- Open Access
Long period astronomical cycles from the Triassic to Jurassic bedded chert sequence (Inuyama, Japan); Geologic evidences for the chaotic behavior of solar planets
© The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB. 2012
- Received: 11 July 2012
- Accepted: 10 September 2012
- Published: 7 May 2013
Astronomical theory predicts that ~2 Myr eccentricity cycle have changed its periodicity and amplitude through time because of the chaotic behavior of solar planets, especially Earth-Mars secular resonance. Although the ~2 Myr eccentricity cycle has been occasionally recognized in geological records, their frequency transitions have never been reported. To explore the frequency evolution of ~2 Myr eccentricity cycle, we used the bedded chert sequence in Inuyama, Japan, of which rhythms were proven to be of astronomical origin, covering the ~30 Myr long spanning from the Triassic to Jurassic. The frequency modulation of ~2 Myr cycle between ~1.6 and ~1.8 Myr periodicity detected from wavelet analysis of chert bed thickness variation are the first geologic record of chaotic transition of Earth-Mars secular resonance. The frequency modulation of ~2 Myr cycle will provide new constraints for the orbital models. Additionally, ~8 Myr cycle detected as chert bed thickness variation and its amplitude modulation of ~2 Myr cycle may be related to the amplitude modulation of ~2 Myr eccentricity cycle through non-linear process(es) of Earth system dynamics, suggesting possible impact of the chaotic behavior of Solar planets on climate change.
- Astronomical cycle
- bedded chert
- Earth-Mars secular resonance
It has been widely demonstrated that Earth’s astronomical parameters (precession, obliquity, and eccentricity) control Earth’s climate through changes in temporal and spatial distribution of insolation on the Earth’s surface (e.g., Milankovitch, 1941; Hays et al., 1976; Berger et al., 1989). With the increase in the lengths of high-resolution sedimentary and paleoclimatic records, long period amplitude modulations of the obliquity and eccentricity cycles with periodicities of ~1 and ~2 Myr have been increasingly recognized (e.g. Beaufort, 1994; Olsen and Kent, 1999; Zachos et al., 2001; Lourens et al., 2005; Pälike et al., 2006; van Dam et al., 2006; Ikeda et al., 2010a, b; Boulila et al., 2011). This fact suggests the significant influence of these astronomical cycles on the global climate.
The long period astronomical cycles (>0.5 Myr periodicity) are predicted to have changed their frequencies through time due to the “chaotic” behavior of the inner planets, especially Earth-Mars secular resonance (e.g. Laskar, 1990; Laskar et al., 2004, 2011a, b). The sensitivity tests on the solar oblateness, tidal dissipation factor, and integration step-size by Laskar et al. (2004, 2011a, b) suggest that a significant frequency change of the long period astronomical cycles could have occurred before Neogene, and that their solution before Neogene may not be accurate enough for orbital tuning due to the uncertainty on the frequency of the long period astronomical cycles. If so, geological records of astronomically paced rhythms are the only evidence on actual frequency changes of these long period astronomical cycles in the past, and will be able to provide new constraints on orbital models with respect to the frequency modulation of the long period astronomical cycles. The eccentricity cycle related to the Earth-Mars secular resonance with the periodicity different from ~2.4 Myr were reported from the older part of the geological records such as ~1.6 Myr cycle in Early Cretaceous (Grippo et al., 2004; Huang et al., 2010b), and ~2.0 Myr cycle in Late Jurassic (Huang et al., 2010a), ~1.8 Myr cycle in Late Triassic (Olsen and Kent, 1999; Hüsing et al., 2011) and Middle Triassic (Ikeda et al., 2010a), and ~1.5 Myr cycle in Late Permian to Early Triassic (Huang et al., 2011). However, so far no study has identified frequency transition of these long period cycles. To identify frequency transition of long period cycles, determine their precise timing, and describe the nature of frequency transition, long and continuous geological records of astronomically driven rhythms are needed.
