The Middle Ordovician breakup event1,2 is currently the best documented example of such events in the Main Asteroid Belt (MAB) thanks to a large number of stratigraphically well-dated, L-chondritic, fossil meteorites3. Geochemical analysis has linked the 7.5-km wide Lockne crater, central Sweden, to this family of meteorites4,5, which supports the previous notion that also the crater production rate was significantly increased during some millions of years after the MAB event3. The recent discovery of the nearby, 0.7-km diameter, contemporaneous Målingen crater6 suggests it to form a doublet impact structure together with the larger Lockne crater and as we will show here, most likely by a binary, ‘rubble pile’7 asteroid. Despite observational evidence that about 16% of the Near Earth Asteroids (NEAs) are binary8, only a handful of the approximately 188 known craters on Earth have been suggested as potential doublets, i.e. Clearwater East & West (Canada), Kamensk & Gusev (Russia), Ries & Steinheim (Germany), Suvasvesi North & South (Finland) and Serra da Cangalha & Riachão (Brazil)9,10, of which most are still disputed11. The continuous sedimentation in the marine target environment at Lockne (diameter of apparent crater, DA = 7.5 km) and Målingen (DA = 0.7 km) has allowed both impact craters to be biostratigraphically dated and correlated with great precision6. The two craters are situated approximately 16 km center-to-center distance from each other (Fig. 1). Whereas the Målingen crater until now has been known only as an enigmatic, circular feature with lithologies of similar type as at Lockne6, the Lockne crater has been extensively studied for the past few decades e.g. refs. 12, 13. At the time of the impact, the Lockne-Målingen area was located on the southern hemisphere in an epicontinental sea that covered most of current Baltoscandia (Fig. 2). The target water depth was approximately 500 m, i.e. about equal to the estimated 600-m diameter Lockne impactor, when modeled as a massive object13. The Målingen impactor would have been about 150 m in diameter14.

Figure 1
figure 1

The location of places mentioned in the text, the Lockne-Målingen doublet impact structure and the distribution of crystalline ejecta from the inner, nested, basement craters.

The map is created in Adobe Illustrator 10 based on several decades of mapping in the area led by the authors J. O., E. S. and our late colleague Professor Maurits Lindström. Some of the mapping results have been published6,12, but are subject to constant revision.

Figure 2
figure 2

Paleogeography of Baltica and neighboring cratons at the time of the increased cosmic bombardment following the ~470 Ma asteroid breakup event and timeline for the related meteorite falls (black dot and line) as well as known craters (red dots).

Light blue color represents areas of shallow epicontinental seas and dark blue areas of deep ocean. This distribution may, however, have varied somewhat due to periodical transgressions and regressions of the sea. The map is created in Adobe Illustrator 10. Paleogeographic map modified from PALEOMAP Project30. For details on the craters and meteorite falls see Supplementary Table 1.

Recent studies suggest that Målingen, just as Lockne, retains much of its original shape, sedimentary infill and ejecta deposits6. Shock metamorphic evidence has confirmed its impact origin6,15. The good preservation of the two adjacent craters is due in large part to the fortunate combination of the marine target environment, wherein continued sedimentation covered and protected the newly formed craters and that they subsequently became entombed by overthrust nappes of the Caledonian orogeny12. Subaerial and glacial erosion have since then re-exposed the craters, but with surprisingly small effects on their original morphologies and the preservation of the impactites. From the ejecta distribution, it is possible to deduce that the impact trajectory was from today's east towards west and with an impact angle of about 45° 13.

The relatively rapid post-impact sedimentation in the craters allows high precision in chronobiostratigraphic dating6. The impact event occurred during the lower part of the, in Baltoscandia synchronous, chitinozoan Lagenochitina Dalbyensis Zone. Considering the relatively short time span of 0.1–1 million years for the L. dalbyensis Zone, the age of the craters can be estimated to 458 ± 0.5 Ma6. Schmieder et al.11 state that only a synchronicity of two neighboring impact events within ~±0.5% hardens the evidence for double impact, a requirement well fulfilled by Lockne-Målingen (i.e., ±0.5 m.y. equals an error of <0.1%). Moreover, our inspection of continuous drill cores penetrating both craters have not revealed any sign of reworking or a distal ejecta layer in the post-impact sequences of either crater, which would be expected in the case of two separate impact events.

