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Violently Variable Black Holes Probed

Date:
October 15, 2008
Source:
European Southern Observatory - ESO
Summary:
Unique observations of the flickering light from the surroundings of two black holes provide new insights into the colossal energy that flows at their hearts. By mapping out how well the variations in visible light match those in X-rays on very short timescales, astronomers have shown that magnetic fields must play a crucial role in the way black holes swallow matter.

Artist's impression of the black holes studied by the astronomers, using ULTRACAM attached to ESO's Very Large Telescope. The systems -- designated Swift J1753.5-0127 and GX 339-4 -- each contain a black hole and a normal star separated by a few million kilometres. That's less than 10 percent of the distance between Mercury and our Sun. Because the two objects are so close to each other, a stream of matter spills from the normal star toward the black hole and forms a disc of hot gas around it. As matter collides in this so-called accretion disc, it heats up to millions of degrees. Near the black hole, intense magnetic fields in the disc accelerate some of this hot gas into tight jets that flow in opposite directions away from the black hole. The orbital period of Swift J1753.5-0127 -- just 3.2 hours -- is the fastest found for a black hole. The orbital period of GX 339-4, by contrast, is about 1.7 days.
Credit: ESO/L. Calηada

Unique observations of the flickering light from the surroundings of two black holes provide new insights into the colossal energy that flows at their hearts. By mapping out how well the variations in visible light match those in X-rays on very short timescales, astronomers have shown that magnetic fields must play a crucial role in the way black holes swallow matter.

Like the flame from a candle, light coming from the surroundings of a black hole is not constant — it flares, sputters and sparkles. "The rapid flickering of light from a black hole is most commonly observed at X-ray wavelengths," says Poshak Gandhi, who led the international team that reports these results. "This new study is one of only a handful to date that also explore the fast variations in visible light, and, most importantly how these fluctuations relate to those in X-rays."

The observations tracked the shimmering of the black holes simultaneously using two different instruments, one on the ground and one in space. The X-ray data were taken using NASA's Rossi X-ray Timing Explorer satellite. The visible light was collected with the high speed camera ULTRACAM, a visiting instrument at ESO's Very Large Telescope (VLT), recording up to 20 images a second. ULTRACAM was developed by team members Vik Dhillon and Tom Marsh. "These are among the fastest observations of a black hole ever obtained with a large optical telescope," says Dhillon.

To their surprise, astronomers discovered that the brightness fluctuations in the visible light were even more rapid than those seen in X-rays. In addition, the visible-light and X-ray variations were found not to be simultaneous, but to follow a repeated and remarkable pattern: just before an X-ray flare the visible light dims, and then surges to a bright flash for a tiny fraction of a second before rapidly decreasing again.

None of this radiation emerges directly from the black hole, but from the intense energy flows of electrically charged matter in its vicinity. The environment of a black hole is constantly being reshaped by a riotous mκlιe of strong and competing forces such as gravity, magnetism and explosive pressure. As a result, light emitted by the hot flows of matter varies in brightness in a muddled and haphazard way. "But the pattern found in this new study possesses a stable structure that stands out amidst an otherwise chaotic variability, and so, it can yield vital clues about the dominant underlying physical processes in action," says team member Andy Fabian.

The visible-light emission from the neighbourhoods of black holes was widely thought to be a secondary effect, with a primary X-ray outburst illuminating the surrounding gas that subsequently shone in the visible range. But if this were so, any visible-light variations would lag behind the X-ray variability, and would be much slower to peak and fade away. "The rapid visible-light flickering now discovered immediately rules out this scenario for both systems studied," asserts Gandhi. "Instead the variations in the X-ray and visible light output must have some common origin, and one very close to the black hole itself."

Strong magnetic fields represent the best candidate for the dominant physical process. Acting as a reservoir, they can soak up the energy released close to the black hole, storing it until it can be discharged either as hot (multi-million degree) X-ray emitting plasma, or as streams of charged particles travelling at close to the speed of light. The division of energy into these two components can result in the characteristic pattern of X-ray and visible-light variability.


Story Source:

The above story is based on materials provided by European Southern Observatory - ESO. Note: Materials may be edited for content and length.


Journal References:

  1. Gandhi et al. Rapid optical and X-ray timing observations of GX 339-4: flux correlations at the onset of a low/hard state. Monthly Notices of the Royal Astronomical Society Letters, 2008; 390 (1): L29 DOI: 10.1111/j.1745-3933.2008.00529.x
  2. Durant et al. SWIFT J1753.5-0127: A Surprising Optical/X-Ray Cross-Correlation Function. The Astrophysical Journal, 2008; 682 (1): L45 DOI: 10.1086/590906

Cite This Page:

European Southern Observatory - ESO. "Violently Variable Black Holes Probed." ScienceDaily. ScienceDaily, 15 October 2008. <www.sciencedaily.com/releases/2008/10/081015110838.htm>.
European Southern Observatory - ESO. (2008, October 15). Violently Variable Black Holes Probed. ScienceDaily. Retrieved September 30, 2014 from www.sciencedaily.com/releases/2008/10/081015110838.htm
European Southern Observatory - ESO. "Violently Variable Black Holes Probed." ScienceDaily. www.sciencedaily.com/releases/2008/10/081015110838.htm (accessed September 30, 2014).

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