Taking a ringside seat for a gamma-ray burst
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Taking a ringside seat
for a gamma-ray burst
for a gamma-ray burst
Supercomputers simulate inner workings
of one theory for the cause of bursts
of one theory for the cause of bursts
Nov. 3, 1999: Supercomputers are being used to take the human mind on a voyage that no space probe can ever take, to a ringside seat near the center of a dying star in the minutes before it becomes a gamma-ray burst that is seen across the universe.
Right: A simple animation covering 27 seconds in the birth of a collapsar. Credit: Woosley, UC Santa Cruz
This virtual seat really is ringside because it places the astrophysicist just outside a swirling accretion disk of matter surrounding the birth of a black hole. And all around, the star is preparing itself for a most spectacular light show.
Welcome to collapsar, the collapsing star scenario that is one of the leading contenders as the cause of gamma-ray bursts.
The collapsar theory was proposed in 1993 by Dr. Stan Woosley of the University of California at Santa Cruz. Since 1996 his work on the collapsar has been done jointly with a UC Santa Cruz graduate student, Andrew MacFadyen. In particular, the multi-dimensional graphics shown here are from MacFadyen's thesis.
Woosley has been well established in astrophysics owing to his work for the last 20 years on the evolution and explosion of massive stars. He reviewed and discussed his concept Oct. 21 during the theory session of the Fifth Biennial Huntsville Gamma Ray Burst Symposium.
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"We shouldn't try to explain everything with one model," he said. "We should push the model as far as possible, but not be surprised that the universe has more going on than just one answer."
Still, the collapsar is an extremely attractive model that fits a wide range of observed gamma-ray bursts. A key requirement for any burst model is how to produce an immense amount of energy in a few seconds.
Before the Burst and Transient Source Experiment aboard the Compton Gamma Ray Observatory piled up evidence that bursts are quite distant, it was possible to build a burst model that only shed modest amounts of energy. But observations of optical and other counterparts since the famous Feb. 28, 1997, burst (GRB 970228) have established that bursts are near the edge of the observable universe.
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The total energy of 1054 ergs assumes the burst is not beamed but is isotropic or evenly distributed, MacFayden explained. But if the energy is beamed by the jets erupting from the poles, then the burst requires "only" 1 percent as much power, 1052 ergs (or, a mere 10 times as much as our sun will generate in its entire life), and only 1 percent of the sky will be illuminated by the blast. This also implies that bursts are 100 times more common than we detect because only 1 burst in 100 will be pointed at Earth.
Left: Hubble Space Telescope image of GRB 970228, the first one for which an optical counterpart was spotted (by the Dutch-Italian Beppo-SAX satellite) shows the burst source apparently associated with a faint galaxy about 12 billion light years away. Credit: Space Telescope Science Institute.
Either way, the energy requirerments help select which models survive.
"The models these days, because of the energy numbers, involve gravitational collapse," Woosley said. Another leading theory is the merger of two neutron stars (sometimes written n*+n*), or a neutron star and a black hole (n*+BH), as they revolve around each other. But it has some shortfalls that the collapsar easily satisfies, Woosley said. The chief argument against merging n*+n* and n*+BH right now is that the event should take place far outside galaxies because they are born with high velocities that would take them outside the galaxy before their orbits decayed to allow merger. So far, most optical counterparts for bursts have been associated with faint galaxies.
But he also cautioned that "even this simple model can get you into a lot of complexity."
Stars can take several different routes to oblivion as they fuse the last of the hydrogen in their cores. Our sun will expand to a red giant then shrink to become a white dwarf that slowly fades away. Stars having 10 to 25 solar masses will go into a series of hotter, faster burn cycles that use the ash of one cycle as fuel for the next. The end products are silicon and, a few hours later, iron and nickel.
The shock that is initially produced following the collapse of the iron core gets its energy from neutrinos (fundamental particles moving at or near the speed of light) emitted by the contracting proto-neutron star which might have a radius of 50 km.
Right: A cross-section from a simulation showing the heart of collapsar where the collapsing star forms an accretion disk (orangle plumes) before swirling into a black hole 3 times more massive than the sun. The scale is in kilometers. Credit: Woosley, UC Santa Cruz
But what happens if the star is a real heavyweight? It fails as a supernova, Woosley contends, and follows either of two paths, prompt or delayed black hole formation.
