Catoctin/Fauquier contact

Catoctin/Fauquier contact
Power washing a quarry block near Aldie, VA that preserves a soft sediment contact of the Fauquier Formation cap carbonate and pillow basalt of the Catoctin Formation.

Thursday, February 5, 2015

Questioning Seismic Tomography


            Making inferences based on data are ubiquitous in science. Unfortunately, all too often the data is far from complete. The roads of reason around that obstacle, are fraught with peril though. Perhaps as much as in any field, Seismic Tomography has felt this cold hard truth. To understand, imagine yourself standing in a large world full of craters, valleys, hills, and deep pits, only that you are blind folded. Someone tells you to find the lowest elevation on the planet. So what you do, is start walking around and trying to find where the ground begins going downward. You eventually find a place, where you know that no matter what direction you walk in, you are going “up”. Alas, you conclude you have reached the lowest point. As stupid as that conclusion is, it is quite similar to many  “scientific” inference techniques.  I am describing the way “altitude” corresponds to the level of disagreement between the data and a theory, the error/misfit, in inverse theory. You may say “well, why not get out of that valley, and go looking around for the true lowest point, comparing each local lowest elevation to the previous ones you have come across”. Alas, with the state of computational resources as they are, for many problems involving huge data sets, this is truly is analogous to telling a person blindfolded wanderer to make that search across that large world on foot.

            There are several categories of methods used to tackle this difficulty in science, other than “just keep searching”. The obvious method, is “just start out close to where you know the lowest elevation is”, to continue the analogy. That is, explore scientific models and hypotheses from a starting point that you think are close to the truth (mathematically, start from an initial condition close to the global minimum). It works terrific! At least, it does assuming where you start is actually close to the right answer. Otherwise, it fails miserably. Even worse, due to noise and other lack of ideality in the data obtained, the “true” answer may not even be the genuine optimum solution.  

            Seismic Tomography, a method that uses this type of search, uses observations of vibrations near the surface that have travelled from a distant source, to infer how those vibrations travelled inside the earth. Namely, it tells how fast waves travel at various places inside the earth.  It starts with a basic model of the earth’s set of “speed limits” and proceeds to improve those estimates from recorded travel times of waves. This has many issues.

Seismic waves are not laser beams, so why do many seismologists keep pretending they are? Ray theory, that treats waves in the manner than geometric optics treats light, is quite inaccurate in many respects, a fact that is often masked through subtle omissions of certain details. If one were to compare the travel time of an actual wave from a source to a quite distant receiver to the prediction made by ray theory, they would find fair agreement often. The missing fact though, is that the velocity model used to make that prediction for ray theory, was constructed explicitly to make it agree with those observations, not the actual velocity of the earth, which is to a large extent unknown. That is one of the huge problems with not just Seismic Tomography, but any discipline that uses very ill-posed inverse problems to attain models: since the answer is horribly non-unique even qualitatively, it is possible to generate quite dubious answers that fit the data exceptionally well, and even allow for a fair amount of consistent extrapolation.

One way to address this issue with some math, would be to simply analyze the uncertainties given by the scientists who made the ”answer”. Unfortunately, Seismic Tomographers don’t really give error bars or any kind of uncertainty measurements.  In some cases, depending on what the result is used for, it is slightly understandable. However, all too often, it makes the issue not “is this good or bad science?” but rather “is this even science?”. The issues don’t just stop at the accuracy of the numbers, but what the numbers even mean is in question as well.

One of the perhaps dumbest and common assumptions in seismic tomography, is isotropy (wave speeds being independent of direction of propagation). In 1982, Don Anderson said “…we knew that our isotropic models were not very good but we had no other choice. It is simply so far, computers were not large enough to integrate the anisotropy parameter”. More recent attempts to include anisotropy have relied on layer models or patches of anisotropy. While this might seem like progress, it is not a full scale inversion with respect to anisotropy, and could simply just be a means of fixing errors produced by assuming isotropy everywhere else.  To make matters worse, even a highly anisotropic model input into a computer, can be modeled as an isotropic one. It means that if you assume isotropic to start, you can find remarkable agreement with data based on inverting for a model, even when the model is horribly anisotropic.


The dejection of learning an imaged plume is a computational artifact, the knowledge that the imaged subducting slab is questionable for many reasons related to bias of incidence angles sampled and ignorance as to the amount of thermal diffusion affecting imaged wavespeed, really makes you wonder what you can and cannot trust in seismic tomography. Not to mention that the vast majority of the other anomalies seen are beneath the floor of systematic uncertainties in the answers.

