Shear wave model HMSL-S06: Click to download
Compressional wave velocity model HMSL-P06: Click to download
Houser et al. GJI, 2008

These Vp and Vs models are based on surface wave data for the upper mantle and body wave travel time data for the lower mantle. The bulk of the S, SS, P, and PP travel times were measured using cluster analysis. Phases such as ScS-S, SS-S, and PP-P from previous studies were also included. The tomographic inversion is based on the ray theory approximation using the LSQR algorithm. The file columns are longitude, latitude, depth, and dV/V starting with the bottom layer with 4 degree spacing. When plotting, it is customary to remove the mean value of each layer.


These models and others can be viewed using IRIS tools, SubMachine, and Dagik Earth .
Please contact me if you have any questions. Enjoy!

While tomographic models are nice to look at, they can also be useful tools for extracting information about Earth dynamics and state. In 2007, 2008, 2009, and 2020, we investigated patterns in 1D and 3D seismic structure to investigate the post perovskite transition, large low shear velocity provinces (LLSVP), subducting slabs, and temperature uncertainty in the lower mantle.

The BEAMS model (bridgmanite enriched ancient mantle structures) proposes that the Earth's lower mantle could be more silica rich than than the upper mantle and shows how the subsequent evolution is consistent with current seismic structure. The high viscosity of the lower mantle for Earth and other rocky planets could help sustain global mantle convetion for billions of years.

We see seismically fast (usually plotted blue) regions that extend from current and ancient subduction zones which appear to be subducted oceanic crust and upper mantle plunging across the mantle and collecting above the core-mantle boundary. Seismically slow (usually plotted red) areas occupy continent-sized regions at the core-mantle boundary with slow velocities extending to the upper mantle which appear to be linked to ocean island volcanos and hot spots.
The iron spin crossover, when electrons transition from a high-spin to a low spin state, has been expected to cause changes in P-wave velocity in the mid-mantle (see velocity sensitivity figure at right) which has elluded seismic detection for over a decade. The question was: are the predictions of the iron spin crossover applicable to our understanding of Earth's composition?
Combining observations from seismic tomography models using the vote map method, mineral physics calculations, and insights from geodynamics, we identified the unique seismic signal of iron spin crossover in these fast and slow velocity regions. The observation is possible because these regions are concentrated the mineral ferropericlase (Mg,Fe)O. Oceanic basaltic crust forms from partial melting of the upper oceanic mantle leading to a crust that is rich in Si and mantle rich in Mg. The unique, compositional detection of oceanic plates in the lower mantle and their regional concentration rather than even distribution across the mantle indicates that the mantle is a mosaic of rock with differing compositions and temperatures which hold the key to our planet's history.

I also make maps of topography of the 410 km and 660 km discontinuities and likewise transition zone thickness Houser et al., GJI, 2008. I followed up with analysis to interpet these maps along with seismic tomography to understand the thermal and composition contributions to these seismic observations EPSL 2010 EPSL 2016.

While some minerals in the mantle transition zone are capable of holding water, is it actually there? Using results from the studies mentioned above, transition zone topography and seismic tomography, the mantle transition zone appears to be quite dry. If the transition zone minerals are dry, then it is likely that the mantle as a whole is also dry. Thus, it may not take much water to explain the amount of water we observe, 1 ocean at the surface, maybe 1-2 oceans worth of hydrogen in the upper mantle, and 1-2 oceans worth of hydrogen in the transition zone. We studied the flux of water between the surface and interior by using the hydrogen isotopes, that is the ratio of deuterium to hydrogen, D/H. There are different scenarios that can explain the current observations, so more measurements in older rocks are necessary. Of course when discussing water in a planetary context, questions of "habitability" often arise, here is a brief comment on why that may not be the best approach when considering rocky planets.