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Orbitally tuned timescale and astronomical forcing in the middle Eocene to early Oligocene

Westerhold, T., Röhl, U., Pälike, H., Wilkens, R., Wilson, P. A., Acton, G.·2014·Climate of the Past
DOI 10.5194/cp-10-955-2014

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Abstract

Abstract. Deciphering the driving mechanisms of Earth system processes, including the climate dynamics expressed as paleoceanographic events, requires a complete, continuous, and high-resolution stratigraphy that is very accurately dated. In this study, a robust astronomically calibrated age model was constructed for the middle Eocene to early Oligocene interval (31–43 Ma) in order to permit more detailed study of the exceptional climatic events that occurred during this time, including the middle Eocene climate optimum and the Eocene–Oligocene transition. A goal of this effort is to accurately date the middle Eocene to early Oligocene composite section cored during the Pacific Equatorial Age Transect (PEAT, IODP Exp. 320/321). The stratigraphic framework for the new timescale is based on the identification of the stable long eccentricity cycle in published and new high-resolution records encompassing bulk and benthic stable isotope, calibrated XRF core scanning, and magnetostratigraphic data from ODP Sites 171B-1052, 189-1172, 199-1218, and 207-1260 as well as IODP Sites 320-U1333, and 320-U1334 spanning magnetic polarity Chrons C12n to C20n. Subsequently orbital tuning of the records to the La2011 orbital solution was conducted. The resulting new timescale revises and refines the existing orbitally tuned age model and the geomagnetic polarity timescale from 31 to 43 Ma. The newly defined absolute age for the Eocene–Oligocene boundary validates the astronomical tuned age of 33.89 Ma identified at the Massignano, Italy, global stratotype section and point. The compilation of geochemical records of climate-controlled variability in sedimentation through the middle-to-late Eocene and early Oligocene demonstrates strong power in the eccentricity band that is readily tuned to the latest astronomical solution. Obliquity driven cyclicity is only apparent during 2.4 myr eccentricity cycle minima around 35.5, 38.3, and 40.1 Ma.