Why are Martian volcanoes so lonely?

First view of the Tharsis Montes from Mariner 9. The poor image quality is due to a global dust storm that was occurring at the probe's arrival.

Martian volcanoes were confirmed to exist in the early 1970s, from pictures taken by the Mariner 9 orbiter. These first images revealed massive shield volcanoes, like Hawaii on Earth but taller than Mount Everest and wider than Ohio.  One of the first observations was that three of these larger volcanoes, the Tharsis Montes, exist in a straight line, each separated by about 750 km. Rather than a volcanic chain like Hawaii, the line of the Tharsis Montes appears to be related to a rifting feature, but why are they spaced with a certain distance?

Topographic map of the Tharsis province.
My research focuses on the processes occurring beneath the surface of Mars that result in the spacing of volcanoes. Specifically I am looking at the role of permeability barriers and decompaction channels in the Martian lithosphere. As hot mantle melt rises up into the Martian lithosphere it cools and crystallizes out in the surrounding rock matrix. At a certain horizon, the crystals will clog the matrix preventing further upwards movement. This horizon is the permeability barrier. Melt from below continues to rise up until it encounters the barrier. Pressure builds as the melt accumulates, so a horizon of high porosity is forced open below the barrier, like air forcing a balloon to expand. This is the decompaction channel.

I use the alphaMELTS computer program to simulate this process. Starting with an estimate of mantle composition, the virtual material is brought up from great depth, where it melts from decompression. When the material reaches the bottom of the lithosphere the melt continues to rise and the crystallization is simulated. The minimum depth of the permeability barrier is assumed to be where the crystallization rate is a maximum.
Results of one dimensional crystallization simulation. The bottom of the graph represents the bottom of an imagined 50 km lithosphere. The red line is the crystallization rate of melt as it ascends. The permeability barrier in this simulation would likely be at about 38 km depth.


Permeability barriers and decompaction channels have been studied in terms of mid ocean ridges on Earth. The slope of the mid ocean ridge combined with the barrier and channel focus a large region of melt to the ridge axis. On Mars a similar focusing could be occurring which would focus melt below surface volcanoes. The act of crystallization actually releases heat, which would allow melt to rise above the normal permeability barrier layer, like thermal erosion. Anywhere in the layer that is a little thermally eroded would focus melt to that point, increasing the erosion rate there. The overall instability of the layer would have a preferred wavelength due to the balance of barrier rise and melt supply rate. This instability is to be modeled in two and three dimensions and compared to the actual distribution of volcanoes on the surface of Mars.

Diagram of permeability barrier instability. Melt (red arrows) releases heat (green arrows) and is focused by the slope of the unstable permeability barrier (thin black line). The initial permeability horizon is represented by dashed black line.

Unraveling Secrets Deep Beneath Our Feet:


Exploring the detailed structure within the continents using Earthscope USArray


    The vast majority of the human population lives on a continent. In fact, you are likely on one right now. The part of the continent on which you stand could have been stable since before even the first bacteria existed, hundreds of million to several billion years ago. It may be surprising to find then, that we know very little about how these continents formed and how they have remained stable over most of earth’s history. (Find out how old the part of the continent you are on right now, check out Figure 1 created by Rob Butler at the University of Leeds.)

Figure 1: The age of the continents
Ma stands for million of years ago. Dark blue regions within the continents
are the oldest ( formed over 2500 million years ago) while yellow regions
within the continents are the youngest (Formed less than 200 million years ago)

Rob Butler- University of Leeds 
http://www.see.leeds.ac.uk/structure/assyntgeology/extra_info/ehistory.htm
 


   The continents have remained, while so much else on earth has changed – they preserve billion year old secrets of their formation, alteration, and breakup and provide insight to the past, present and future of continental stability. Understanding more about what is beneath our feet does more than just help us understand the long lasting stability of the continents. We may all be more familiar with one hazard associated with the geologic structure (the type and thickness of differing rock layers)  – earthquakes . Understanding what makes up the continents beneath our feet – specifically the geologic structure - can help us address more pressing questions such as: What determines the locations of large earthquakes that happen within the interiors of continents? (See Figure 2 for the locations of the some of the largest earthquakes since 1980, are any near you?) These types of questions led to a National Science Foundation funded project to improve the image of the interior of the earth called Earthscope USArray.
  