In the prompt formation case, the shock that usually blows up a supernova fails to be launched. Within a second the neutronized core is converted into a black hole that accretes infalling material thru a disk at about 1/10th of a solar mass per second.
In the delayed formation case, a shock is launched, and is successful in the sense that it never stops moving out and would have made it to the surface of the star, given time. However the shock fails to eject all the star. Enough falls back over about 100 seconds to make a black hole that accretes material through a disk but at about 1/10th of a solar mass per second.
Bursts, and Supernovae, by S. E. Woosley, A. I. MacFadyen,
A. Heger (UC Santa Cruz). Excellent review paper on the subject,
available through the Los Alamos Abstracts Server.|
More images and links on collapsars are available at Andrew MacFayden's web site, including Collapsars - Gamma-Ray Bursts and Explosions in "Failed Supernovae", (MacFadyen & Woosley, Astrophysical Journal 524, 262 (1999)).
Department of Astronomy and Astrophysics at UC Santa Cruz
When stars go hyper Oct. 21, 1998 - Scientists thought they understood supernovae - the death throes of huge, exploding stars. However, a new kind of supernova, far too bright to be an "ordinary" supernova, confounds current theories.
About 100 seconds after the supernova blast wave departed, it returns with a vengeance. That energy has to go somewhere, so the star blows its top - and bottom.
As the avalanche of stellar material forms the black hole, it also tunnels outward along the star's rotational poles at about 1/3rd the speed of light. The star's mass presses back, so the jet forms a sharp cone with an angle of about 20 degrees.
"That gives a very powerful jet," Woosley said. When the jet erupts like a hellish geyser from the star's poles, the geyser quickly envelopes the whole star with a shock wave that rips the star apart.
From that point the collapsar becomes a "relativistic fireball" with material hurled nearly at the speed of light into the solar wind the star had been blowing off until a few minutes ago and then into the interstellar medium.
Right: A larger view of the density structure in a model where no jet was initiated, 15.63 s after collapse. The inner disk with its higher density is unresolved here. As an indication of how dense material is around the disk, the "thin" areas along the polar axis are about as dense as the star. The Earth is shown to the same scale. Links to 455x905-pixel, 181KB JPG. Credit: MacFayden and Woosley, UC Santa Cruz (top), NASA/Goddard (bottom).
Woosley admits that the collapsar theory is still a work in progress and depends on conjectures "both reasonable and unproven." Nor does the model yet predict all types of bursts, such as short, fast bursts lasting a few seconds.
Meanwhile, Woosley and his colleagues continue to refine their models in supercomputers with advanced programs that describe the behavior of fluids under extreme conditions. No spacecraft will ever have so good a ringside seat. Never mind getting inside a star. Gamma-ray bursts appear to be a creature of the past, occurring early in the universe when it was easier to make supermassive stars. Bursts, as we see them today, are from the cosmic fossil record.
So, like the creatures of Jurrasic Park,the inner workings of gamma-ray bursts - be it collapsars or some other model - will be something we can view only through the eyes of a computer.1999 GRB Symposium series
Nov 2: Taking a ringside seat for a gamma-ray burst Supercomputers are giving scientists a ringside seat for one of the most violent events in nature, the heart of a gamma ray burst. The "collapsar" model simulates a star that is too heavy to go supernova, and thus turns itself inside out.
Oct 29: A Swift Look at the Biggest Explosions in the Universe Spurred by the thousands of gamma-ray bursts recorded over the last three decades, NASA is planning missions dedicated to discovering the causes of what had been an oddity and now has become a primary mystery.
Oct 25: Postmortems in the Sky To say they are ghoulish may be going too far, but like ghouls those studying Gamma Ray Bursts gleefully seek the moldering remains, and never see the living victim. But they are very much interested in both the victim and the cause.
Oct 21: Dodging pitfalls in the hunt for the cause of gamma-ray bursts Scientists discuss how to avoid making mistakes while searching for the solution to a big astrophysical mystery - What causes gamma-ray bursts?
Oct 20: Outbursts Result in Controversy Scientists have different ideas to explain the behavior of Soft Gamma Repeaters (SGRs).
Oct 18: After three decades of study, gamma-ray bursts still mystify Science@NASA caught up with Dr. Gerald Fishman for an interview about bursts and the symposium.
Oct 11: Gamma-ray bursts to take center stage at international meeting More than 200 astronomers will gather to talk about gamma-ray bursts, one of the most mysterious and increasingly watched-for phenomena in the universe.
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|Author: Dave Dooling|
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