In this study, we adopted method of Ikeda et al. (2010a) to an Upper Triassic to Lower Jurassic bedded chert sequence that covers ~30 Myr interval, in order to identify orbital cycles and explore the evolution of long period astronomical cycles. Bedded chert consists of centimeter-scale rhythmical alternations of chert and shale beds whose rhythms are paced by precession and eccentricity cycles (e.g. Fischer, 1976; Hori et al., 1993; Ikeda et al., 2010a). The sedimentary rhythms of bedded chert formed as a result of cyclic changes in the accumulation rate of biogenic SiO2 within a background of extremely slow accumulation of pelagic clay (e.g. Hori et al., 1993). Additionally, bedded chert accumulated continuously on pelagic deep seafloor so that it covers a long time interval over hundreds of millions of years. Consequently, a bedded chert sequence has a potential to record the evolution of the long period astronomical cycles. We measured thickness of individual chert bed throughout the sequence, and confirmed ~20 kyr precession cycle origin of chert-shale couplet based on biostrati-graphic ages. We then constructed the astronomical time scale of the bedded chert sequence by tuning ~20 beds cycle to 405 kyr eccentricity cycle of constant duration, and conducted spectral analyses on the chert bed thickness time series to reconstruct temporal changes in the frequency and amplitude of ~2 Myr eccentricity cycle. Additionally, we examined amplitude modulation of ~2 Myr cycle and its relation to the origin of ~8 Myr cycle of chert bed thickness variations detected in this study.
To estimate the average duration of individual chert-shale couplets, we constructed an age model for the Upper Triassic to Lower Jurassic bedded chert sequence based on radiolarian-conodont-ammonoid biostratigraphic correlation with reference sections, where numerical ages have been estimated. The Norian/Rhaetian boundary in the studied section is correlated to the horizon of the last occurrence of the radiolarian Betracclum deweveri within the interval between the bed number 400 and 450 based on the radiolarian biostratigraphic correlation with the Queen Charlotte Island, Canada (Sugiyama, 1997). In the Queen Charlotte Island, the Norian/Rhaetian boundary is also identified as the Gnomohalorites cordileranus/Paracochloceras amoenum ammonoid zone boundary (Carter, 1993; Carter and Orchard, 2007). This ammonoid zone boundary is correlated with the Metasibirites spinescens/Cochlocearas suesssi ammonoid zone boundary in European sections, which is assigned as the Norian/Rhaetian boundary (Ogg, 2012). The age of the Norian/Rhaetian boundary is estimated as 209.5 ±1.0 Ma by magnetstratigraphic correlation with the astronomically tuned geomagnetic polarity time scale in the Newark Supergroup (Hüsing et al., 2011; Olsen et al, 2011; Ogg, 2012). The end-Triassic mass extinction interval in the studied section is well constrained within the interval of a chert bed number 796 based on the radiolarian faunal turnover from the Globolaxtorum tozeri zone to Pantanellium tanuense zone with the last occurrence of conodont Misikella posthernsteini (Hori, 1992; Carter and Hori, 2005). Across the end-Triassic mass extinction interval, radiolarian fauna shows a similar turnover pattern between the pelagic bedded chert sequence in the Inuyama area and the shallow marine sequence in the Queen Charlotte Islands, Canada (Carter and Hori, 2005). In the Queen Charlotte Islands, the radiolarian turnover is also followed by the last occurrence of conodont Norigondolella sp. and Triassic ammonoid Choristoceras rhaeticum, and predated by the first occurrence of Jurassic ammonoid Psiloceras aff. primocostatum (Tipper et al., 1994; Williford et al., 2007). The similar ammonoid turnover across the end-Triassic mass extinction is widely found in shallow marine sequences, such as the New York Canyon section in U.S.A., Pucara section in Peru and the St. Audrie’s Bay section in UK (e.g. Warrington et al., 2008; Schoene et al., 2010). The correlation among these areas is supported