adsabs/AstroCLIMB huggingface dataset:
Paper: Methods for the Detection of Stellar Rotation Periods in Individual TESS Sectors and Results from the Prime Mission
Authors: Isabel L. Colman, Ruth Angus, Trevor David, Jason Curtis, Soichiro Hattori, Yuxi (Lucy) Lu
Figure caption: TESS single-sector light curve for TIC 137555668 (sector 14), dominated by noise, with no visually discernible signal of any kind. The bottom panels show the LS periodogram, two-term LS periodogram, and ACF of the light curve. Peaks A, B, and C are marked by vertical highlights of decreasing width. Note that the LS peaks are very low amplitude and close to the noise level; also note the lack of periodic pattern in the ACF.
Paper: Methods for the Detection of Stellar Rotation Periods in Individual TESS Sectors and Results from the Prime Mission
Authors: Isabel L. Colman, Ruth Angus, Trevor David, Jason Curtis, Soichiro Hattori, Yuxi (Lucy) Lu
Figure caption: TESS single-sector light curve for TIC 1271268578 (sector 21), a marginal case with a period visible close to the noise level. The bottom panels show the LS periodogram, two-term LS periodogram, and ACF of the light curve. Peaks A, B, and C are marked by vertical highlights of decreasing width. Note the lack of clarity in the ACF, and the two-term LS detection of the double period. As will be discussed in Section 3.1, this star is in fact a “double-dipper.” Due to the high noise level, the single-term LS does not detect the correct period in this case, though the sector does pass both classifiers as a detection of rotation.
Paper: Methods for the Detection of Stellar Rotation Periods in Individual TESS Sectors and Results from the Prime Mission
Authors: Isabel L. Colman, Ruth Angus, Trevor David, Jason Curtis, Soichiro Hattori, Yuxi (Lucy) Lu
Figure caption: TESS single-sector light curve for TIC 58365762 (sector 19), exhibiting a clear signal of stellar rotation. The bottom panels show the LS periodogram, two-term LS periodogram, and ACF of the light curve. Peaks A, B, and C are marked by vertical highlights of decreasing width, which are colored to guide the eye and make them distinct from the plotted functions.
Paper: Methods for the Detection of Stellar Rotation Periods in Individual TESS Sectors and Results from the Prime Mission
Authors: Isabel L. Colman, Ruth Angus, Trevor David, Jason Curtis, Soichiro Hattori, Yuxi (Lucy) Lu
Figure caption: Left: period accuracy in the training set for Classifier #2, with O18 periods plotted on the x-axis and detections from this work on the y-axis. Periods classified as accurate for training purposes are shown in the darker color. Right: failure modes used to select accurate periods in the training set, with the unused failure modes also highlighted. We expect that ground-truth periods lying along these lines are likely aliases, due to the systematic feature at 1 day from Earth’s rotation.
Paper: Methods for the Detection of Stellar Rotation Periods in Individual TESS Sectors and Results from the Prime Mission
Authors: Isabel L. Colman, Ruth Angus, Trevor David, Jason Curtis, Soichiro Hattori, Yuxi (Lucy) Lu
Figure caption: Flowchart describing the pipeline used in this work to detect rotation periods in single TESS sectors.
Paper: Methods for the Detection of Stellar Rotation Periods in Individual TESS Sectors and Results from the Prime Mission
Authors: Isabel L. Colman, Ruth Angus, Trevor David, Jason Curtis, Soichiro Hattori, Yuxi (Lucy) Lu
Figure caption: Two TESS light curves with points colored by time for comparison to folded versions, which are presented in the panels below. The left folded light curve is phased on the period detected by a LS periodogram in our pipeline, and the right is phased on twice that period. This allows us to visually identify double-dippers. For the first star (TIC 12359079, sector 2), the double-period phase curve has two peaks of equal flux, which suggests that the original period is in fact correct. For the second star (TIC 1126556, sector 22), the two peaks in the double-period curve are at different heights, which suggests that we are observing a double-dipping pattern. Indeed, the initial LS measurement for this star was flagged by our pipeline as being a likely half-period.
Paper: LHS 475 b: A Potential Venus Analog Orbiting a Nearby M Dwarf
Authors: Kristo Ment, David Charbonneau, Jonathan Irwin, Jennifer G. Winters, Emily Pass, Avi Shporer, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Keith Horne, Zahra Essack, Veselin B. Kostov, Michelle Kunimoto, Alan Levine, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: Phase-folded photometry of LHS 475 highlighting the 3 hr window surrounding the planetary transits. Solid lines depict the median model obtained from sampling the posterior distributions whereas the shaded gray areas show the 16th and 84th percentiles. Median values and 1σ uncertainties for the orbital period P and planet radius R are also given. We produce separate subplots for TESS data (top panel), MEarth data (second panel), LCOGT data (third panel), and the combined data set (bottom panel). The combined model is used for the values in Table 2.
