adsabs/AstroCLIMB huggingface dataset:
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: Coverage of each major stage of the TESS mission in ecliptic coordinates, including the Prime Mission (Sectors 1–26), first Extended Mission (Sectors 27–55), and planned second Extended Mission (Sectors 56–96). Stars are color-coded by the number of observed sectors, either 1 (red), 2 (orange), 3 (yellow), 4–12 (green), or 13 and greater (blue).
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: Number of planets detected as a function of planet radius from FFI observations only (blue), 2-minute observations only (gray), and both (orange), in each major TESS mission stage, as well as the 7 yr cumulative total.
Paper: Predicting the Exoplanet Yield of the TESS Prime and Extended Missions through Years 1–7
Authors: Michelle Kunimoto, Joshua Winn, George R. Ricker, Roland K. Vanderspek
Figure caption: Simulated planet detections with FFI (left) and 2-minute (right) observations from the PM (top), EM1 (middle), and EM2 (bottom), plotted using a Mollweide projection of ecliptic coordinates. Only new detections are plotted for each mission stage. To improve the visibility of the features, detections from all 100 simulations are included.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Results from Step 2. Cepheid position residuals plotted against TJD, after applying the coefficients A–F from Equations (4)–(7) while solving for Cepheid parallax and proper motion. Large residuals suggest unmodeled η Aql motion, with rms residuals for η Aql (x, y) = (1.8, 1.6 mas). ζ Gem, with no known companion, has rms residuals (x, y) = (1.7, 1.4 mas).
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Results from Step 1. Reference star position residuals from the model of Equations (4)–(7) plotted against TJD for the η Aql and ζ Gem fields. We identify reference stars by Table 7 ID number. Because there are outliers, the equivalent (x, y) rms values have values of 1.1 and 0.8 mas for η Aql, and 1.3 and 1.2 mas for ζ Gem, all larger than the 1σ standard deviations of the Gaussian distribution in Figure 6 for these same residuals.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: The γ-corrected RV (γ corrections produced by the Fourier modeling of pulsational RV, coefficients listed in Table 6), plotted as a function of quadratic phase (Equation (1)). We list the RV sources and associated γ values in Table 5. We color-coded the RV values by Cepheid phase (red = 0 to blue = 1). Residuals are in the upper panel.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Results from Step 1. Histograms of x and y residuals obtained from modeling the FGS observations of each FGS reference frame (for η Aql stars 2, 3, 4, 6; for ζ Gem stars 2, 5, 8, 10, 11; in Figure 4) with Equations (2)–(5). Distributions are fit with Gaussians with standard deviations, σ, indicated in each panel. In addition to fewer reference stars, one entire set of η Aql observations was discarded due to anomalously large residuals.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Residuals (Figure 1, top) to the pulsation-induced RV, modeled by the Fourier coefficients listed in Table 6 plotted as a function of time for the sources listed in Table 5. Errors come from Tables 1–4 and the various published sources in Table 5. RV values are color-coded by Cepheid phase as for Figure 1 (red = 0 to blue = 1). The solid red bars on the zero RV line indicate astrometric coverage from HST/FGS (left) and Gaia EDR3 (right).
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Top: relative positions of η Aql (1, center) and the astrometric reference stars (2, 3, 4, 6). Bottom: relative positions of ζ Gem (1, center) and the astrometric reference stars (2, 5, 8, 10, 11). Table 7 identifies each reference star.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption: Lomb–Scargle periodogram of RV in Figure 2. No peak indicates a false alarm probability less than 61%. The minimum frequency range (maximum period) explored corresponds to roughly 2/3 the total time span of the RV data.
Paper: The η Aquilae System: Radial Velocities and Astrometry in Search of η Aql B
Authors: G. Fritz Benedict, Thomas G. Barnes, Nancy R. Evans, William D. Cochran, Richard I. Anderson, Barbara E. McArthur, Thomas E. Harrison
Figure caption:  B − V variation as a function of phase. Fit is the fifth-order polynomial listed in Table 9. The red dots indicate phases at which we secured FGS astrometry. This fit provides the B − V values used for η Aql and ζ Gem in Equations (4) and (5).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Proper motion offsets vs. parallactic distance for candidate young low-mass stars (G BP − G RP = 1.4–3.4, ∼0.15–1 M ⊙) toward Sco-Cen (top). Candidate members of Sco-Cen have been identified by applying a GMM to these data. I have plotted the resulting candidates that are located within the boundary of Ophiuchus from Esplin et al. (2018; middle) and the candidates that are outside of that boundary and within the triangular area in Upper Sco from Luhman & Esplin (2020; bottom). I have included density contours that encompass the main concentration of candidates in each sample, which serve as criteria for selecting candidate members of these populations.
