Abstract
The Chicxulub impact is thought to have triggered a global winter at the Cretaceous-Palaeogene (K-Pg) boundary 66 million years ago. Yet the climatic consequences of the various debris injected into the atmosphere following the Chicxulub impact remain unclear, and the exact killing mechanisms of the K-Pg mass extinction remain poorly constrained. Here we present palaeoclimate simulations based on sedimentological constraints from an expanded terrestrial K-Pg boundary deposit in North Dakota, United States, to evaluate the relative and combined effects of impact-generated silicate dust and sulfur, as well as soot from wildfires, on the post-impact climate. The measured volumetric size distribution of silicate dust suggests a larger contribution of fine dust (~0.8–8.0 μm) than previously appreciated. Our simulations of the atmospheric injection of such a plume of micrometre-sized silicate dust suggest a long atmospheric lifetime of 15yr, contributing to a global-average surface temperature falling by as much as 15°C. Simulated changes in photosynthetic active solar radiation support a dust-induced photosynthetic shut-down for almost 2 yr post-impact. We suggest that, together with additional cooling contributions from soot and sulfur, this is consistent with the catastrophic collapse of primary productivity in the aftermath of the Chicxulub impact.
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Data availability
The palaeoclimate general circulation model (GCM) output data as well as the silicate dust grain-size data from the Tanis K-Pg site that support the findings of this study are publicly available in the OSF repository via https://doi.org/10.17605/OSF.IO/2CDQG. The proxy-based latest Cretaceous temperature reconstruction data are available online in the PANGEA repository: https://doi.org/10.1594/PANGAEA.879763.
Code availability
The Python and Matlab source codes developed for reproducing the figures in this study are publicly available at the GitHub repository via github.com/cem-berk-senel/naturegeoscience-chicxulub/. The PlanetWRF model is available upon request from https://planetwrf.com/.
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Acknowledgements
This research is supported by the Belgian Federal Science Policy (BELSPO) through the Chicxulub BRAIN-be (Belgian Research Action through Interdisciplinary Networks) project (to P.C. & Ö.K.) and FED-tWIN project Prf-2020-038 (to J.V.), as well as the Research Foundation-Flanders (FWO; project G0A6517N, grant 12AM624N to C.B.S., grant 11E6621N to P.K., 12Z6621N to J.V., 12ZZL20N to O.T.). S.G. and P.C. acknowledge support of the VUB strategic programme. Ö.K. acknowledges the support of BELSPO through the ESA/PRODEX programme. M. Hagen and U. van Buuren (VU Amsterdam) are thanked for their assistance during the laser-diffraction particle-size analyses.
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C.B.S. and P.K. led the writing of the paper. C.B.S., P.K., O.T., J.V., S.G., P.C. and Ö.K. built the conceptualization of study and wrote the original text. C.B.S., P.K., O.T., J.V., S.G., R.D., M.A.P., P.C. and Ö.K. commented on and edited the original and revised manuscripts. C.B.S., O.T. and Ö.K. developed the general circulation model, implemented microphysics and radiation models and performed palaeoclimate simulations and post-processing of the results. P.K. and R.D. collected sediment samples during fieldwork at the Tanis K-Pg site in August 2017. P.K. carried out laser-diffraction grain-size analyses, with lab supervision of M.A.P. P.K. created Figs. 1 and 2 and Extended Data Fig. 1. C.B.S. created all other figures. All authors approved the final draft of the manuscript.
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Extended data
Extended Data Fig. 1 Geological context of the Chicxulub impact ejecta stratigraphy at the Tanis K-Pg boundary site.
a The inset shows a paleogeographic reconstruction and relief map for the latest Cretaceous42 as used in this modeling study with locations of Chicxulub and Tanis indicated. The base map is based on the latest Cretaceous paleogeographic data42. b Stratigraphy of the Tanis K-Pg boundary event deposit highlighting the lithological units (adapted from41; based on sections X-2741-A and X-2761) together with data on grain-size classes (clay, silt, and sand fractions), median grain-size values (in µm) and different types of impact ejecta found within this deposit. HCF = Hell Creek Formation (Upper Cretaceous). FUF = Fort Union Formation (Paleocene). c Representative grain-size distribution curves throughout the section, the colors match the stratigraphic units in b. The uppermost K-Pg boundary claystone (unit P1), indicated with a bold orange line, corresponds to final phases of atmospheric fallout of silicate dust injected by the impact and is used in present GCM simulations.
