On the detection of the Wilkes Land impact crater
Earth, Planets and Space volume 70, Article number: 135 (2018)
The definitive existence of a giant impact crater, two times larger than the Chixulub crater in the Yucatan peninsula, from an extraterrestrial origin, 1.6 km beneath Wilkes Land, East Antarctica, remain controversial. Here, we use the latest high-resolution gravito-topographic geopotential (SatGravRET 2014) model over Antarctica to offer a plausible confirmation of its existence. SatGravRET 2014 has a spatial resolution between 1 and 10 km at most places and included contemporary space gravimetry and gradiometry data from GRACE and GOCE, and other data including Bedmap 2 bedrock topography. We computed the gravity disturbances, the Marussi tensor of the second derivatives of the disturbing potential, the gravity invariants and their specific ratio, the strike angles and the virtual deformations to quantify the detailed geophysical features for the Wilkes Land anomaly. This set of the gravitational parameters revealed enhanced and more detailed geophysical features on the Wilkes Land Crater than previously possible only with the traditional gravity anomalies. Our findings support prior studies stating that in the Wilkes Land there is a huge impact crater/basin with detectable gravity mascon which is mostly consistent with the characteristics of an impact crater.
Motivation, method, and data
Motive and aim
This paper has been written with one of the aims to confirm prior published controversial findings, including von Frese et al. (2013) and Weihaupt et al. (2015) arguing that the Wilkes Land anomaly beneath the ice in East Antarctica is consistent with the geophysical characteristics of an impact crater/basin. The Wilkes Land anomaly (also known as the Wilkes Land) is centered at \(\varphi\) = –70°S and λ = 120°E. Von Frese et al. (2009) described the possibility of existence of a huge impact crater basin. We have analyzed the most recent gravity field model tailored for Antarctica. We used it to compute not only the traditional gravity anomalies but a whole spectrum of functions of the disturbing gravitational potential of the Earth (called here: the gravity aspects), thus providing more detailed information about the putative crater, basin, mascon and its possible enjambement to southern Australia. We also work with bedrock topography model Bedmap 2 (published in 2013); for references see below.
A giant impact crater beneath the Wilkes Land ice sheet was first proposed by Schmidt (1962); the hypothesis was developed by Weihaupt (1976), challenged by Bentley (1979) and supported by Weihaupt (2010). The Wilkes Land anomaly or mascon was first reported by von Frese et al. (2006, 2009) analyzing satellite gravity data available at that time. They used data from the GRACE mission (Gravity recovery and climate experiment, see, e.g., https://www.nasa.gov/mission_pages/Grace/index.html) in spherical harmonic expansion to degree and order 90 (half-wavelength resolution on the ground ~ 200 km); they worked with gravity anomalies and the derived first vertical derivative of them to enhance the resolution and the accuracy of the Wilkes Land anomaly. Their findings were further supported by magnetic data in von Frese et al. (2013) and by Weihaupt et al. (2015). The latter authors wrote: “…recent data from various sources revealed that the structure has a diameter of some 510 km, …, has a subglacial topography relief of ≥ 1500 m, and exhibits a negative free air gravity anomaly associated with a larger central positive free air gravity anomaly…”. A more comprehensive review of the Wilkes Land anomaly, and its plausible origin, is described in detail by Weihaupt et al. (2015).
The primary objective of this study is to use recently available high-resolution gravity and subglacial topography models to provide an independent assessment and to contribute positively to the hypothesis claiming that the Wilkes lowland is an impact crater (basin).
In addition to the GRACE gravity model, the data in Antarctica were recently amended by a rich set of gradiometry data from Gravity field and steady-state ocean circulation explorer (GOCE, see, e.g., http://www.esa.int/Our_Activities/Observing_the_Earth/GOCE; ESA 2014). Here, we use the gravity aspects computed from the recent SatGravRET 2014 model (shortly: RET 14, see Hirt et al. 2016) with spherical harmonic expansion to degree and order 2190 (half-wavelength resolution corresponding to ~ 9 km spatial scale) for the study. They originated, roughly speaking, by combining the gravity model European improved gravity model of the Earth by new techniques (EIGEN 6C4; Foerste et al. 2014), also with the GOCE gradiometry data, and the bedrock topography from Bedmap 2 (Fretwell et al. 2013). We then compute various gravity functions (the aspects) of the disturbing gravitational potential in addition to the gravity anomalies. These are: the Marussi tensor of the second derivatives of the disturbing potential, the gravity invariants and their specific ratio, the strike angle and the virtual deformations.
