主要内容:
X射线耀发的等待时间（间隔时间）和光度之间的关系和自组织现象的表现一致。
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| Title: |
| Self-organized criticality in X-ray flares of gamma-ray-burst afterglows |
| Authors: |
| Wang, F. Y.; Dai, Z. G. |
| Affiliation: |
| AA(School
of Astronomy and Space Science, Nanjing University, Nanjing 210093,
China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing
University), Ministry of Education, Nanjing 210093, China), AB(School of
Astronomy and Space Science, Nanjing University, Nanjing 210093, China;
Key Laboratory of Modern Astronomy and Astrophysics (Nanjing
University), Ministry of Education, Nanjing 210093, China) |
| Publication: |
| Nature Physics, Volume 9, Issue 8, pp. 465-467 (2013). |
| Publication Date: |
| 08/2013 |
| Origin: |
| NATURE |
| Abstract Copyright: |
| (c) 2013: Nature Publishing Group |
| DOI: |
| 10.1038/nphys2670 |
| Bibliographic Code: |
| 2013NatPh...9..465W |
Abstract
X-ray flares detected in nearly half of gamma-ray-burst (GRB) afterglows
are one of the most intriguing phenomena in high-energy astrophysics.
All of the observations indicate that the central engines of bursts,
after the gamma-ray emission has ended, still have long periods of
activity, during which energetic explosions eject relativistic
materials, leading to late-time X-ray emission. It is thus expected that
X-ray flares provide important clues as to the nature of the central
engines of GRBs, and more importantly, unveil the physical mechanism of
the flares themselves, which has so far remained mysterious. Here we
report statistical results of X-ray flares of GRBs with known
redshifts,
and show that X-ray flares and solar flares share three statistical
properties: power-law frequency distributions for energies, durations
and waiting times. All of the distributions can be well understood
within the physical framework of a self-organized
criticality (SOC)
system. The statistical properties of X-ray flares of GRBs are similar
to solar flares, and thus both can be attributed to a SOC process. Both
types of flares may be driven by a magnetic reconnection process, but
X-ray flares of GRBs are produced in ultra-strongly magnetized
millisecond pulsars or long-term
hyperaccreting disks around
stellar-mass black holes.
