Avalanche statistics suggest Tabby’s star is near a continuous phase transition
12/20/2016 11:41 AM
Now a team of scientists at the University of Illinois at Urbana-Champaign—physics graduate student Mohammed Sheikh, working with Professors Karin Dahmen and Richard Weaver—proffer an entirely novel solution to the Tabby’s star puzzle. They suggest the luminosity variations may be intrinsic to the star itself.
Tabby’s star is in most regards a standard F-class star, located in the constellation Cygnus, approximately 1,276 light years from Earth. Its unusual light curve—the graph of its light intensity as a function of time—shows intense dimming events of up to 20 percent, punctuated with smaller irregular dimming events.
The Ilinois team applied a statistical analysis to the light curve’s smaller irregular variations. What they found is a mathematical pattern consistent with a well-established avalanche model: the smaller dimming events are the “crackling noise” or small avalanches that are observed during the time intervals between the larger avalanches, equated to the larger dimming events. The small dimming events come in a remarkably broad range of sizes, which are distributed according to a simple scaling law. These results suggest the dimming events may be intrinsic to Tabby’s star and that the star may be near the critical point of an underlying continuous phase transition.
Sheikh performed the calculations for the analysis of the observational data. He explains the mathematical method, which starts by establishing a median dimming threshold across the light curve.
“The threshold is an artifice we resort to in order to define what an avalanche is in the context of the light curve. In fact, the statistics are pretty robust to where we choose the threshold, so the exact value isn't important. What is important is that we get enough avalanches to do statistics. Once the light curve drops below the threshold, we consider such an event the start of an avalanche. While the light curve remains below the threshold the avalanche continues, and it stops when it increases again to a value above the threshold.”
Avalanches have two main properties, size and duration. The size is the total area enclosed by the light curve (underneath the threshold) and the threshold.
The avalanche size,” continues Sheikh, “is related to the net decrease in energy emitted by the star during the dimming event, when compared to a constant emission rate of the star, or the constant threshold value. The avalanche duration is the length of the event. We also look at the power spectral density, which is related to how much power per unit of frequency is contained in the light curve.
“Basically, we are looking at the statistical distributions of the fluctuations. All of these things have power laws associated with them. This gives us an independent way to interpret the events and check consistency with the model.”
Power laws have the interesting feature that they look the same on different scales. So when you zoom in to small scales and short times you get the same types of statistical distributions as when you zoom out to larger scales and longer times. Power laws reflect self-similarity of the system over a wide range of length and time scales—similar to fractals—that look the same when you zoom in or when you zoom out.
Significantly, the statistics of Tabby star’s smaller dimming events are consistent with the predictions of a scaling theory. In her body of research, Dahmen has established that a small-event scaling pattern punctuated by larger events is typical of systems near a phase transition. She has seen this in the intermittent deformation dynamics of nanocrystals, the event statistics of metallic glasses, rocks, and granular materials, and in earthquakes on much larger scales spanning 12 decades in length. Similar types of avalanches are also seen in neuron firing avalanches in the brain, in magnetic systems, and in many other condensed matter systems.
“We know from other systems near nonequilibrium phase transitions that a system can have small events that show power law scaling and large events that have different dynamics,” Dahmen explains. “Examples of such transitions are magnetic systems that are slowly driven with a magnetic field, or the slow deformation of somewhat brittle materials where there is often first little crackling that gets louder and louder until there is a big snap when the material breaks.”
“The small events in our star analysis would be like the little crackles while the large events would be the analogue of the big snap,” she continues. “Our mean field model is actually able to account for both, small events and large ones. It has a built in ‘weakening’ mechanism that explains why there should be two types of avalanches.”
If the dimming events are associated with an oncoming phase transition, what would the star be transitioning toward and in what time frame? Weaver explains, “As more data is being analyzed we hope it will be possible to identify exactly what type of transition this is. We don't have a deep enough understanding to get a definitive answer, and more observations are required. We can only speculate on what such a transition would be.”
“It’s important to note—lack of periodicity alone is not enough to rule out occultation. That's part of the reason why theories such as comets or planetary debris are so popular. We can't definitely rule out these things with our findings, but we can say that the power laws we have obtained are more consistent with intrinsic variation.”
Dahmen adds, “Our work gives a framework on how to analyze the data and perhaps even to classify stars into how close or how far away the stars are from such a transition. These statistical analysis tools have been tested and successfully applied to avalanche noise in magnetic systems and plastic deformation. We are transporting these tools to astrophysics to learn more about the dynamics of stars and eventually to compare different stars.
“As a next step we believe the same type of analysis should be applied to other stars to see how universal these fluctuation statistics are among the stars that are already known. In other words we would use the statistics of the noise in the light curves in these stars to learn something about the dynamical processes that are going on inside the star.”
This research is published in the December 19 issue of Physical Review Letters.