Paper: LHS 475 b: A Potential Venus Analog Orbiting a Nearby M Dwarf
Authors: Kristo Ment, David Charbonneau, Jonathan Irwin, Jennifer G. Winters, Emily Pass, Avi Shporer, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Keith Horne, Zahra Essack, Veselin B. Kostov, Michelle Kunimoto, Alan Levine, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: MEarth-South follow-up photometry of five individual transits of LHS 475. The Barycentric Julian Date values (BJD) within the plots denote the times of transit midpoints. The vertical dashed lines encompass the full transit duration. The solid line depicts the best-fit model for all MEarth data; it is identical to the model in the middle panel of Figure 6 and is further described in Section 5.2. The bottom panel displays the residuals after subtracting the best-fit model from the data.
Paper: LHS 475 b: A Potential Venus Analog Orbiting a Nearby M Dwarf
Authors: Kristo Ment, David Charbonneau, Jonathan Irwin, Jennifer G. Winters, Emily Pass, Avi Shporer, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Keith Horne, Zahra Essack, Veselin B. Kostov, Michelle Kunimoto, Alan Levine, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: Left: relative radial velocities of LHS 475 from CHIRON. The estimated systemic velocity is −10.3 ± 0.5 km s−1. Right: Same as the left panel, with the radial velocities phase-folded at the fitted orbital period of the planet. The black dotted line shows the modeled RV signature of the planet using the estimated semiamplitude of 1.1 m s−1 from Section 6.
Paper: LHS 475 b: A Potential Venus Analog Orbiting a Nearby M Dwarf
Authors: Kristo Ment, David Charbonneau, Jonathan Irwin, Jennifer G. Winters, Emily Pass, Avi Shporer, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Keith Horne, Zahra Essack, Veselin B. Kostov, Michelle Kunimoto, Alan Levine, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: Combined and phase-folded LCOGT light curves of LHS 475 b. Top: gray symbols show the unbinned data and red symbols show the same data in 5 minutes bins. Bottom: the transit model from a joint fit to all five LCOGT light curves is overplotted on the binned data. The model has a planet-to-star radius ratio ﹩r/R={0.033}_{-0.003}^{+0.002}﹩, consistent with the value from the combined fit in Section 5.4.
Paper: LHS 475 b: A Potential Venus Analog Orbiting a Nearby M Dwarf
Authors: Kristo Ment, David Charbonneau, Jonathan Irwin, Jennifer G. Winters, Emily Pass, Avi Shporer, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Keith Horne, Zahra Essack, Veselin B. Kostov, Michelle Kunimoto, Alan Levine, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: TESS photometry of LHS 475 in Sectors 12, 13, 27, and 39. The black line represents the fitted baseline as described in Section 3.1.
Paper: LHS 475 b: A Potential Venus Analog Orbiting a Nearby M Dwarf
Authors: Kristo Ment, David Charbonneau, Jonathan Irwin, Jennifer G. Winters, Emily Pass, Avi Shporer, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Keith Horne, Zahra Essack, Veselin B. Kostov, Michelle Kunimoto, Alan Levine, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: Speckle imaging sensitivity curves of LHS 475 utilizing the 562 nm (blue line) and 832 nm (red line) bandpasses. No nearby light sources are detected.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: The long-term (from RECONS) and midterm (from TESS) changes in irradiance are shown for the 46 exoplanets (excluding Earth) reported to be orbiting the 22 ATLAS stars for which we have both 0.9 m telescope and TESS data. Irradiance changes are expressed in units of erg s–1 cm–2, calculated for the stars using BT-Settl model stellar fluxes at the planetary orbital distances and using the variability measurements in the respective filters of observation as given in Table 1 (described in detail in Section 6.2). Points are colored by their reported orbital semimajor axis. A black circle denotes that the exoplanet lies in the HZ at a distance appropriate for liquid water to exist. The gray lines (solid, dashed, and dotted–dashed) are, respectively, the 1:1, 1:2, and 2:1 comparison lines between the long-term variability and midterm variability.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: The decade+ stellar variability of 32 ATLAS targets observed by RECONS in the VRI filters (blue, green, and orange, respectively) at the CTIO 0.9 m telescope and the ∼month variability observed by TESS (averaged over multiple sectors, if available) are shown. The IDR noise floor (horizontal gray dashed line) is set at 10 mmag for RECONS, determined using observations of photometrically stable white dwarfs, whereas the noise floor for TESS is ∼1 mmag. Nine data points with a TESS IDR < 0 are targets for which TESS data are unavailable due to their locations along the ecliptic and represent “N.O.” values in Table 1. Note that the y-axis extends to 100 mmag while the x-axis extends to 30 mmag. The blue line traces 1:1 equal variability on both timescales. As shown in Kopp (2016), the Sun’s total solar irradiance varies by 0.1%, which would place it in the region near 1 mmag on both axes, assuming the same variations in our filters.