Extended Data Fig. 2 Mass and number density spectra of the grain-size dataset.
a Mass density spectrum of Tanis sediment sample X-2761-8A displayed by filled orange circles, which corresponds to the uppermost K-Pg claystone interval just below a Paleocene lignite and yields a median grain-size of 2.88 µm. The measured mass density spectrum was fitted by a trimodal lognormal size distribution as depicted by the blue solid line. This fitted model curve is the sum of lognormal size distributions comprising 3 modes. Model parameters are as follows: w0 = 0.002, Dpg,0 = 0.18 μm, lnσg,0 = 0.3087 (mode 1, green solid line), w0 = 0.125, Dpg,0 = 2.6 μm, lnσg,0 = 1.1193 (mode 2, cyan solid line), w0 = 0.01, Dpg,0 = 30 μm, lnσg,0 = 0.7284 (mode 3, magenta solid line), b Converted grain-size distribution into number density spectrum displayed by filled cyan circles. The converted spectrum is fitted by a lognormal size distribution (blue solid line), which is the input parameter for our GCM study. Converted model median grain-size corresponds to 0.125 µm with a logarithmic standard deviation of 0.446.
Extended Data Fig. 3 Number density spectrum of soot along with the particle size from K-Pg boundary layer.
It indicates a median diameter of 0.22 μm (Toon et al., 201639; Wolbach et al., 198520). Concerning the aerosol life cycle and processes, coagulation is one of the crucial microphysical mechanisms that might pose as important for the transport of aerosols in the atmosphere. Nanometric particles below 0.1 μm, that is, 0.015 μm < Dp < 0.052 μm79, whose range is referred to as the Aitken-mode (within the cyan dashed lines), are formed by two processes: (i) condensational growth on existing aerosol particles, and (ii) coagulation due to the random particle collisions. These nanometric particles can further grow into larger particles or chains, resulting in the so-called accumulation-mode (0.056 μm < Dp < 0.26 μm)79 (within the red dashed lines) where the coagulation can occur especially at high particle concentrations following the K-Pg impact. The median diameter of soot (0.22 μm20,39) in our simulations are prominently larger than the Aitken-mode interval, while lying within the range of accumulation-mode.
Extended Data Fig. 4 Latest Cretaceous surface temperatures from our GCM simulations, one year before the impact, in comparison with proxy observations43.
Proxy temperature data are presented as mean values +/- standard error of mean (SEM), displayed by black circles and horizontal error bars. Here, the proxy data consists of N = 66 samples at different latitudes. Green solid and dashed lines display the zonal mean of land temperatures during the boreal summer and winter seasons, from GCM simulations. Blue solid (boreal summer) and dashed (boreal winter) lines indicate the zonal mean of ocean temperatures. Both green (land) and blue (ocean) shaded areas show the region between the mean boreal summer and winter profiles. The black solid line refers to the GCM-based annual average of land and ocean surface temperatures at each latitude.
Extended Data Fig. 5 Global surface temperature reconstructions using the combined fine-grained ejecta scenario.
Results are displayed on a latest Cretaceous paleogeographic map (Extended Data Fig. 1a) and shown for different time snapshots. a Latest Cretaceous, 1 year before impact (annual mean). b Latest Cretaceous, 1 week before impact. c Impact winter, 1 month after impact. d 6 months after impact. e 2 years after impact. f 10 years after impact (annual-mean). Base maps are based on the latest Cretaceous paleogeographic data42.
Extended Data Fig. 6 Impact-generated global surface net radiative responses.
