adsabs/AstroCLIMB huggingface dataset:
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: Fits to the 1180 Å (top) and UVW2 (bottom) light curves found using JAVELIN (left) and PYROA (right). JAVELIN can only achieve a good fit by introducing unrealistic large-amplitude, short-timescale variability. PYROA achieves a good fit by significantly inflating the 1180 Å error bars, but the model still does not match all the peaks and troughs in the light curves. The failure of both methods is a consequence of analyzing light curves that are not simply shifted, smoothed, and scaled versions of each other.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Schematic diagram of an LPDA (not to scale).
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: Fits to the detrended 1180 Å (top) and UVW2 (bottom) light curves using JAVELIN (left) and PYROA (right). The dashed line shows the detrending light curve. Significantly improved fits are achieved with both JAVELIN and PYROA once the light curves are detrended.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: The UV/optical SED of Mrk 817 during AGN STORM 2. The variable (rms, black circles) spectrum approximately follows f  ν  ∝ λ −1/3 as expected for an accretion disk. The constant component is shown as orange squares. The purple circles show the maximum, mean, and minimum SED. Error bars are plotted, but are mostly smaller than the symbols.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: HST/STIS spectrum of Mrk 817 from 2021 April 18 compared to the Swift filter transmission curves. Several strong broad emission lines fall within the Swift filters.
Paper: AGN STORM 2. IV. Swift X-Ray and Ultraviolet/Optical Monitoring of Mrk 817
Authors: Edward M. Cackett, Jonathan Gelbord, Aaron J. Barth, Gisella De Rosa, Rick Edelson, Michael R. Goad, Yasaman Homayouni, Keith Horne, Erin A. Kara, Gerard A. Kriss, Kirk T. Korista, Hermine Landt, Rachel Plesha, Nahum Arav, Misty C. Bentz, Benjamin D. Boizelle, Elena Dalla Bontà, Maryam Dehghanian, Fergus Donnan, Pu Du, Gary J. Ferland, Carina Fian, Alexei V. Filippenko, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Jelle Kaastra, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Yan-Rong Li, Jacob N. McLane, Missagh Mehdipour, Jake A. Miller, John Montano, Hagai Netzer, Christos Panagiotou, Ethan Partington, Luka Č. Popović, Daniel Proga, Daniele Rogantini, David Sanmartim, Matthew R. Siebert, Thaisa Storchi-Bergmann, Marianne Vestergaard, Jian-Min Wang, Tim Waters, Fatima Zaidouni
Figure caption: Top: the normalized UVW2 (red) and 1180 Å (blue) light curves. Bottom: the difference between the normalized UVW2 and 1180 Å fluxes (red) as compared to the strength of the UV absorption, as measured by the EW of the broad Si IV absorption trough (blue).
Paper: Fast Gravitational-wave Parameter Estimation without Compromises
Authors: Kaze W. K. Wong, Maximiliano Isi, Thomas D. P. Edwards
Figure caption: Cumulative distribution of the quantile of which the true value lies for each marginalized distribution. The shadow band denotes the 95% credible interval drawn from a uniform distribution with the same number of events as the injection campaign. The legend shows the p-values for each marginalized distribution, with a combined value of p = 0.70.✎
Paper: Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25
Authors: Jiaqi Lin, 家琪 林, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Hui Deng, 辉 邓, Ying Mei, 盈 梅, Xiaojuan Zhang, 小娟 张
Figure caption: The monthly number of SXR flares and SGs from 1982 January to 2022 December. The black line represents the northern hemisphere, and the red line represents the southern hemisphere.
Paper: Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25
Authors: Jiaqi Lin, 家琪 林, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Hui Deng, 辉 邓, Ying Mei, 盈 梅, Xiaojuan Zhang, 小娟 张
Figure caption: The cumulative distribution of α, β, β δ, β γ, and β γ δ SGs in the northern and southern hemispheres under different solar cycles.
Paper: Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25
Authors: Jiaqi Lin, 家琪 林, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Hui Deng, 辉 邓, Ying Mei, 盈 梅, Xiaojuan Zhang, 小娟 张
Figure caption: The evolution of the total number between various SXR flares and SGs in the northern and southern hemispheres under different cycles, where the left column shows SXR flares and the right column shows SGs.