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Figures

Figure 1 Location map of sites used in this study on 34 Ma paleogeographic reconstruction in Mollweide projection (ODSN, 2011; Hay et al., 1999) and detailed location map in the Pacific (big map, red stars) with additional IODP/ODP/DSDP sites. F.Z. = fracture zone (modified from Pälike et al., 2010).
Figure 1 Location map of sites used in this study on 34 Ma paleogeographic reconstruction in Mollweide projection (ODSN, 2011; Hay et al., 1999) and detailed location map in the Pacific (big map, red stars) with additional IODP/ODP/DSDP sites. F.Z. = fracture zone (modified from Pälike et al., 2010).CC-BY · From the PDF
Figure 2 Overview of data from ODP Site 1218 and IODP Sites U1333/U1334 in the depth domain (in brackets the water depth of each site at 34 Ma; Pälike et al., 2010). The plots show stable carbon isotope data (black, gray), normalized median scaled (NMS) wt% based on calibrated XRF core scanning data for Si (green), Ca (blue), and Fe (red) (for details see methods chapter), spliced core image, and magnetic polarity reversal pattern transferred to 1218 and U1334 by correlation to U1333 (Pälike et al., 2010; Westerhold et al., 2012a). Data sources: all XRF core scanning data from this study; bulk δ 13 C U1334 from Wilson et al. (unpublished) (black) and this study (gray), 1218 from Coxall et al. (2005) (black), U1333 from Wilson et al. (unpublished) (black), and Leon-Rodriguez and Dickens (2013) (gray); benthic ( Cibicidoides spp.) δ 13 C of 1218 from Lear et al. (2004), Coxall et al. (2005), Tripati et al. (2005), and Coxall and Wilson (2011).
Figure 2 Overview of data from ODP Site 1218 and IODP Sites U1333/U1334 in the depth domain (in brackets the water depth of each site at 34 Ma; Pälike et al., 2010). The plots show stable carbon isotope data (black, gray), normalized median scaled (NMS) wt% based on calibrated XRF core scanning data for Si (green), Ca (blue), and Fe (red) (for details see methods chapter), spliced core image, and magnetic polarity reversal pattern transferred to 1218 and U1334 by correlation to U1333 (Pälike et al., 2010; Westerhold et al., 2012a). Data sources: all XRF core scanning data from this study; bulk δ 13 C U1334 from Wilson et al. (unpublished) (black) and this study (gray), 1218 from Coxall et al. (2005) (black), U1333 from Wilson et al. (unpublished) (black), and Leon-Rodriguez and Dickens (2013) (gray); benthic ( Cibicidoides spp.) δ 13 C of 1218 from Lear et al. (2004), Coxall et al. (2005), Tripati et al. (2005), and Coxall and Wilson (2011).CC-BY · From the PDF
Figure 3 High-resolution XRF core scanning data, bulk and benthic stable carbon isotope data, core images and cyclostratigraphy from Chron C12n to C13n for Sites U1334, 1218, and U1333 in the depth domain. For details see captions of Fig. 2. Blue lines mark early Oligocene ash layers apparent in all three sites (Kuroda and and Westerhold, 2013). Numbers represent the assigned short (green) and long (blue) eccentricity cycle maxima positions in the orbital solution (see Supplement Fig. S8). Band pass filters: for Site U1334 from Si data (0 . 14 ± 0 . 042 cycle meter -1 (c m -1 ), 7.2 m band in Supplement Fig. S2a), for Site 1218 from benthic stable carbon isotope data (0 . 164 ± 0 . 049 c m -1 ), and for Site U1333 from Si data (0 . 2 ± 0 . 06 c m -1 ; 5 m band in Supplement Fig. S2c).
Figure 3 High-resolution XRF core scanning data, bulk and benthic stable carbon isotope data, core images and cyclostratigraphy from Chron C12n to C13n for Sites U1334, 1218, and U1333 in the depth domain. For details see captions of Fig. 2. Blue lines mark early Oligocene ash layers apparent in all three sites (Kuroda and and Westerhold, 2013). Numbers represent the assigned short (green) and long (blue) eccentricity cycle maxima positions in the orbital solution (see Supplement Fig. S8). Band pass filters: for Site U1334 from Si data (0 . 14 ± 0 . 042 cycle meter -1 (c m -1 ), 7.2 m band in Supplement Fig. S2a), for Site 1218 from benthic stable carbon isotope data (0 . 164 ± 0 . 049 c m -1 ), and for Site U1333 from Si data (0 . 2 ± 0 . 06 c m -1 ; 5 m band in Supplement Fig. S2c).CC-BY · From the PDF