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption:                       ﹩{M}_{{G}_{\mathrm{RP}}}﹩ vs. G BP − G RP and G − G RP for candidate members of V1062 Sco within a radius of 2° from the center of that group (top) and all candidate members of Sco-Cen (bottom) selected with the kinematic criteria in Figures 1 and 2. To further refine those kinematic candidates, I have defined boundaries that follow the lower envelopes of the sequences in V1062 Sco (red solid lines) and I have rejected candidates that appear below them unless they exhibit mid-IR excess emission, in which case they are retained. For reference, I have indicated the spectral types that correspond to the colors of young stars (Table 4), and I have marked the completeness limits for 2MASS and WISE in J and W1, respectively, based on those colors and a distance of 200 pc, which is just beyond the far side of Sco-Cen (blue dashed lines).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Spatial distribution of candidate members of populations in Sco-Cen based on the kinematic and photometric criteria in Figure 1–3. I have marked the boundaries for Upper Sco, UCL, and LCC from de Zeeuw et al. (1999; dashed lines), the boundary for Ophiuchus from Esplin et al. (2018; green polygon), a field toward the center of Upper Sco defined by Luhman & Esplin (2020; red triangle), the fields encompassing Lupus clouds 1–4 from Luhman (2020; orange ellipses), and a 2° radius field toward V1062 Sco (magenta ellipse).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Same as Figure 1 but for Lupus clouds 1–4 (top), the V1062 Sco group (middle), and UCL/LCC (bottom).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Top: spatial distributions of stars from this work that have kinematics consistent with membership in Upper Sco or Ophiuchus (left) and candidate members of Ophiuchus from Grasser et al. (2021) that have σ  π  < 1 mas (right). I have marked the boundary for Ophiuchus from Esplin et al. (2018; green polygon), a field toward the center of Upper Sco defined by Luhman & Esplin (2020; red triangle), and contours for A  K  = 0.5 from the extinction map of Juvela & Montillaud (2016; magenta curves). Bottom: proper motion offsets vs. parallactic distance for the candidates from Grasser et al. (2021) are shown with the thresholds from Figures 1 and 2 that are used in this work for selecting candidate members of populations in Sco-Cen.
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Histograms of G BP − G RP and G − G RP for the most reliable sample of Sco-Cen candidates (solid lines) and the estimated contamination from field stars (dotted lines). For each color, the candidates are required to have photometric errors of <0.1 mag in both bands, RUWE < 1.6, σ  π  < 0.5 mas, and locations within the Sco-Cen boundaries from de Zeeuw et al. (1999).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Fraction of sources from Gaia EDR3 toward Sco-Cen that have RUWE < 1.6, σ  π  < 0.5 mas, and σ BP < 0.1/σ RP < 0.1 or σ  G  < 0.1/σ RP < 0.1. The data in this diagram provide an estimate of the completeness of samples of candidates in Sco-Cen that are required to satisfy those criteria in order to reduce field star contamination (Sections 2.6 and 3.1).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Equivalent widths of Li vs. spectral type for candidate members of Ophiuchus, Lupus, Upper Sco, and UCL/LCC.