Paper: Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25
Authors: Jiaqi Lin, 家琪 林, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Hui Deng, 辉 邓, Ying Mei, 盈 梅, Xiaojuan Zhang, 小娟 张
Figure caption: The cumulative distribution of B-class, C-class, M-class, and X-class flares in the northern and southern hemispheres under different solar cycles.
Paper: Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25
Authors: Jiaqi Lin, 家琪 林, Feng Wang, 锋 王, Linhua Deng, 林华 邓, Hui Deng, 辉 邓, Ying Mei, 盈 梅, Xiaojuan Zhang, 小娟 张
Figure caption: The monthly time series of B-class flares and various SGs in the northern (left) and southern (right) hemispheres.
Paper: The Metallicity Variations Along the Chromosome Maps: The Globular Cluster 47 Tucanae 
Authors: A. F. Marino, A. P. Milone, E. Dondoglio, A. Renzini, G. Cordoni, H. Jerjen, A. Karakas, E. P. Lagioia, M. V. Legnardi, M. McKenzie, A. Mohandasan, M. Tailo, D. Yong, T. Ziliotto
Figure caption: Chromosome map of 47 Tucanae from Milone et al. (2017). Gray dots represent the complete sample of RGB stars used to construct the map. Our spectroscopic targets observed with UVES are highlighted with large colored symbols. In particular, green circles are 1P stars, magenta squares are normal 2P stars, and magenta triangles represent candidate anomalous stars. The locations of two RV binaries are indicated by black crosses.
Paper: The Metallicity Variations Along the Chromosome Maps: The Globular Cluster 47 Tucanae 
Authors: A. F. Marino, A. P. Milone, E. Dondoglio, A. Renzini, G. Cordoni, H. Jerjen, A. Karakas, E. P. Lagioia, M. V. Legnardi, M. McKenzie, A. Mohandasan, M. Tailo, D. Yong, T. Ziliotto
Figure caption: From top to bottom, [Fe/H] and absolute chemical abundances for all the α and s elements as a function of the ΔF275W,F814W values on the ChM of 47 Tucanae. The left and right panels represent 1P and 2P stars, respectively. The dashed line on the left panel at ΔF275W,F814W = −0.10 separates the two groups of 1P a  and 1P b  stars (see text for details). The plotted error bars represent the dispersion of the values in each group divided by the square root of the number of stars. Symbols are as in Figure 1.
Paper: The Metallicity Variations Along the Chromosome Maps: The Globular Cluster 47 Tucanae 
Authors: A. F. Marino, A. P. Milone, E. Dondoglio, A. Renzini, G. Cordoni, H. Jerjen, A. Karakas, E. P. Lagioia, M. V. Legnardi, M. McKenzie, A. Mohandasan, M. Tailo, D. Yong, T. Ziliotto
Figure caption: Examples of two portions of FLAMES@UVES spectra including some analyzed Fe and Ca spectral features, plus the Ba line 6496.9 Å. The displayed spectra are relative to stars #11746 and #112499, which have similar atmospheric parameters but different ΔF275W,F814W values. Overall, the spectral features of star #11746 (with higher ΔF275W,F814W) are deeper.
Paper: The Metallicity Variations Along the Chromosome Maps: The Globular Cluster 47 Tucanae 
Authors: A. F. Marino, A. P. Milone, E. Dondoglio, A. Renzini, G. Cordoni, H. Jerjen, A. Karakas, E. P. Lagioia, M. V. Legnardi, M. McKenzie, A. Mohandasan, M. Tailo, D. Yong, T. Ziliotto
Figure caption: Chemical abundances ﹩\mathrm{log}\epsilon ﹩(X) as a function of the ΔF275W,F814W and Δ C F275W,F336W,F438W values on the ChM of 47 Tucanae. The color code is indicative of the Spearman correlation coefficient (r). The coefficients and their associated significance are listed in Table 7.
Paper: The Metallicity Variations Along the Chromosome Maps: The Globular Cluster 47 Tucanae 
Authors: A. F. Marino, A. P. Milone, E. Dondoglio, A. Renzini, G. Cordoni, H. Jerjen, A. Karakas, E. P. Lagioia, M. V. Legnardi, M. McKenzie, A. Mohandasan, M. Tailo, D. Yong, T. Ziliotto
Figure caption: Location of our spectroscopic targets along the ChM of 47 Tucanae from Milone et al. (2017). The color of each star is indicative of the inferred chemical abundances, as illustrated in the color bar. In these two plots we illustrate the chemical pattern of Na and Al abundances relative to Fe.