by a positive excursion of organic carbon isotope after a sharp negative excursion (Ward et al., 2001, 2004, 2007; Hesselbo et al., 2002; Guex et al., 2004; Williford et al., 2007). U-Pb age of 201.36 ± 0.13 Ma was measured at the horizon between the end-Triassic mass extinction interval and the Triassic/Jurassic boundary in the Pucara section (Schoene et al., 2010). Additionally, the duration of the interval between the end-Triassic mass extinction interval and the Triassic/Jurassic boundary, which is characterized by the last occurrences of the Triassic fauna and flora, including conodont Misikella posthernsteini, and the first occurrence of Jurassic ammonoid Psiloceras planorbis, respectively, was equivalent to 6 precession cycles (~120 kyr), according to the cyclostratigraphy at the St. Audrie’s Bay section, (Ruhl et al., 2010). Based on these chronostratigraphic constraints, the end-Triassic mass extinction interval in the Inuyama bedded chert can be estimated as 201.36 ± 0.20 Ma. This age uncertainties arose from the U-Pb age error and the duration of the end-Triassic mass extinction interval of the shallow marine section in UK, as described above (Schoene et al., 2010; Ruhl et al., 2010; Ogg and Hinnov, 2012). The Hettangian/Sinemurian and Sinemurian/Pliensbachian boundaries are not well constrained in this section (Hori, 1990, 1997). Thus, we treated an interval between Het-tangian and Pliensbachian as “Hettangian to Pliensbachian” interval. The Pliensbachian/Toarcian boundary is correlated with a horizon within an interval between bed number 1540 and 1563 based on the uppermost part of P. simplum IV Subzone of Hori (1990, 1997; Trillus elkhornensis Assem-blagezone) and the lower part of the H. hexagonus (Hh) Zone (Hori, 1990, 1997; Gröcke et al., 2011). These radiolarian zones correspond to the radiolarian zones of Eucyr-tidiellum nagaiae—Praeparvicingula tlellensis to Elodium pessagnoi—H. hexagonus (Carter et al., 2010). The ages of these radiolarian zones are constrained as the upper Pliensbachian and lower Toarcian, respectively, by ammonite biostratigraphy of Queen Charlotte Islands and other areas from North America (Carter et al., 2010). Thus, the horizon of the uppermost part of P. simplum IV Subzone of Hori (1990, 1997) is correlated with the Emaciaticeras emacia-tum/Dactylioceras tenuicostatum ammonite Zone boundary of European sections, which corresponds to the Pliens-bachian/Toarcian boundary (Ogg and Hinnov, 2012). The age of the Pliensbachian/Toarcian boundary was assigned as 182.7 ± 0.5 Ma (Ogg and Hinnov, 2012). This correlation is supported by a negative excursion of organic carbon isotope (Gröcke et al., 2011).
Based on the above age model, the average durations for a chert-shale couplet were calculated for the intervals corresponding to Rhaetian, Hettangian to Pliensbachian, and Rhaetian to Pliensbachian by dividing the duration by the number of beds in each interval. The average duration of an individual chert-shale couplet ranges between 17 and 28 kyr (median value, 22 kyr) for Rhaetian, between 18 and 27 kyr (median value, 21 kyr) for Hettangian to Pliensbachian, and between 19 and 25 kyr (median value, 21 kyr) for Rhaetian to Pliensbachian, respectively (Fig. 2). These estimated durations for an individual chert-shale couplet are consistent with the 17 to 21 kyr duration of the precession cycle during Late Triassic to Early Jurassic (Berger et al., 1989).
To assess the cyclicity of stratigraphic variations in the chert bed thickness, we performed wavelet analyses on the bed number series of chert bed thickness using a series of Matlab algorithms modified from those developed by Torrence and Compo (1998). This software can identify whether peaks in the spectrum of time series are significant against the red-noise (autoregressive lag1) background spectrum. The analysis was conducted in the bed number domain rather than in the depth domain because the sedimentation rates are considered to have changed significantly between chert beds and intercalated shale beds (Hori et al., 1993).