In the Thorsberg quarry at Kinnekulle in southern Sweden (Fig. 1), the discovery of > 90 fossil L-chondritic meteorites in a Middle Ordovician limestone section16, which were deposited over a period of ~2 m.y.3,17, support the theory that the meteorite flux to Earth and likely also the cratering rate, was enhanced by one to two orders of magnitude for at least a few million years as a consequence of the large breakup event in the MAB ~470 Ma3,18. The increased influx was further corroborated by the analysis of the approximately 5 m.y. younger meteorite from Brunflo19, near the Lockne crater (Fig. 1) and additional findings of equally high concentrations of L-chondritic chromite micrometeorites in both Chinese and Russian coeval limestones20,21. In figure 2, we have plotted confirmed Middle- to early Late Ordovician impact craters in Europe and North America as well as a timeline with known craters and meteorite falls from the first few tens of millions of years following the ~470 Ma asteroid breakup to illustrate the position of the Lockne-Målingen impact in the succession of events.

On the Baltoscandian shield, five confirmed (Lockne-Målingen, Tvären, Granby, Kärdla) and one suspected (Hummeln) impact craters of relevant ages have been identified so far (Fig. 2; Supplementary Table 1). Of these craters, only Lockne has been studied in sufficient detail with respect to its meteoritic component to unequivocally be linked to the L-chondrite parent body4,5. However, preliminary results from our ongoing search for chromite in the Målingen resurge deposits indicate an impactor of similar composition as at Lockne. A more comprehensive study dealing with the identification of the impactor is planned. Thus, the lithology of the Lockne- and possibly also the Målingen-, impactor is known from chemistry. In addition, as we will show here, its physical properties can be inferred by the circumstance of a doublet crater and its geomorphology.

The probability that Lockne and Målingen occurred together by chance, rather than having been paired in space can best be calculated supposing that Lockne (i.e., the larger, less frequent size of the two) formed first during the c. 1 million year interval allowed by the ±0.5 m. y. uncertainty in their crater ages. The maximum distance between two craters to be considered a doublet is 120Dp, where Dp denotes the diameter of the principal object. It is controlled by the maximum limit of stability of an asteroid satellite22,23. For the Lockne impactor (Dp = 600 m) this gives a 144 km in diameter circular area, which represents about 3.2 × 10−5 of the Earth's surface. The probability that a crater of Målingen's diameter forms somewhere on Earth is today about 9 × 10−5 per year24, but here we adjust this with the maximum estimate of a two orders of magnitude higher cratering rate for the time period of interest3,18. The probability of a chance occurrence within 144 km is about 0.29 when assuming the highest cratering rate. If we restrict the range to the observed 16 km between the two craters, the probability of a chance occurrence falls to 1.4 × 10−2. Even if assuming the highest suggested cratering rate of two orders of magnitude higher than today's impact flux the cratering rate must still have to be raised by a factor between 3.4 (for the 144 km range) to 71 (for the observed 16 km separation) to make the association between Lockne and Målingen a chance event, which is very unlikely.

Thus, with an unequivocal doublet impact at Lockne-Målingen we can assess the physical properties of the culprit binary projectile. The fragmentation of a parent asteroid tends to lead to gravitational re-accumulation of dust and coarser debris to form families of ‘rubble pile’ asteroids7. Simulation has shown that the formation of satellites around parent bodies is a natural and frequent outcome of this type of collisional events7,22,25. Other potential processes for binary formation, e.g. capture, are considered of less importance in the Lockne-Målingen case due to low probability and insufficient separation between the bodies8.