The results presented below support the hypothesis about the impact crater and mascon in the Wilkes Land and its possible continuation to present-day southern Australia. However, we are very well aware that the gravity data alone which is used in this study cannot provide the complete constraint to unravel the geophysical interpretation of the above.
The core of our method is in the use of various gravitational aspects, namely the gravity anomalies or disturbances Δg, the components of the Marussi tensor Γ of the second derivatives Tij of the disturbing potential, the gravity invariants I1 and I2, their specific ratio I, the strike angle θ and the virtual deformations vd. Every single one gravity aspect tells its own “story” about density and in turn about gravity anomalies. By “topography,” we mean the bedrock topography, derived mainly from airborne ice-penetrating radars (Bedmap 2). All the gravity aspects and the bed topography create a composite data set which should always be accounted for together.
The theory underlying our methodology is described mainly in Pedersen and Rasmussen (1990) and Beiki and Pedersen (2010). The new contribution of this study is related to the computation of all gravitational aspects listed above including the virtual deformation, vd, which comes from Kalvoda et al. (2013). A more complete review of the theory (and examples) used for this study is in Klokočník et al. (2016, 2017a, b).
The Marussi tensor provides more complex information than the gravity anomalies (or disturbances) Δg only; Tzz informs about the target body location, the other components Tij of Γ refer to the orientation of the causative structure. The components Tij provide sharpening of the anomalies and enhancements of the high-frequency content without changes in the location or shapes of the anomalies (e.g., Saad 2006). The invariants I1 and I2 can be looked upon as nonlinear filters enhancing the sources having big volumes; they discriminate major density anomalies into separate units. The specific ratio I (sometimes called “2D indicator”) of I1 and I2 can indicate two-dimensionality of the causative body (e.g., Pedersen and Rasmussen 1990, p. 1559; Jekeli 2009, p. 120). The condition I = 0 is necessary but not a sufficient condition for two-dimensionality. The strike angle θ tells us how the measurements (used to derive Γ) rotate within the main directions of the underground structure; when I = 0, the values of θ may indicate a dominant 2D structure. The virtual deformation vd, as an analogy to the tidal deformation, characterizes the “tensions” (compression and dilatation) generated by the causative body; one can imagine the directions of such a deformation due to “erosion” brought about solely by “gravity origin” (Klokočník et al. 2013, p. 90).
Many examples of the local use of some of the gravity aspects (mostly Δg, sometimes also or solely Tij, seldom I1 and I2 or θ) can be found in the literature (see, e.g., Saad 2006; Murphy and Dickinson 2009; Mataragio and Kieley 2009; Beiki and Pedersen 2010). Our theory, method and notation (with various results for different parts of the world) can be found in Kalvoda et al. (2013), Klokočník and Kostelecký (2015) or Klokočník et al. (2010, 2013, 2014, 2016, 2017a, b, 2018). The computations of all the aspects listed above were done by the software developed by B. Bucha (see Bucha and Janák 2013) and by our own software.
“Gravito-topographic” gravity model over Antarctica
The gravity of the Earth can be represented by a geopotential model in terms of harmonic coefficients, also known as Stokes coefficients. The gravity field of the Earth at an external point outside of the Earth can be computed as a double summation of the Stokes coefficients, Clm, Slm, to degree l and order m, derived usually from a combination of diverse satellite and terrestrial data. The “topography” is represented by a model of the bedrock topography for Antarctica achieved dominantly but not only via the airborne radio-echo sounding (RES) techniques.