Figure 3(a) shows the results of wavelet analyses of the bed number series of chert bed thickness. The global wavelet power spectrum (Torrence and Compo, 1998) of the bed number series of chert bed thickness variations shows cyclicities of ~3 to 5 beds, ~100 beds, and ~500 beds above the 90% confidence level (Fig. 3(a)). The wavelet spectrum of the bed number series of chert bed thickness variations revealed occurrences of a ~ 100 bed cycle within the intervals between bed number 0 and 400, 700 and 900, 1200 and 1300, and 1500 and 1563 and a ~20 bed cycle in intervals between bed number 0 and 120, 200 and 270, 1000 and 1040, 1100 and 1140, and 1520 and 1563 above the 10% significant level (Fig. 3(a)).
To convert a bed number series of chert bed thickness variations to a time series, we used the 405 kyr eccentricity cycle as a tuning target for the time series (e.g. Olsen and Kent, 1999; Ikeda et al., 2010a). Laskar et al. (2004) proposed the use of the 405 kyr eccentricity cycle for the absolute time calibration for Mesozoic, because this cycle is originated from gravitational interaction between Jupiter and Venus, and is highly stable and constant in duration, as well as showing a dominant spectral peak due to the great mass of Jupiter (Laskar et al., 1993). On the contrary, the ~20 bed cycle, which is correlated with the 405 kyr cycle assuming each chert-shale couplet as the ~20 kyr precession cycle, is modulated its frequency between ~18 beds and ~25 beds due to the frequency modulation of the precession cycle between 17 kyr and 21 kyr cycle (the wavelet spectra in Fig. 3(a); see also figure 6 of Ikeda et al., 2010a). This is the reason the spectral peak of 20 bed cycle is not a dominant cycle, but split between ~18 bed and ~25 bed cycle.
To test the idea of changes in thickness of one chert-shale couplet, we converted the ~20 bed cycle in the bed number domain to a cycle with a constant duration of 405 kyr in the time domain, assuming ~20 bed cycle as 405 kyr eccentricity cycle. We then conducted spectral analyses of the tuned time series of chert bed thickness variations. As is shown in Fig. 3(c), the wavelet spectra of the chert bed thickness time series revealed distinct peaks at periodicities of ~0.1, ~2 and ~8 Myr above the 90% confidence levels, in addition to the 405 kyr periodicity. Additionally, we found frequency modulation of ~2 Myr eccentricity cycle with ~8 Myr periodicity and the amplitude modulation with ~4 Myr and ~8 Myr periodicities (Fig. 3(c)), respectively.
To further examine the long period cycles in the sedimentary rhythms of bedded chert and confirm their astronomical cycle origin, we compare the nature of the frequency modulation of ~2 Myr cycle between our geological data and the orbital solutions of Laskar et al. (2004, 2011a) during the period from Late Triassic to Early Jurassic. To compare the long period astronomical cycles in the geologic data with that of orbital solution with high frequency resolution, we conducted S-transform on the chert bed thickness time series and orbital solution of Laskar et al. (2004). The S-transform is a sophisticated wavelet analysis customized to better visualize the frequency modulation of low frequency cycles using a moving and scalable localizing Gaussian window (Stockwell et al., 1996). The orbital models of La2004 and La2010 were demonstrated as precise for the last 40 Myr and 50 Myr, respectively (Laskar et al., 2004, 2011a, b). The main difference between the La2004 and La2010 models is that the initial conditions of La2004 are adjusted to the JPL numerical ephemeris DE406 (Standish, 1998) over −5000 yr to +1000 yr from the present date, while La2010 is fit to the most precise planetary ephemeris INPOP06 and INPOP08 (Fienga et al., 2008, 2009). In particular, the La2010d version is adjusted to INPOP06 over the last 1 Myr that includes the five major asteroids, Ceres, Vesta, Pallas, Iris, and Bamberga (Laskar et al., 2011a), although La2010a, La2010b and La2010c are fit to INPOP08 over only the last 580 kyr for the La2010a and La2010b, and over the last 1 Myr for La2010c, but La2010c does not include the five major asteroids. Thus, the La2010d version could be considered as the most constrained version in the La2010 models (Laskar et al., 2011a, b). Nevertheless, the orbital solutions for pre-Neogene time cannot be solved precisely due to the uncertainty in the frequency of the long period astronomical cycles that reflects the “chaotic” behavior of the inner planets, especially the ~2 Myr cycle of Earth-Mars secular resonance (Laskar et al., 2004,2011a, b). Here we examine the general trend and nature of frequency modulation and amplitude modulation of the ~2 Myr eccentricity cycle computed by the orbital models.