Figure 2: Earthquake and Hazard map of the Continental United States
This map shows earthquakes with magnitude 4.8 and larger that have been recorded since 1980 as white circles. Magnitude 4.8 earthquakes have been chosen as the smallest  shown on the map as they can be easily felt and may cause small structural damage. This map also shows areas prone to earthquake hazard in the United States. Regions that have high earthquake hazard are in warmer colors while low earthquake hazard areas are in cooler colors. Notice some areas within the continents have high earthquake hazard. Figure made using USGS Hazard Program























    Earthscope USArray uses seismic stations spaced 70 kilometers apart across the continental US and Alaska to collect information about the earth beneath our feet (Figure 3).  These seismic stations collect seismograms, which contain information about four main things: an earthquake, the station, background movement, and the structure of the earth. If we remove the earthquake, station, and background information, we are left with information from the earth’s structure. This is one method seismologists use to “see” into the earth’s structure at each station. The effect is similar to a taking a telescope and pointing it into the earth at each station. Using the many stations increases the resolution of the images we have of the continent’s structure, and just like increasing the number of pixels in a picture, gives us a more clear idea of what is beneath our feet (Figure 4). Earthscope USArray provides the highest “pixel” or resolution image of any continent. Allowing scientists to look at the earth in a whole new way. 

Figure 3: Earthscope USArray Stations
Earthscope has added seismic stations across the US. This figure shows the improvement of station coverage from prior to the Earthscope USArray project (right) to after (left). Stations are represented by any color triangle. 

Figure 4: An example of resolution improvement
Increasing the number of stations is similar to increasing the number pixels in an image like these smilies. The left could be likened to poor station coverage (the right image in Figure 3) going to a higher and higher resolution with better station coverage ( the left image in Figure 3). The edges of the smilies become more clear with higher pixel coverage, just like the geologic structure beneath the earth becomes more clear with higher station coverage. 




















For more information about Earthscope and projects being done, visit:

To make your own earthquake map (like  Figure 2)  visit:




References:

Butler, Rob, Claire Gordon, and Martin Krabbendam."Making New Continents." The Moine Thrust.  University of Leeds. 

"Earthquake Hazards Program." Earthquake Hazards Program. US Department of the Interior -  United States Geological Society, 26.Aug, 2014. 




Wild images of Martian meteorites Lead to Information About Mars’s Ancient Surface and Atmosphere




By James W. Dottin III

                    
               
“Are those fossils of a piranha and a griffon”? This may be the first question to pop into your mind! Your second question may be, “wait was there life on Mars”? Unfortunately, the answer to both questions is no. These are two images of a Martian volcanic rock, found in Antarctica, that formed skeletal-type minerals within itself.  Although, the cool photos fail at answering the question of life on Mars, they do provide us with valuable information about how the surface of Mars interacted with its atmosphere. Previous studies on these Martian rocks have told us that when you use chemistry to separate sulfur from the Martian rocks and analyze it closely, you receive data that tell you that early on in Mars’s lifetime, the sun was ripping apart molecules that are bound by sulfur in the atmosphere in cool and unusual ways. The images tell us how the sulfur got into the rocks!!

I was able to use a microscope with a camera to take really zoomed in pictures of the Martian meteorite and load the images into a computer program that is able to detect small differences in color within the image. The colors of interest in these images are the light/tan/gold color of the “fossil looking minerals” and the really tiny bright gold/yellow specs which are the sulfur minerals. I hypothesized that the we found sulfur in these rocks due to a process called “assimilation”, a lava flow picking up material as it flows across a surface. A proposed chemical reaction suggested that we should expect a certain amount of “fossil looking minerals” to sulfur minerals. The computer software calculated the amount of “fossil looking minerals” and sulfur minerals (by distinguishing their color differences) and confirmed that the hypothesis was indeed correct!

So what’s the overall big picture? Billions of years ago, the sun ripped a bunch of sulfur molecules apart, allowing the sulfur to fall onto the surface of mars. A volcano erupted, spewing lava over the surface, allowing the lava to capture and incorporate the sulfur into the flow. The lava cooled and became rock. A large asteroid hit mars and ejected large amounts of surface material into space. Some of the surface material traveled through space and made its way to earth and fell in Antarctica. Brave meteorite hunters found the Martian rock, it was delivered to me, and I delivered this information to you. Thank you for reading my blog and stay tuned!