We use the best data now available. In particular, we work with RET 14 (Hirt et al. 2016). It is a degree-2190 gravity field model SatGravRET2014, given as a set of harmonic geopotential coefficients, meaningful for the continent of Antarctica (not for all the world). Roughly speaking, it combines the global gravity field model EIGEN 6C4 and the Bedmap 2 topography. The EIGEN 6C4 Foerste et al. 2014) is a global combined gravity solution including gradiometry data from the whole GOCE mission. The important fact is that EIGEN 6C4 is better and higher resolution gravity model namely in Antarctica in a comparison with its predecessors. Note that EIGEN 6C4 is free of gravity anomalies measured in Antarctica (it contains there only satellite data from GRACE, GOCE and other satellites).
More precisely: the RET 14 combines predecessors of EIGEN 6C4 with other and very important gravity data sets; it combines the ITG-GRACE2010s and the unconstrained GOCE TIM5 satellite gravity models to degree and order 180 (for references see Foerste et al. 2014). These models describe the long- and medium-wavelength components of the Earth’s static gravity field from GRACE and GOCE missions. The “non-gravity” data to RET 14 come from the Earth 2014 1 arcmin global topography model (Hirt and Rexer 2015) which incorporates the Bedmap 2 bedrock topography (see below) and the other data sets; these are topography from the Shuttle Radar Topography Mission (SRTM), Greenland Bedrock Topography v3 and SRTM30_PLUS v9 bathymetry (for more references see Hirt et al. 2016).
Bedmap 2 (Fretwell et al. 2013) contains the bedrock elevation beneath the grounded ice sheet. It is given as a 1 × 1 km grid of heights of the bedrock above sea level; the actual spatial resolution is worse, say 5 × 5 km (but not everywhere). The bedrock topography for Antarctica has been achieved mostly via the RES data. The resolution and quality are still much worse in some areas with rare data or without any data (see Figs. 3, 12 and other material in Fretwell et al. 2013, esp. pp. 379 and 388), see Fig. 5. The authors themselves call these two big areas (Recovery and Support Force Glaciers and Princess Elizabeth Land) “poles of ignorance”; they do not concern this analysis.
RET14 increases the resolution of underlying gravity field models and decreases the resolution of Bedmap 2; generally, the spatial resolution of RET14 should be about 10 km over the area of our interest.
Precision in RET 14 should be about 10 mGal, but is not homogeneous over the whole continent of Antarctica. For EIGEN 6C4, based on information deduced from (Pavlis et al. 2012; Foerste et al. 2014; Fretwell et al. 2013; Hirt et al. 2016), we estimated 10 mGal as a pessimistic limit. These statistical estimates are available only for the gravity anomalies/disturbances in the fundamental source Pavlis et al. (2012). In Klokočník et al. (2017a), we studied this problem (see Section Discrimination criterion in that paper) and found that owing to mutual high correlations of the gravity disturbances for close localities, the error of Δg in EIGEN 6C4 can be about 5 mGal. For RET 14, this should be still better, a few milligals; this number (2–3 mGal) is considered here as a rough error estimate of Δg in RET 14. But, again, this optimistic number is not valid anywhere in Antarctica.
Color figures presented here have various nonlinear scales to emphasize specific features and details. The gravity disturbances are in given milliGals [mGal], the second-order derivatives are in Eötvös [E]. Recall that 1 mGal = 10−5 ms−2, 1E ≡ 1 Eötvös = 10−9 s−2. The invariants have units [s−4] and [s−6]. The virtual deformations (vd) are shown in blue color, where compression takes place and in red where dilatation occurs. The bedrock topography from Bedmap 2 yields heights above present-day sea level (asl) in [m]; here the topography is presented in the same system as the gravitational aspects, i.e., in the geographic coordinates (\(\varphi\), λ), related to the reference ellipsoid WGS 84; sometimes we append the original coordinate system of Bedmap 2, i.e., the rectangular system of coordinates (x, y), northing/easting (in [km]). Both types of maps are in the polar stereographic projection with a geographic latitude of true scale at 71°S (which is an optimum choice for Antarctica). This is not true for the zooms.