The S-transform spectra for the orbital solutions of Laskar et al. (2004, 2011a) also show the frequency modulation and amplitude modulation of ~2 Myr periodicities, but their timing and frequency of the local maxima in amplitude are different with each other (Fig. 4(c)). Namely, the local maxima in amplitude of the ~2 Myr eccentricity cycle in the orbital solution of La2004 occur as ~2.6 Myr periodicity around 217 Ma, ~2.1 Myr periodicity around 212 Ma and 201 Ma, and ~2.3 Myr periodicity around 192 Ma, respectively. Those of La2010d occur as ~1.8 Myr periodicity around 218 Ma, ~2.5 Myr periodicity around 212 Ma, ~1.8 Myr periodicity around 205 Ma, ~1.6 Myr periodicity around 200 Ma, and ~2.8 Myr periodicity around 188 Ma, respectively. In other words, the frequency transition of the ~2 Myr eccentricity cycle in the orbital solution of La2004 occurred around 215 Ma and 198 Ma, and that of La2010d occurs at 215 Ma, 207 Ma, 203 Ma, and 195 Ma (Fig. 4(c)). Additionally, the ~2 Myr eccentricity cycles in the orbital solutions of La2004 and La2010d show amplitude modulation with ~5 to ~10 Myr periodicities, but the ~8 Myr cycle detected in the chert bed thickness time series is not dominant in the wavelet spectral results of the eccentricity in the orbital solutions of Laskar et al. (2004, 2011a) (Fig. 4).
7.1 Evolution of long period astronomical cycles during Late Triassic to Early Jurassic
The Upper Triassic to Lower Jurassic bedded chert sequence, a ~30 Myr long sedimentary record, is useful for examining the frequency transitions of long period astronomical cycles (Figs. 3 and 4). The ~2 Myr (100 bed) cycle observed in the chert bed thickness variations shows one of the strongest peaks on the wavelet and S-transform spectra. This could be correspond to the ~2.4 Myr eccentricity cycle observed today, because the ~2.4 Myr eccentricity cycle shows the strongest peaks among long period astronomical cycles (e.g. Laskar et al., 2004, 2011a). This ~2.4 Myr eccentricity cycle is considered as having undergone frequency transitions before Neogene due to the “chaotic” behavior of Earth-Mars secular resonance (figure 23 in Laskar et al., 2004). Frequency transitions of the ~2 Myr eccentricity cycle can be used as constraints for orbital models, if they are detected in geological records (Olsen and Kent, 1999; Laskar et al., 2004). The present state of Earth-Mars secular resonance characterized by the presence of ~2.4 Myr cycle in geological records can be traced back to 40 Ma (e.g. Pälike et al., 2004). On the other hand, in addition to the ~2.4 Myr periodicity caused by the eccentricity cycle related to Earth-Mars secular resonance, ~1.6 Myr cycle is reported from the gray scale record of the Lower Cretaceous limestone sequence in the Fucoid Marls, Italy (Grippo et al., 2004; Huang et al., 2010b), ~2.0 Myr cycle is reported from the TOC record of the Upper Jurassic limestone sequence in the Kimmeridge Clay, England (Huang et al., 2010a), ~1.8 Myr cycles are reported from the depth rank and color records of the Upper Triassic lacustrine sequence in the Newark Supergroup in North America (Olsen and Kent, 1999), magnetic suscepitability records of the Upper Triassic limestone sequence in Italy (Hüsing et al., 2011) and from the chert bed thickness record of the Middle Triassic bedded chert sequence in Japan (Ikeda et al., 2010a), and ~1.5 Myr cycles are reported from the magnetic susceptibility record of the Upper Permian to Lower Triassic hemi-pelagic sequence in China (Huang et al., 2011), respectively. However, no geological evidence has been presented on the timings and nature of frequency transitions of the ~2 Myr long eccentricity cycle.