The temporal evolution from ~2 years of the latest Cretaceous towards 25 years of post-impact conditions, for the individual silicate dust, sulfur, soot, and combined scenarios. a Global-average surface net shortwave radiation flux. b Global-average surface net longwave radiation flux. Here in x-axis, the year of 0 refers to the start of the year where the impact event occurs. The solid purple dashed line denotes the moment of Chicxulub impact, that is, boreal spring season38. Our paleoclimate simulations indicate that the drastic changes in surface net shortwave/longwave radiation stabilize to pre-impact levels within the first 3 years after impact. Accordingly, this timescale, in which large radiative anomalies emerged, determines the timescale of the initial extreme cold (Fig. 4a).
Extended Data Fig. 7 Global PAR flux reconstructions in the latest Cretaceous.
Land-Ocean PAR flux a 1 day before impact (boreal spring) and b 6 months before impact (austral summer), displayed on a latest Cretaceous paleogeographic map (Extended Data Fig. 1a). The range of the green and purple colorbar represents the photosynthetically high and low radiative flux, varying between 0-160 W/m2. Base maps are based on the latest Cretaceous paleogeographic data42.
Extended Data Fig. 8 PAR flux reconstructions following the Chicxulub impact.
Land and ocean PAR flux from 1 day (post-impact state, instantaneous) to 1 and 2 weeks after impact for a silicate dust; b sulfur; and c soot scenarios, displayed on a latest Cretaceous paleogeographic map (Extended Data Fig. 1a). The range of the green-white colorbar denotes the photosynthetically high and low radiative flux. Base maps are based on the latest Cretaceous paleogeographic data42.
Extended Data Fig. 9 Effect of silicate dust particle size on the global column-integrated fine-grained ejecta mass.
Orange line refers to the present study, using the Tanis K-Pg silicate dust. Gray and black lines show GCM results using particle size constraints reported in previous modeling studies18,39. The gray line displays the response of nanometric sized particles, indicating a deposition rate with an atmospheric lifetime of ~7 years (as a lower threshold). The black line refers to the type 2 spherules39, representing microkrystites of 250 µm in diameter prone to very swift gravitational settling within a few days after impact. Cyan dashed line displays the shocked ejected quartz grains (mean diameter of 50 µm) defined as clastic debris27. We use the same amount of ejecta release in each GCM simulation, in the order of 2×1018 g as an upper limit. The optical properties of nanoparticles and type 2 spherules are the same as in the Tanis K-Pg silicate dust simulation, as we compare the microphysical response to the changes in particle size. Here in x-axis, the year of 0 refers to the start of the year where the impact event occurs. The purple dashed line denotes the moment of Chicxulub impact, that is, boreal spring season38. Regarding nanoparticles, those nanometric sized particles (median diameter of 20 nm) would grow into larger particles in atmosphere due to the coagulation. Such larger aggregates would have lower deposition rates on land and ocean (Fig. 3), hence higher atmospheric lifetimes. To illustrate, the deposition rate of nanoparticles (gray dashed line) would have occasionally shifted rightward through the response of silicate dust (orange dashed line) depending on the rate of coagulation. Therefore, the present simulation of nanoparticles, excluding coagulation, would serve as the minimum threshold for the atmospheric lifetime (t ~ 7 years). The inclusion of coagulation mechanism forming larger aggregates would lead to lower deposition rates on land and ocean (Fig. 3) for some fraction of nanoparticles, thus relatively high atmospheric lifetime of more than 7 years. Nevertheless, we do not expect nanoparticles to have an atmospheric lifetime and PAR response as substantial as single soot or micrometer-sized silicate dust.
Extended Data Fig. 10 Global-average surface temperature.
It is same as Fig. 4a, yet the time evolution is shown from 15 years before the Chicxulub impact instead of 2 years, for the individual silicate dust, sulfur, soot, and combined scenarios. The first 15 years correspond to the model initial spin-up simulation of 15-years, in which the latest Cretaceous conditions stabilized.
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Senel, C.B., Kaskes, P., Temel, O. et al. Chicxulub impact winter sustained by fine silicate dust. Nat. Geosci. 16, 1033–1040 (2023). https://doi.org/10.1038/s41561-023-01290-4
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DOI: https://doi.org/10.1038/s41561-023-01290-4
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