The nearly horizontally configured target sequence at Lockne and Målingen comprised ~500 m of seawater, ~50 m of lithified, bedded ‘orthoceratite limestone,’ and ~30 m of dark, organic-rich mud (today ‘alum shale’), resting on a peneplained Proterozoic crystalline basement6,12,13. Numerical simulations of the marine Lockne impact event show the development of a ‘soup plate’ –shaped concentric transient cavity that is also reflected in the apparent morphology of the crater and that only large (tens of meters) ejecta blocks from the inner, deeper, ‘nested’ crater in the basement was able to penetrate the water cavity wall and impact the sea up to 6 km beyond the center of the target (i.e., >2.5 km outside the nested crater rim)13. The extent of the outer crater outside the nested crater rim is in the simulations at the most ~2 km on the down-range side and even less on the up-range side13. However, the simulations assumed a monolithic impactor. We here argue that the observed geology of the Lockne crater is more consistent with the impact of a fragmented projectile. For instance, up to 100 × 100 m wide bodies of ballistic basement crater ejecta in the form of a crystalline breccia occur at three times the distance of the modelled extent of the outer crater in the seawater and sediments on the western, down-range side (Fig. 1). These ejecta lie in stratigraphic positions indicating several tens of meters penetration into the sedimentary succession. It seems unlikely that the crystalline ejecta could have passed the water cavity wall and the layer of seawater intact and with enough force for this penetration into the seafloor (Fig. 3). Thus, the outer crater of Lockne must have been wider than indicated by the numerical simulations using a massive impactor. In addition, geophysical modeling (magnetic and gravity) has indicated a relatively shallow nested crater in the basement with a poorly developed central uplift despite a diameter well above the simple- to complex crater transition26,27. Likewise, core drilling and geological mapping of the Målingen crater have revealed a similar shallow and wide outer crater surrounding a relatively shallow nested, basement crater compared with the expected depth-to-diameter ratio of a simple crater in crystalline rock6. We believe that the reasons for these unusual morphologies of Lockne and Målingen are to be found in the properties of the projectile. During the passage of the atmosphere a fragmented or ‘rubble pile’ asteroid in the size range of the Lockne-Målingen projectiles will be subject to aerodynamic breakup. Numerical simulation has shown that aerodynamic disruption is expected for monolithic, rocky meteors of less than 200 m in diameter and that they then develop into a broad, flat projectile with a cross-section that may exceed that of the parent body by an order of magnitude28. A similarly-sized weaker body such as a comet would develop into a debris jet28. Obliquity of impact is intensifying the breakup effect. For already fragmented, or ‘rubble pile’, asteroids it can be expected that the same occurs also for a significantly larger projectile diameter than for a monolithic. Likewise, a low-density impactor is known to produce a relatively smaller and shallower crater than a dense projectile with the same kinetic energy29. However, the fragmentation may be of less importance for the cratering process if the effective diameter of the disrupted impactor, or debris jet, is smaller than the diameter of the expected transient crater from an equal mass nondisrupted impactor28. The numerical simulation of the Lockne impact assuming a monolithic 600-m in diameter projectile gave a transient crater diameter of 5 km13. Thus, with an order of magnitude wider diameter for an aerodynamically disrupted projectile (i.e. 6 km) it would exceed the transient crater width and affect the cratering process leading to the observed geomorphology of the Lockne crater.

Figure 3
figure 3

The development of the unusually wide brim (i.e., outer crater) in the water column and sedimentary strata surrounding the nested, basement crater of the Lockne impact structure (inset figure indicates the down-range location).

Preserved bodies of crystalline ejecta (photo of locality “Berget”, Fig. 1) have penetrated tens of meters down into the succession of consolidated limestones and are thus thought to have landed directly on exposed sedimentary strata without first passing the water cavity wall and the hundreds of meters thick water column.

The here presented unique Lockne-Målingen doublet offers a likewise unique opportunity to reconstruct the properties of an impactor (i.e., L-chondritic, fragmented or even ‘rubble-pile’, binary asteroid) and to provide detailed ground truth in deciphering the consequences such a projectile has on the cratering process, ejecta distribution and the final crater shape. This is to great aid in the interpretation of remote sensing data from doublets on other planetary bodies such as the moon and Mars. In addition, the precise dating of the Lockne-Målingen impact in relation to the MAB breakup event provides a hands-on reference for studies of the formation of binaries from asteroid breakup events.