In this study, ~2 Myr cycle changed its dominant frequency between ~1.6 and ~1.8 Myr at least twice during the Late Triassic to Early Jurassic (Fig. 4). Namely, the frequency transition of the ~2 Myr cyclicity of the chert bed thickness time series occurred around 212 to 206 Ma, and 201 to 192 Ma (Fig. 4). These frequency changes of ~2 Myr cycle indicate that the Earth-Mars secular resonance have undergone the chaotic transitions during the Late Triassic to Early Jurassic. The ~1.8 Myr cycle during Rhaetian is consistent with the previous reports from lake level records of Newark Supergroup and magnetic suscepitability records of the limestone sequence in Italy (Hüsing et al., 2011).
Worthy of note is the fact that the timings and nature of frequency changes of the ~2 Myr cycle are different between the chert bed thickness time series and the orbital solutions of Laskar et al. (2004, 2011a), although La2010d and chert bed thickness time series are similar in the ~1.6 Myr cycle at 200 Ma (Fig. 4). Additionally, the ~2 Myr cycle detected in the S-transform spectra of the chert bed thickness time series shows the amplitude modulation with ~4 Myr and ~8 Myr periodicities, which is different from the orbital solutions in which the ~2 Myr eccentricity cycle shows the amplitude modulation with ~5 to 10 Myr periodicity (Fig. 4). As described by Laskar et al. (2004, 2011a, b), their orbital solutions before Neogene have large degree of uncertainty due to the chaotic behavior of Earth-Mars secular resonance. The timings and nature of frequency transition of the ~2 Myr cycle detected in the geological record should have potential to constrain the “chaotic” evolution of the Solar system by adjusting the timings and nature of frequency modulation of the ~2 Myr eccentricity cycle in the orbital solutions to those of our geologic record.
7.2 Origin of the ~8 Myr cycle and its possible relation with the chaotic behavior of Solar planets
Although a spectral peak at the ~8 Myr (400 bed) cycle of the chert bed thickness variation has the strongest power, this periodicity is not known as the dominant periodicity of astronomical cycles (Laskar et al., 2004) (Fig. 4). Similar ~9 Myr cycle has recently been reported from the Cenozoic carbon isotope records of Zachos et al. (2001, 2008), which has been interpreted as the result of the amplitude modulation of the ~2 Myr eccentricity cycle (Boulila et al., 2012). This study also record the ~8 Myr periodicity as the amplitude modulation cycle of the ~2 Myr cycle of the chert bed thickness time series with nearly in-phase with the ~8 Myr cycle (Fig. 4(a)). Therefore, the amplitude modulation of the ~2 Myr eccentricity cycle is probably related to the ~8 Myr cycle in the chert bed thickness time series.