Paper: The Solar Neighborhood LI: A Variability Survey of Nearby M Dwarfs with Planets from Months to Decades with TESS and the CTIO/SMARTS 0.9 m Telescope
Authors: Aman Kar, Todd J. Henry, Andrew A. Couperus, Eliot Halley Vrijmoet, Wei-Chun Jao
Figure caption: From TESS, 23 of 32 ATLAS targets were identified whose light curves are shown here and all the variability metrics are reported respectively in Table 1. TESS sectors have spatial overlap, and therefore some targets have multiple light curves. The missing targets are a consequence of their location along the ecliptic, which the TESS primary mission did not observe. For the unpopular fluxes, LP 771–95A and L 34–26 were reduced without the polynomial (purple) applied while the rest included the polynomial (red). No SPOC fluxes were available for GJ 667C. The light curves are ordered by R.A. from left to right and top to bottom. The color code and zero y-axis values are the same as in Figure 3.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Color–magnitude diagram in the Maunakea Observatories passbands for substellar objects as in Kuzuhara et al. (2022) but adding photometry for HIP 99770 b (Currie et al. 2023b) and HIP 39017 b (this work). Teal triangles denote young or low-surface-gravity MLT dwarfs (Leggett et al. 2010; Dupuy & Liu 2012; Best et al. 2020) using distances from Best et al. (2020). HIP 99770 b (Currie et al. 2023b) and substellar companions HIP 21152 B (Kuzuhara et al. 2022) and HD 33632 Ab (Currie et al. 2020a) are included for comparison, as well as a selection of other planets and brown dwarf companions denoted by indigo error bars: GJ 504 b (Janson et al. 2013; Kuzuhara et al. 2013), HD 95086b (De Rosa et al. 2016), 51 Eri b (Rajan et al. 2017; Best et al. 2020), 2M1027 b (Dupuy & Liu 2012; Best et al. 2020), β Pic b (Dupuy & Liu 2012; Best et al. 2020), 1RXS J160929.1-210524B (Dupuy & Liu 2012; Best et al. 2020), and κ And b (Dupuy & Liu 2012; Best et al. 2020), all using distances from Bailer-Jones et al. (2021). Indigo error bars with filled circles are the HR 8799 planets (Skrutskie et al. 2006; Marois et al. 2008; Metchev et al. 2009; Currie et al. 2014; Skemer et al. 2014; Zurlo et al. 2016; Skrutskie et al. 2019).
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Select Sonora Diamondback (Morley et al. 2024) model spectra, smoothed to R = 50 at 2.65 μm, overplotted with the HIP 39017 b observations. Left: the best-fit Sonora Diamondback spectra with each metallicity provided in the spectral grid. The T eff, [M/H], and ﹩{\chi }_{\nu }^{2}﹩ for each model are given in the legend. All three best-fit spectra have ﹩\mathrm{log}g=4.0﹩. Right: model spectra with the same T eff (1300 K), log(g) (4.0), and [M/H] (0.0) as the best-fit spectrum, but showing variation with the cloud prescription. Each spectrum’s f sed value (or “nc” for no clouds) and its corresponding ﹩{\chi }_{\nu }^{2}﹩ are given in the legend.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: The four smoothed and binned, best-fit SpeX Prism spectra (in color) compared to the HIP 39017 b broadband CHARIS spectrum from 2022 December (black), plotted with vertical offset for visualization. Uncertainties on the SpeX Prism library spectra are plotted, but error bars appear small compared to the marker size due to CHARIS’s larger spectral resolution. NIR spectral types are as given in the SpeX Prism library (Burgasser et al. 2004; Looper et al. 2007; Burgasser et al. 2008, 2010).