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Top: L X/L bol vs. G BP − G RP for candidate members of Upper Sco from Luhman & Esplin (2020) based on eRASS1 data from Schmitt et al. (2021) and G-band bolometric corrections from Andrae et al. (2018). The latter are available for T eff ≳ 3300 K (G BP − G RP ≲ 2.7). A limit of 0.056 counts s−1 has been assumed for the nondetections. Middle: the candidates from Luhman & Esplin (2020) are plotted in terms of a ratio of X-ray and G RP fluxes (in arbitrary units), which does not require a bolometric correction. Bottom: the same ratio is shown for candidate members of Sco-Cen from this work (Section 2.9).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Histograms of spectral types for candidate members of Upper Sco, Ophiuchus (A  K  < 0.5), V1062 Sco, and UCL/LCC that satisfy the criteria in Section 3.1 (solid histograms). For stars that lack spectroscopy, spectral types have been estimated from photometry (Figure 12, Section 3.2). A second histogram is shown for Upper Sco that includes additional young stars that are absent from the Gaia sample and have been identified in spectroscopic surveys (dotted histogram; Luhman & Esplin 2020 and references therein). The arrows mark the spectral types that correspond to masses of 0.1 and 1 M ⊙ for ages of 10 Myr according to evolutionary models (e.g., Baraffe et al. 1998).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Galactic Cartesian coordinates for candidate members of Sco-Cen (top). The density contours encompass most of the candidates within the fields marked in Figure 4 for Upper Sco, Ophiuchus, Lupus, and V1062 Sco. Candidates that have radial velocities are plotted in diagrams of XYZ and UVW (middle and bottom) if they are within those four fields and are kinematic members of those populations. In addition, kinematic members of UCL/LCC are plotted as blue points if they are within the boundary of LCC from de Zeeuw et al. (1999) and otherwise are plotted as gray points.
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption:                       ﹩{M}_{{G}_{\mathrm{RP}}}﹩ vs. G BP − G RP and G − G RP for candidate late-type (∼K0–M5) members of Upper Sco, V1062 Sco, and UCL/LCC that have σ  π  < 0.1 mas and A  K  < 0.1 and do not have full disks. The boundaries from Figure 3 that were used for selecting candidates have been included (red lines).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Median offsets in ﹩{M}_{{G}_{\mathrm{RP}}}﹩ from the median sequence of UCL/LCC for each candidate member of UCL/LCC from Figure 14 and its six closest neighbors in XYZ. The offsets are defined so that positive values correspond to younger ages. The colors of the points correspond to the values of the ﹩{M}_{{G}_{\mathrm{RP}}}﹩ offsets.
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption:  G RP − J vs. J − H and J − H vs. H − K  s  for candidate members of populations in Sco-Cen as defined in Section 3.1. The intrinsic colors of young stars from B0–M9 are indicated (red lines, Table 4).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Count rate vs. G magnitude for eRASS1 sources from Schmitt et al. (2021) toward Sco-Cen (left) and an area within Sco-Cen toward Upper Sco (right). The typical flux limit adopted for Upper Sco in that study is indicated (dashed line).
Paper: A Census of the Stellar Populations in the Sco-Cen Complex 
Authors: K. L. Luhman
Figure caption: Proper motion offsets vs. parallactic distance for eRASS1 sources toward Sco-Cen from Schmitt et al. (2021) are shown with the thresholds from Figures 1 and 2 that are used in this work for selecting candidate members of populations in Sco-Cen.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: The δ Lyr cluster is ﹩{38}_{-5}^{+6}﹩ Myr old. Top: color−absolute magnitude diagram of candidate δ Lyr cluster members, in addition to stars in IC 2602 (≈38 Myr), the Pleiades (≈115 Myr), and the Gaia EDR3 Catalog of Nearby Stars (gray background). The zoomed right panel highlights the pre-main sequence. The δ Lyr cluster and IC 2602 are approximately the same isochronal age. Bottom: TESS and Kepler stellar rotation period vs. dereddened Gaia color, with the Pleiades and Praesepe (650 Myr) shown for reference (Rebull et al. 2016; Douglas et al. 2017). Most candidate δ Lyr cluster members are gyrochronally younger than the Pleiades; outliers are probably field interlopers.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Phase-folded transit of Kepler 1627Ab with stellar variability removed. Windows over 20 hr (left) and the entire orbit (right) are shown, and the residual after subtracting the transit is in the bottom row. The 2σ model uncertainties and the best-fit model are the light purple band and the dark purple line. Gray points are individual flux measurements; black points bin these into 15 minute intervals and have a representative 1σ error bar in the lower right of each panel. The asymmetric residual during transit is larger than the out-of-transit scatter.