Orbital solutions suggested that the eccentricity cycles have negligible power in annual and seasonal insolation time series, although it does modulate the amplitude of the climatic precession, and the amplitude of seasonal insolation. According to the researches on astronomical cycles during Quaternary, it is generally thought that the ~100 kyr glacial-interglacial cycles are paced by the ~100 kyr eccentricity, which is amplified and/or rectified through non-linear internal climate feedback processes influenced through the amplitude modulation of the seasonal insolation by the eccentricity (e.g. Hays et al., 1976; Imbrie et al., 1993; Huybers and Wunsch, 2003). The signal of astronomical cycles detected in this study would also be amplified and/or rectified by similar internal non-linear processes(es). Similarly, we suggest that the ~8 Myr cycle in the chert bed thickness time series results from amplitude modulation of the ~2 Myr eccentricity cycle through non-linear amplification process(es). Boulila et al. (2012) suggested that the amplitude modulation of the ~2 Myr eccentricity cycle may play an important role in carbon cycling, controlling a chain of astro-climatically sensitive processes such as terrestrial weathering, biosphere productivity, carbonate sedimentation and dissolution, burial and oxidation of organic carbon, etc. (e.g., Pälike et al., 2006; Li et al., 2009). Although their potential link with the chert bed thickness variation is highly speculative, productivity is most likely related with the chert bed thickness variation (e.g. Hori et al., 1993). In addition, terrestrial weathering is also potentially a controlling factor of the chert bed thickness variation, because the extreme source of biogenic silica burial in the ocean is the dissolved silica from continents (e.g. Tréguer et al., 1995; Tréguer, 2002). The formation mechanism of bedded chert rhythms and their genetic relation to long period astronomical cycles would be a key for understanding this non-linear amplification process(es), which should be clarified in the future. The ~30 Myr orbitally-paced lake level records in the Newark Supergroup during Late Triassic will also provide additional constraints for this topic. These issues must be addressed for complete understanding of the impact of long period astronomical cycles on global surface environments.
The nature of long-term astronomical cycles preserved in the Late Triassic to Early Jurassic bedded chert sequence in the Inuyama area, Japan, covering ~30 Myr has been examined. The average duration of a chert-shale couplet during Late Triassic to Early Jurassic is ~20 kyr, supporting its precession cycle origin. Spectral analyses of the chert bed thickness time series, which is fine-tuned based on the assumption that ~20 bed cycle is the 405 kyr eccentricity cycle of constant duration, revealed the presence of ~0.1, ~2 and ~8 Myr periodicities in addition to the 405 kyr periodicity above 10% significant level. Among these, the ~2 Myr cycle, which is interpreted as the long period eccentricity cycle caused by Earth-Mars secular resonance, changes its frequency between ~ 1.6 and ~ 1.8 Myr. The frequency transitions of the ~2 Myr cycle in the chert bed thickness time series are the first geologic evidence of chaotic transitions of Earth-Mars secular resonance. Such modulation patterns of the ~2 Myr cycle in the geological records will provide an important constraint on orbital models. Furthermore, the ~8 Myr (400 beds) cycle is detected from the spectral analyses of the chert bed thickness variation. Our results suggest that the ~8 Myr cycle in our record may reflect the amplitude modulation of the ~2 Myr eccentricity cycle associated with Earth-Mars secular resonance through non-linear amplification and/or rectification process(es) within the global climate system, probably similar to the origin of ~9 Myr cycle of the carbon isotope variation during Cenozoic (Boulila et al., 2012).
We thank Prof. Paul E. Olsen (Lamont-Doherty Earth Observatory, Columbia University) for his constructive comments for cyclostratigraphy and astronomical theory, Dr. T. Ito (National Astronomical Observatory of Japan) for his advice concerning the astronomical theory and orbital calculation model, Dr. H. Miyahara (The University of Tokyo) for her advice regarding spectral analysis, and Drs. A. Karasuda, H. Sakuma, S. Yamamoto, S. Takahashi (The University of Tokyo), and R. S. Hori (Ehime University) for their fruitful discussion. We also wish to thank Mr. S. Robbins of the University of Tokyo’s GCOE program for the English proofreading and editing of this paper. We are grateful for editor T. Yamazaki. The manuscript was greatly improved by careful reviews from Prof. J. Ogg (Purdue University) and an anonymous referee. This research was partly supported by grants from the Japan Society for the Promotion of Science (20098755 and 20127776), Overseas Internship Program for Outstanding Young Earth and Planetary Researchers, and Fujiwara Natural History Foundation awarded to M. Ikeda.
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