Image 4
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Image 5
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Figure 6 Cyclostratigraphy from Chron C15r to C18n.1n for ODP Site 1052 in the depth domain. Ca / Fe data, revised depth scale and paleomagnetic reversal pattern with errors from Pälike et al. (2001), inclination data from Ogg and Bardot (2001). Numbers represent the assigned short (green) and long (blue) eccentricity cycle maxima positions in the orbital solution (see Supplement Fig. S8). Band pass filters: 405 kyr filter in black (0 . 09 ± 0 . 027 c m -1 ); 100 kyr filter in green (0 . 32 ± 0 . 096 c m -1 ). Please note the strong obliquity component present from 10 to 30 rmcd in the 1052 sedimentary record.
Figure 6 Cyclostratigraphy from Chron C15r to C18n.1n for ODP Site 1052 in the depth domain. Ca / Fe data, revised depth scale and paleomagnetic reversal pattern with errors from Pälike et al. (2001), inclination data from Ogg and Bardot (2001). Numbers represent the assigned short (green) and long (blue) eccentricity cycle maxima positions in the orbital solution (see Supplement Fig. S8). Band pass filters: 405 kyr filter in black (0 . 09 ± 0 . 027 c m -1 ); 100 kyr filter in green (0 . 32 ± 0 . 096 c m -1 ). Please note the strong obliquity component present from 10 to 30 rmcd in the 1052 sedimentary record.CC-BY · From the PDF
Figure 7 High-resolution XRF core scanning data, bulk and benthic stable carbon isotope data, core images, and cyclostratigraphy from Chron C18n.1n to C20n for Sites U1333, 1218, 1260, and Hole 1172A in the depth domain. For details see caption of Fig. 2. ODP Site 1260 XRF Fe intensity data from Westerhold and Röhl (2013), benthic stable isotope data, and magnetostratigraphy from Edgar et al. (2007). ODP 1172A XRF data from Röhl et al. (2004), bulk δ 13 C data from Bijl et al. (2010). Extend of the MECO is marked by a light orange bar and the carbon isotope excursion at the end of the MEO is marked by a orange bar in 1260 and 1172A (for correlation details see Supplement Fig. S10). Arrows mark change in phase relation between stable isotope and XRF core scanning data. 405 kyr band pass filters: for Site U1333 from Fe data (155-165 rmcd 0 . 36 ± 0 . 110 c m -1 ; 165175 rmcd 0 . 25 ± 0 . 07 c m -1 ; 175-190 rmcd 0 . 36 ± 0 . 1 c m -1 ; 2.78, 4, and 2.78 m bands in Fig. S6c); for Site 1218 from Si data (260270 rmcd 0 . 42 ± 0 . 105 c m -1 ; 270-278 rmcd 0 . 22 ± 0 . 05 c m -1 ; 278-293 rmcd 0 . 11 ± 0 . 027 c m -1 ; 2.38, 4.55, and 9.09 m bands in Supplement Fig. S5b); for Site 1260 from benthic stable carbon isotope data (0 . 1 ± 0 . 03 c m -1 ); and for Hole 1172A from log ( Ca / Fe ) data (0 . 1 ± 0 . 03 c m -1 ). Note the dominant obliquity component in Hole 1172A.
Figure 7 High-resolution XRF core scanning data, bulk and benthic stable carbon isotope data, core images, and cyclostratigraphy from Chron C18n.1n to C20n for Sites U1333, 1218, 1260, and Hole 1172A in the depth domain. For details see caption of Fig. 2. ODP Site 1260 XRF Fe intensity data from Westerhold and Röhl (2013), benthic stable isotope data, and magnetostratigraphy from Edgar et al. (2007). ODP 1172A XRF data from Röhl et al. (2004), bulk δ 13 C data from Bijl et al. (2010). Extend of the MECO is marked by a light orange bar and the carbon isotope excursion at the end of the MEO is marked by a orange bar in 1260 and 1172A (for correlation details see Supplement Fig. S10). Arrows mark change in phase relation between stable isotope and XRF core scanning data. 405 kyr band pass filters: for Site U1333 from Fe data (155-165 rmcd 0 . 36 ± 0 . 110 c m -1 ; 165175 rmcd 0 . 25 ± 0 . 07 c m -1 ; 175-190 rmcd 0 . 36 ± 0 . 1 c m -1 ; 2.78, 4, and 2.78 m bands in Fig. S6c); for Site 1218 from Si data (260270 rmcd 0 . 42 ± 0 . 105 c m -1 ; 270-278 rmcd 0 . 22 ± 0 . 05 c m -1 ; 278-293 rmcd 0 . 11 ± 0 . 027 c m -1 ; 2.38, 4.55, and 9.09 m bands in Supplement Fig. S5b); for Site 1260 from benthic stable carbon isotope data (0 . 1 ± 0 . 03 c m -1 ); and for Hole 1172A from log ( Ca / Fe ) data (0 . 1 ± 0 . 03 c m -1 ). Note the dominant obliquity component in Hole 1172A.CC-BY · From the PDF