A critical inspection of the data to understand various artifacts and to avoid misinterpretations is necessary; it has already been done elsewhere (e.g., Klokočník et al. 2016, 2017a, 2018). The artifacts are due to insufficient or missing data or their irregular, inhomogeneous distribution. For example, the ground track density of the RES data in Bedmap 2 and other data are highly anisotropic. The RES data are densely sampled along track (along the flight direction of the vehicle bearing RES) while the flight tracks themselves are often widely spaced. Due to this anisotropy, along-track measurements show many details, but only in narrow tracks along the flights, while the cross-track gaps may create a problem (similar problem is known from satellite dynamics, see Klokočník et al. 2015). Due to this effect in some areas, the bedrock topography is reliable, in other areas not (Figs. 4, 5).
The results and discussion
For our computations, we used RET 14 and Bedmap 2 (and EIGEN 6C4 alone only for South Australia). We present a choice of the relevant disturbances Δg, the component Tzz of Γ, I1, I2, I, θ, vd and the bed topography; due to space reasons we cannot present all the gravity aspects.
First, we introduce Δg and vd for the whole Antarctica (Figs. 1, 2). The putative Wilkes Land mascon is centered at \(\varphi\) = –70°S and λ = 120°E (von Frese et al. 2009, 2013). The Wilkes Land anomaly is clearly visible as a semicircular structure (the northern part is deformed roughly at seashore). Then, we inform about the bedrock topography in the same area according to the Bedmap 2 model; in color in Fig. 3, in black and white in Fig. 4. The subglacial topography also exhibits a semicircular pattern. The coverage of ground tracks in Bedmap 2 is shown in Fig. 5; we can see the lines with measurements and with data and the gaps without data between them, like a fan (spreading from a seashore station). One has to be aware of this data distribution (Figs. 4, 5) and consequent limitations when interpreting RET 14.
We continue in the range of latitudes and longitudes of Fig. 3 and show Δg, Tzz, I1, I2, and vd in the series of Figs. 6, 7, 8, 9 and 10. Reader can see semicircular shape namely by Δg, Tzz and vd, interrupted on the northern side by the ocean. Central part of the impact structure, belonging to the mascon (centered at \(\varphi\) = –70°S and λ = 120°E), yields positive Δg and Tzz but due to various geological processes after the impact, we can detect river valleys and similar details crossing this area. The positive part is surrounded, namely from southern directions, by significant negative values of Δg and Tzz of semicircular shape. As for vd, Fig. 10 shows the compression zones (in blue color) around the former mascon.
Our figures document that the Wilkes Land anomaly is a candidate for the greatest impact crater or the only one impact basin known till now on the Earth (over 500 km diameter), partly preserved and now hidden under the ice or sea.
The putative Wilkes Land mascon is centered at \(\varphi\) = –70°S and λ = 120°E (von Frese et al. 2009, 2013). We can now more evidently observe it in terms of the gravito-topographic signal using RET 14 and Bedmap 2. There is no central peak typical of large impact craters (with a positive Δg and Tzz, surrounded by their negative values, then with positive values at a ring, etc.), there is a wide central area with prevailing positive Δg.
Figures 6, 7, 8, 9 and 10 confirm it (see previous subsection). Moreover, we prepared zooms for the mascon; they are in Figs. 11 and 12 for Δg and Tzz, respectively. The mascon is depicted very well as a significant Δg reaching more than + 100 mGal and Tzz reaching ~+ 100 E. It is shown with various details, indicating influence of external and internal forces acting since the time of impact (a river valley), step by step degenerating the original gravity footprint.
The shape of the putative basin and its mascon is not perfectly circular, but rather semicircular, or of a U-shape; the northern (sea) side part is disrupted and fragmented. Accounting Fig. 2 from von Frese et al. (2013), we have to seek the gravity aspects at the southern Australia, too, because there we may depict a “continuation” of the Wilkes Land anomaly from Antarctica. The area of investigation is shown in Fig. 13, and the results follow in Figs. 14, 15, 16, 17 and 18.
