telescope
 
In January, 2005 9 GRB events were detected. The first detection was in December, 2004, as shown below as an energy plot and the actual image derived from the data:
Energy plot of the first Swift-detected GRB
 
The bright spot is the GRB; the blue lines are background radiation effects.
 
Swift also peered at the Cassiopeia A (circa 1680 BPE) supernova to test its ability to measure afterglow using the X-ray Telescope;
 
Swift XRT image of the 425 year old GRB in Cassiopeia A, now a wide afterglow.
 
As mentioned above, GRBs are all short-lived, even in human terms, lasting from milliseconds to hundreds of seconds. One very short duration type, which releases much less energy, is known as gamma rays flashes. These have been observed by Swift and by earth-based telescopes. Their cause(s) may be neutron star pair interactions but other mechanisms have not been ruled out. Here are several that occurred simultaneously:
 
Lower energy GRBs, called 'flashes', or 'baby bursts'.
 
Problems with explaining GRBs are compounded by observations (using EGRET, NASA's orbiting Energetic Gamma Ray Experiment Telescope, part of the Compton X-ray Observatory) of about 170 sources of continuously emitting high energy gamma rays. Thus, these do not display short-lived bursts. This class was first discovered by the Compton Gamma Ray Observatory (page 20-3). They may be associated with clumps of supersymmetric particles (page 20-1) including a type called the neutralino.
Needless to say, GRBs continue to fascinate cosmologists since they represent the largest and fastest explosive events beyond that of the Big Bang itself. As they are better understood, they may reveal the action of physical processes only now being speculated upon, and suggested by particle physics experiments. The next big step in studying GRBs and the continuous types will be the launch of GLAST (Gamma-ray Large Area Space Telescope), perhaps as early as 2007.
 

Colliding Stars

At least some of the GRBs and X-Ray bursts may stem from collisions of (usually two) stars (check back at the bottom of page 20-3 for the earlier review of galaxy collisions). As recently as the 1970s astronomers considered collisions to be rare stellar events. Although an actual collision has as yet not be observed by HST or other astronomical satellites and ground telescopes, phenomena associated with certain stellar configurations have now been postulated (attributed) to either head-on or glancing encounters between stars.
As we have seen, stars in the arms of spiral galaxies or the fringes of elliptical galaxies are very widely spaced and hence the probability of collision is low. But star distributions in central cores of these two types show much closer spacing (denser). Even higher densities are found in globular clusters, such as 47 Tucanae:
 
The Globular Cluster 47 Tucanae, one of about 150 in the halo region of the Milky Way.
To appreciate the significant increase in density, if one counts the stars that are about 25 light years from our Sun, the number would be about 100 but if the same 25 l.y. volume is set around the center of a globular cluster, that star number rises to an order of about 1,000,000. This crowding means that those stars are very closely packed and hence capable of numerous collisions. Three processes make collisions much more likely: 1) a process called "evaporation", in which stars approach other and some are then flinged out of the grouping which contracts to such densities as to make collisions inevitable; 2) gravitational focusing, in which approaching stars have their pathways deflected so that two stars now follow a collision course; 3) tidal capture, in which neutron stars or black holes latch onto nearby stars and in time draw these into the high gravity
Theoreticians have developed computer models to simulate pictorially different modes of collision. Shown here is the sequence of change as two Sunlike stars are merged:
 
Simulated sequence showing the stages of collision of two stars of similar size.
The end result of a collision depends on several factors: 1) whether there is a direct hit or a glancing encounter; 2) the relative size (mass) difference between colliding bodies; 3) the terminal speed of each body. The process can be as brief as an hour; or as long as days to years (this rapid time for completion is one reason while such events have yet to be observed in "real time"). Any two of the 7 density types shown near the top of page 20-5 can experience a collision. In some combinations, such as a white dwarf striking a red giant, the end result is two White Dwarfs (one being the incoming member; the other [Red Giant] dispersing and losing so much of its gas by the interaction that only its core remain which quickly evolves into the new White Dwarf, Or, one star remains relatively intact as the second star is incorporated within it.
In this last case, the result is that the now coalesced star pair has gained considerable mass. This means that it now appears to be a bigger star, and since the total mass determines the rate of hydrogen fuel consumption, the new, brighter star would appear as though it will burn its hydrogen mass much faster and thus appears to have a shorter lifetime - hence seems younger. A specific case: if two stars, each with a mass of the Sun (5 billion years old) that has a total burn out time of 10 billion years, collide and form a single star with twice the mass, the now more luminous composite star would have a life expectancy of 800 million years. This seems to be the best explanation of "Blue Straggler" stars - much brighter than the majority of stars in a globular cluster. This is evident in this HST image of NGC 6397:
 
Large blue stars in globular cluster NGC6397.
An excellent summary of collision processes and consequences is offered in the November 2002 edition of Scientific American under the title "When Stars Collide", by Michael Sharma.
 
 
 


 
 
 

 
 
 
 

 

 
 

 
 
 
 

 

 

 
 
 
 

 

 
 
 
 
 

 

 
 
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Primary Author: Nicholas M. Short, Sr. email: nmshort@ptd.net


 http://www.fas.org/irp/imint/docs/rst/Sect20/A6.html

 

 

 

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