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Galactic positions and tangential velocities of stars in the δ Lyr cluster. Points are reported cluster members from Kounkel & Covey (2019). The tangential velocities relative to Kepler 1627 (bottom right) are computed assuming that every star has the same three-dimensional spatial velocity as Kepler 1627. Our analysis considers stars (black points) in the spatial and kinematic vicinity of Kepler 1627 (yellow star). The question of whether the other candidate cluster members (gray points) are part of the cluster is outside our scope. The location of the Sun (⊙) is shown to clarify the direction along which parallax uncertainties are expected to produce erroneous clusters.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Kepler 1627 is a binary. Left: High-resolution imaging from Gemini North/‘Alopeke and Keck/NIRC2 shows an ≈M3V companion at ρ ≈ 0.″16, which corresponds to a projected separation of 53 ± 4 au. The inset shows a cutout of the stacked NIRC2 image (North is up, East is left, and the scale is set by the separation of the binary). The lines show 5σ contrast limits for the ‘Alopeke filters, and 6σ contrast limits for NIRC2 outside of 0.″15. Right: Gaia EDR3 renormalized unit weight error (RUWE) point estimates for candidate δ Lyr cluster members. Since other members of the cluster with similar brightnesses have comparable degrees of photometric variability, the high RUWE independently suggests that Kepler 1627 is a binary.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Kepler’s view of the δ Lyr cluster, shown in equatorial coordinates. Each black circle is a candidate cluster member selected based on its position and kinematics (Figure 1). Of the 1201 candidate cluster members, 58 have at least one quarter of Kepler data. TESS has also observed most of the cluster, for one to two lunar months to date.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Keck/HIRES radial velocities and MuSCAT3 photometry from the transit of 2021 Aug 7. Top: the radial velocity jitter across the 15 minute exposures (σ RV ≈ 30 m s−1) prevented us from detecting the RM effect; a model including the RM anomaly and a quadratic trend in time to fit the spot-induced ≈250 m s−1 trend is shown (see Appendix C). Shaded bands show 2σ model uncertainties. Middle: the RV variations are strongly correlated with varying emission in the Ca H and K lines. Bottom: the photometric transit depths are consistent across the griz bandpasses. The photometry is binned at 10 minute intervals.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Radii, orbital periods, and ages of transiting exoplanets. Planets younger than a gigayear with τ/σ  τ  > 3 are emphasized, where τ is the age and σ  τ  is its uncertainty. Kepler 1627Ab is shown with a star. The large sizes of the youngest transiting planets could be explained by their primordial atmospheres not yet having evaporated; direct measurements of the atmospheric outflows or planetary masses would help to confirm this expectation. Selection effects may also be important. Parameters are from the NASA Exoplanet Archive (accessed 2021 September 15).
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Statistics of interflare arrival times. Twenty-four flares were recorded with amplitudes exceeding 0.5% over the 97.7 days of short cadence observations. The histogram of the time intervals between every possible pair of flares is shown in black. Some plausibly important timescales for star−planet interactions, namely the planetary orbital period and synodic period (the orbital period as seen from the rotating stellar frame) are shown along with their linear combinations. Monte Carlo draws from a Poisson distribution are shown with the gray bands. While peaks in the observed distribution do coincide with some of the “special periods,” the statistical evidence for a non-Poissonian process driving the flares does not clear the 5σ threshold.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Weak evidence for a prograde orbit of Kepler 1627Ab. The time of each Kepler transit was measured, along with the local slope of the light curve. The two quantities might be anticorrelated (≈2σ), which could be caused by starspot crossings during the first (second) half of transit inducing a positive (negative) TTV, provided that the orbit is prograde (Mazeh et al. 2015). The units along the abscissa can be understood by considering that the stellar flux changes by ∼60 ppt per half rotation period (∼1.3 days).
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Transit models and residuals, binned by quartiles in the local slope of the light curve. Representative uncertainties for the black points (binned at 20 minute intervals) are shown in the lower right of each panel. A similar transit asymmetry to that shown in Figure 6 seems to be present in three of the four bins.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Flares in Kepler 1627. Top: the 1 minute cadence Kepler data (black points) are shown with a stellar variability model superposed (blue line). Middle: residual after subtracting the stellar variability model. Flares appear as spikes. Bottom: zooms of the brightest and third-brightest flares. A timing coincidence—that both flares have “successors” approximately one planetary orbital period after the initial event—is emphasized.