The series of Figs. 14, 15, 16, 17 and 18 illustrate a plausible continuation of the Wilkes Land anomaly from Antarctica to the southern Australia. We have to account for seashore zones where the crater/mascon is deformed and rings are fragmented. Reader can watch narrow belts of negative and positive Δg and Tzz along South Australian coastline; he/she can follow vd in Figs. 10 and 18. One can imagine the central place of the impact (roughly the northern seashore of Antarctica) now at \(\varphi\) = –70°S and λ = 120°E.
To further support our findings, and thus also conclusions of von Frese et al. (2009, 2013), we prepared Fig. 19, a composite of Figs. 10 and 18, shifted significantly in latitude (to mask mostly SN motion due to plate tectonics) and slightly in longitude to achieve experimentally, by eye, the best fit of both parts in one unit. We guess it is convincing: two components evolving from one piece in the past.
These results widen space for geophysical interpretations and speculations. The huge impact had a planetary consequence, including for example the striking antipodal relationship of it to the Siberian Raps (claimed by von Frese et al. 2009). Therefore, we can look at various large mostly SN oriented depressions in Antarctica in south, west and east directions from the mascon, including the subglacial Lake Vostok, in new eyes, as a part of or as an item among many consequences after the giant impact nearby. The impact may trigger separation of Antarctica from Australia.
By applying recent gravito-topographic models valid for Antarctica (SatGravRET 2014 and Bedmap 2), we support findings by von Frese et al. (2006, 2009), Weihaupt et al. (2015) and others who claimed that in the Wilkes Land there is a huge impact basin with a mascon centered at \(\varphi\) = –70°S and λ = 120°E from an extraterrestrial origin. This would be the greatest impact crater known or the only one impact basin on the Earth preserved (but only partly and under the ice or sea) till the present, with over 500 km in diameter. The Wilkes anomaly in Antarctica has, according to our study, and in agreement with von Frese et al. (2013), a continuation (shifted by plate tectonics since the time of separation) to the southern Australia. The geophysical structure is well visible with the virtual deformations. Nevertheless, the exact geophysical interpretation of the continental dynamical process remains speculative. It is noted that the new gravito-topographic model SatGravRET 2014 that we used to conduct this study has about two orders better precision and resolution than that used by von Frese et al. (2006).
- GRACE mission:
Gravity recovery and climate experiment
Gravity field and steady-state ocean circulation explorer
- EIGEN 6C4:
European improved gravity model of the Earth by new techniques
radar echo sounding
- RET 14:
Hirt et al. (2016); gravity field model SatGravRET2014
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J. Klokočník is responsible for the concept and the text, J. Kostelecký partly for the theory, mostly for the figures and a part of software, A. Bezděk for computations and overall checks of everything. All authors read and approved the final manuscript.
This work has been prepared in the frame of projects #13-36843S (Grant Agency of the CR) and RVO #679,858 15 (Czech Academy of Sciences), partly supported by the project LC 1506 (PUNTIS) from the Ministry of Education of the CR. We thank B. Bucha for the computations of the gravity aspects with EIGEN 6C4 and RET 14, H. D. Pritchard for his help with the bedrock topography data and Prof. C.K. Shum for reading and improving our manuscript. We are obliged to two anonymous reviewers for many useful comments.
The authors declare that they have no competing interests.
Availability of data and materials
We declare that input data from the models EIGEN 6C4, SatGravRET2014 or Bedmap 2 are generic (see the list of reference below). The outputs (the files to plot our figures) are available on request at the authors.
Work of J. Klokočník and A. Bezděk on the whole paper (data collection, analysis, interpretation of data, writing the manuscript) has been partly paid by the projects #13-36843S (Grant Agency of the Czech Republic, CR) and RVO #679,858 15 (Czech Academy of Sciences), work of J. Kostelecký (analysis, interpretation of data, plotting figures, writing the manuscript) was partly supported by the project LC 1506 (PUNTIS) from the Ministry of Education of the CR.
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Klokočník, J., Kostelecký, J. & Bezděk, A. On the detection of the Wilkes Land impact crater. Earth Planets Space 70, 135 (2018). https://doi.org/10.1186/s40623-018-0904-7