Paper: The Metallicity Variations Along the Chromosome Maps: The Globular Cluster 47 Tucanae 
Authors: A. F. Marino, A. P. Milone, E. Dondoglio, A. Renzini, G. Cordoni, H. Jerjen, A. Karakas, E. P. Lagioia, M. V. Legnardi, M. McKenzie, A. Mohandasan, M. Tailo, D. Yong, T. Ziliotto
Figure caption: As Figure 3, but for [Fe/H].
Paper: Updated Reference Wavelengths for Si VII and Mg VII Lines in the 272–281 Å Range
Authors: Peter R. Young
Figure caption: (a) An AIA 171 Å image (logarithmic scaling) showing an active region from 2010 September 22. The blue box shows the region rastered by EIS. (b) An EIS image (linear scaling) formed from the Si VII λ275.37 line observed in the raster beginning 11:26 UT. The blue contour shows the spatial region averaged to yield the spectrum from which wavelength measurements were made in the present work. Three adjacent data columns between x = 66″ and x = 72″ are missing in the EIS data and have been interpolated for display purposes.
Paper: Updated Reference Wavelengths for Si VII and Mg VII Lines in the 272–281 Å Range
Authors: Peter R. Young
Figure caption: Line profiles from the 20070221_0115 data set. The spectra are shown in blue, and Gaussian fits to the lines are shown in red. Panel (c) shows the two-Gaussian fit for this blended feature.
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Summary of observational data for 18 Sco. The light gray stripes indicate the approximate regions of magnetic maxima spaced at ≈15 yr intervals. Top panel—calibrated S-index measurements taken from seven different sources. The horizontal dashed line indicates the maximum measured activity level in this period. Middle panel—spectropolarimetric observations of the magnetic field. The red and blue backgrounds represent the expected polarities for a ≈15 yr magnetic cycle. Bottom panel—differing levels of processing applied to the original S-index time series for each analysis: last 30 yr (gray circles), seasonal averages (blue squares), and smoothed interpolation (orange line).
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Overplotted spectra of 18 Sco in the K-line region for each instrument. The colors represent individual spectra for visualization purposes. For instruments with more than 50 spectra in their final sample, only 50 are shown in the plot. Top left—HIRES (250 total spectra). Top right—HARPS (2716 total spectra). Bottom left—NARVAL (70 total spectra). Bottom right—OPD (31 total spectra).
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Global data analysis. (a) GLS periodogram. The dotted horizontal line indicates the level corresponding to a 10% false alarm probability. The corresponding periods of the two peaks above this level are annotated. (b) Θ statistic of PDM (lighter line) and its smoothed version (darker line). The corresponding periods of the two lowest minima are annotated. (c) Phase-folded data at 7.1 yr (primary PDM period). The dashed blue line is the sinusoidal GLS fit at this same frequency, and the red line is a moving average of the folded data. (d) Same as (c), but folded at 14.6 yr (secondary PDM period).
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: The historical sunspot number record smoothed by yearly averages. MM and DM indicate the time periods of the so-called Maunder Minimum and Dalton Minimum, respectively. The odd-cycle maxima are highlighted with arrows to help visualize the Gnevyshev–Ohl pattern. Sunspots were observed avidly with telescopes soon after Galileo called attention to their existence in the Western world. From a historical perspective, we note that if the telescope had been invented about 100 yr later, the Maunder Minimum episode would have been missed entirely.
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: GP regression results based on a sum of two SHO terms (adopted solution). (a) Prediction of the maximum a posteriori model, with a shaded band between the 16th and 84th percentiles. (b) PSD of the process with uncertainties determined by an MCMC. The periods corresponding to the peaks are shown and highlighted. (c) Residuals after subtraction of the MAP predictions. (d) Samples of the oscillation frequency posterior probability distribution for each SHO, obtained via MCMC. The corresponding vertical bands encompass 68% of the posterior mass for these parameters.
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Decomposition of the solar K-line emission index. Left panels—time-domain representation for the original signal x, its trend component r, the identified cyclic components C  k  , and the remaining high-frequency low-amplitude noise. Right panels—corresponding Fourier and Hilbert power spectral densities for each signal. The marginal Hilbert spectrum is used to estimate the frequency distribution of each cyclic component.
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Same as Figure 6, but for the sunspot number time series.