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Color–magnitude diagram drawn from Gaia DR3 photometry. We overplot PARSEC isochrones (Bressan et al. 2012) appropriate for the Pleiades (t ∼ 115 Myr; dark gray line) and Hyades (t ∼ 750 Myr; red line), add photometry for Pleiades and Hyades members, stars in the 400 Myr old Ursa Majoris association (blue stars; Jones 2016), young stars with CHARA-constrained radii and ages (magenta triangles; Jones 2016), and stars orbited by directly imaged planets: 51 Eri, HR 8799, and HIP 99770. HIP 39017's position lies very close to that of 51 Eri and HR 8799.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Maps of the ﹩{\chi }_{\nu }^{2}﹩ derived from fitting the HIP 39017 b spectrum to the Sonora Diamondback (Morley et al. 2024) model spectrum grids as a function of model ﹩\mathrm{log}g﹩ and T eff. Columns of subfigures show the three available metallicities: [M/H] = −0.5 (left column), 0.0 (middle column), and +0.5 (right column). Rows of subfigures show four of the six different cloud prescriptions: f sed = 1 (top row), 3 (second row), 4 (third row), and no clouds (fourth row).
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: CHARIS spectrum of HIP 39017 b extracted from 2022 February (royal blue) and 2022 December (orange) data. Because of its slightly higher S/N and lower levels of residual speckle contamination in the J band, we focus our analysis on the December spectrum.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption:                       ﹩{\chi }_{\nu }^{2}﹩ of each SpeX Prism template spectrum fit to the HIP 39017 b CHARIS spectrum vs. its NIR spectral type as given in the SpeX Prism library. Template spectra with “peculiar” NIR spectral type are shown as diamonds. Dotted lines indicate the ﹩{\chi }_{\nu }^{2}﹩ values that correspond to the 1, 2, and 3σ confidence intervals, from bottom to top.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Detections of HIP 39017 b (denoted with arrows) with SCExAO/ CHARIS IFS data at 1.1–2.4 μm (left, middle panels) and Keck/NIRC2 in the ﹩L^{\prime} ﹩ filter at 3.78 μm (right).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Evolution of fundamental solar system frequencies. The g and s frequencies (in arcsec yr −1 = ″ yr −1) were determined from our solar system integrations using FFT over consecutive 20 Myr intervals and Earth’s k and q variables (see Section 2). The g and s modes are loosely related to the apsidal and nodal precession of the planetary orbits (see Figure A1). Solutions including σ 12-resonance intervals (∼40%) are highlighted in color, the remaining solutions are displayed in gray. The frequencies g 1, s 1, and s 2 drift most strongly over time owing to chaotic diffusion. In addition, g 2 shows large and rapid shifts (spikes) at specific times when the spectral g 2 peak splits into two peaks at significantly reduced power during σ 12-resonance episodes (see Figure 5). Alternating maximum power between the two peaks then causes the spikes in g 2. As a result, g 25 = (g 2 − g 5) is unstable and weak/absent during σ 12-resonance intervals (see Figure B1). g 5, g 6, and s 6 (dominated by Jupiter and Saturn) are practically stable over 3.5 Gyr (s 5 is zero due to conservation of total angular momentum/existence of an invariable plane, see Figure A1).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Earth’s orbital eccentricity from ensemble integrations. (a) Eccentricity pattern in the recent past (last 20 Myr) with short and long (∼100 and ∼405 kyr) cycles (nearly identical in all solutions). Note the strong bundling of four short cycles into one long cycle (highlighted by 405 kyr filter). Panels (b), (c), (d) display examples of solutions during σ 12-resonance intervals. (b) Solution R28 (Run 28) over a 20 Myr interval centered at t = −1450 Myr. The LEC is virtually absent and the eccentricity pattern is unrecognizable compared to (a). (c) Solution R06 over a 20 Myr interval centered at t = −1180 Myr. In addition to a weak LEC, the maximum eccentricity is reduced to ∼0.04, which affects the total insolation Earth receives over one year (see text). (d) Solution R44 over a 20 Myr interval centered at t = −528 Myr; the LEC is present but weak relative to the short eccentricity cycle.
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Fast Fourier transform (FFT ﹩={ \mathcal F }(e)﹩) over 20 Myr intervals of Earth’s orbital eccentricity. Frequencies in arcsec yr −1 = ″ yr −1. (a) Standard spectrum in the recent past centered at t = −10 Myr (nearly identical in all solutions). Note the dominant (g 2−g 5) 405 kyr LEC. (b) and (c) Spectra of solutions R06 (Run 06) and R45 during σ 12-resonance episodes (see Section 3) centered at t = −1180 Myr and t = −3260 Myr, respectively. Note the unrecognizable spectrum pattern in (c) compared to (a) and the reduced/absence of power around the LEC frequency of ∼3.″2 yr −1 (∼405 kyr) in (b) and (c). The peaks around 10–13″ yr −1 are due to the short eccentricity cycle.