Figure 8 Sedimentation rate estimate in cm kyr -1 based on astronomical tuning compared with paleomagnetic based estimates using the timescale of Cande and Kent (1995, CK95). For reference the CK95 and tuned GPTS (this study) are drawn.
Figure 8 Sedimentation rate estimate in cm kyr -1 based on astronomical tuning compared with paleomagnetic based estimates using the timescale of Cande and Kent (1995, CK95). For reference the CK95 and tuned GPTS (this study) are drawn.CC-BY · From the PDF
Figure 9 Comparison of magnetochron boundary ages and durations for Chron C12 to C19 based on estimates from Cande and Kent (1995; CK95), Ogg and Smith (2004; GPTS 2004), Pälike et al., (2006; P06), Ogg (2012; GPTS 2012), Pacific Equatorial Age Transect (PEAT; this study), and combined ODP Sites 1052 and 1260 (this study). Orange lines track changes between different estimates. Calibration points with error bar used by CK95, GPTS2004 and GPTS2012 are plotted in red dots. Also given is the respective absolute age of the Eocene-Oligocene boundary (E-O; blue line) and the long eccentricity cycle number for reference (see Supplement Fig. S8).
Figure 9 Comparison of magnetochron boundary ages and durations for Chron C12 to C19 based on estimates from Cande and Kent (1995; CK95), Ogg and Smith (2004; GPTS 2004), Pälike et al., (2006; P06), Ogg (2012; GPTS 2012), Pacific Equatorial Age Transect (PEAT; this study), and combined ODP Sites 1052 and 1260 (this study). Orange lines track changes between different estimates. Calibration points with error bar used by CK95, GPTS2004 and GPTS2012 are plotted in red dots. Also given is the respective absolute age of the Eocene-Oligocene boundary (E-O; blue line) and the long eccentricity cycle number for reference (see Supplement Fig. S8).CC-BY · From the PDF
Figure 10 Tuned bulk and benthic stable carbon isotope data plotted against La2011 orbital solution for eccentricity (Laskar et al., 2011b). Bulk data: 1218 (gray; Pälike et al., 2006), U1333 (green; this paper; Wilson et al., unpublished; Leon-Rodriquez and Dickens, 2013), U1334 (red; this paper; Wilson et al., unpublished). Benthic data: 1218 (black; Lear et al., 2004; Coxall et al., 2005; Tripati et al., 2005; Coxall and Wilson, 2011), 1260 (blue; Edgar et al., 2007). Long eccentricity (405 kyr) band pass filters of the detrended, tuned records are plotted on top La2011 (dash line). Magnetostratigraphy as provided in Table 1 and combined core images from Site U1333, U1334, and 1218 for illustration.
Figure 10 Tuned bulk and benthic stable carbon isotope data plotted against La2011 orbital solution for eccentricity (Laskar et al., 2011b). Bulk data: 1218 (gray; Pälike et al., 2006), U1333 (green; this paper; Wilson et al., unpublished; Leon-Rodriquez and Dickens, 2013), U1334 (red; this paper; Wilson et al., unpublished). Benthic data: 1218 (black; Lear et al., 2004; Coxall et al., 2005; Tripati et al., 2005; Coxall and Wilson, 2011), 1260 (blue; Edgar et al., 2007). Long eccentricity (405 kyr) band pass filters of the detrended, tuned records are plotted on top La2011 (dash line). Magnetostratigraphy as provided in Table 1 and combined core images from Site U1333, U1334, and 1218 for illustration.CC-BY · From the PDF

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Cited by

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Metadata

Authors
Westerhold, T., Röhl, U., Pälike, H., Wilkens, R., Wilson, P. A., & Acton, G.
ORCID
Venue
Climate of the Past
Publisher
Copernicus GmbH
Published
2014-05-16
Volume
10
Issue
3
Pages
955-973
ISSN
1814-9332
DOI
10.5194/cp-10-955-2014
Cited by
72
References
1
Language
en
Licence
creativecommons.org/licenses/by/3.0/ (vor)

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