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Same as Figure 6, but for 18 Sco.
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Three representations of the relationship between cycle duration and rotation period (A). Fits from Equation (10) as a function of Ro. (B) Same fits for a fixed value of τ = 12 days and τ = 21 days for the lower branch. (C) Same as panel (B), but on a linear scale. G-type stars are displayed with filled symbols, and F- and K-type stars are shown as open symbols. The circles represent stellar cycles that lie on the inactive branch, while the squares represent either the additional longer cycles for multicyclic stars or monocycle stars lying on the active branch. The Sun (1) and 18 Sco (20), both G-type stars, are indicated with colored stars, with the Schwabe-like component in yellow and the Hale-like component in red. Multiple cycles observed in the same star are connected with vertical dotted lines. Our proposed new fits are displayed with solid lines for two values of convective turnover times corresponding to G- and K-type stars, while the dashed–dotted lines represent the corresponding variance intervals from changing τ by ±1 day. The data were compiled from Brandenburg et al. (2017) and Boro Saikia et al. (2022).
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Summary of the results after applying our analysis to the S-index data of both stars. The panels show from top to bottom the GLS periodogram, the PDM statistic, the PSD obtained from MCMC sampling a triple-frequency GP model, and the marginal Hilbert spectrum. The colored strips in each panel indicate the confidence intervals for the three main periods found by each method. The vertical black line represents the newly determined third period: (a) 1.42 yr (HD 78366), and (b) 1.74 yr (HD 114710).
Paper: A Hale-like Cycle in the Solar Twin 18 Scorpii
Authors: J.-D. do Nascimento, S. A. Barnes, S. H. Saar, G. F. Porto de Mello, J. C. Hall, F. Anthony, L. de Almeida, E. N. Velloso, J. S. da Costa, P. Petit, A. Strugarek, B. J. Wargelin, M. Castro, K. G. Strassmeier, A. S. Brun
Figure caption: Preprocessed S-index time series taken from Mount Wilson Observatory observations from 1966 to 1995. Blue squares are seasonal averages used by the GLS periodogram and GP regression, and the orange line is a smooth spline interpolation used by the HHT. The panels show both stars: (a) HD 78366, and (b) HD 114710.
Paper: Mass Ratio Estimates for Overcontact Binaries Using the Derivatives of Light Curves
Authors: Shinjirou Kouzuma
Figure caption: Comparison of synthesized LCs (uppermost panel) and their third derivatives (middle panel) for overcontact binaries with l 3 = 0 (purple circles), 0.2 (green triangles), and 0.8 (blue squares), where l 3 is the ratio of the third light to the total light. The top figure corresponds to binaries with i = 90° and q = 0.35, while the bottom figure corresponds to binaries with i = 70° and q = 0.15. The other binary parameters are the same as those shown in Figure 1. The LCs are represented in magnitudes, and the third derivatives are in units of 104 and 103 W m−2 day−3 for the binaries with i = 90° and 70°, respectively. The top (l 3 = 0.8) and bottom (l 3 = 0) curves in the middle panels are shifted by ±2.0 × 104 and ±2.0 × 103 W m−2 day−3 for the binaries with i = 90° and 70°, respectively. The lowermost panel shows the differences between the third derivatives of LCs with and without a third light, where the units are in W m−2 day−3.
Paper: Mass Ratio Estimates for Overcontact Binaries Using the Derivatives of Light Curves
Authors: Shinjirou Kouzuma
Figure caption: Example of a synthetic LC (the uppermost panel) and its first to third derivatives (the second to fourth panels, respectively) for an overcontact binary with q = 0.35, P = 1 day, M p = 1.5 M ⊙, i = 90°, T p = 5000 K, T s = 6000 K, and f = 0.2. The values of the flux and the first to third derivatives are in units of W m−2, 10 W m−2 day−1, 102 W m−2 day−2, and 104 W m−2 day−3, respectively.
Paper: Mass Ratio Estimates for Overcontact Binaries Using the Derivatives of Light Curves
Authors: Shinjirou Kouzuma
Figure caption: The relation between W (Equation (1)) and mass ratio q, calculated from our synthesized LCs (see Section 2). The red, green, blue, and brown crosses represent binaries with i = 90°, 80°, 70°, and 60°, respectively. The solid line is the regression line, accompanied by a pair of parallel dashed lines for reference, with mass ratios larger and smaller by 0.1 than the regression line.