adsabs/AstroCLIMB huggingface dataset:
Paper: The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Trevor Z. Dorn-Wallenstein, Emily M. Levesque, James R. A. Davenport, Kathryn F. Neugent, Brett M. Morris, K. Azalee Bostroem
Figure caption: Upper left: scatter plot showing the dominant frequency in each FYPS as a function of effective temperature, after filtering out stars with more than ten frequencies or with any frequencies above 10 day−1. Upper right: similar, but for dimensionless frequencies calculated by multiplying the observed frequencies for each star by an estimated dynamical timescale based on the star’s position in the HR diagram, assuming a mass of 15 M ⊙. Center left: a KDE showing the distribution of observed FYPS frequencies for the same sample as a function of effective temperature. The KDE has been scaled by the distribution of FYPS in temperature space to highlight the distribution of FYPS frequencies. Center right: similar, but for the dimensionless frequencies. For both lower panels, we show the shape of the KDE kernel in the space as a white ellipse, and a vertical line at ﹩\mathrm{log}{T}_{\mathrm{eff}}=3.8﹩ showing where H− opacity begins to contribute significantly to the opacity of stellar atmospheres. To the left of this line, stellar envelopes are radiative, while to the right, stars begin to develop increasingly deep convective envelopes. This physical transition corresponds to a difference in the observed properties of FYPS pulsations. Bottom: frequencies recovered by iterative prewhitening of four example FYPS. Red points show a cool FYPS with high pulsational frequencies, and brown points show a warm FYPS with low pulsational frequencies. Two FYPS at ﹩\mathrm{log}{T}_{\mathrm{eff}}\approx 3.8﹩ are shown, both with frequencies spanning the range of those seen in FYPS, but one with a low dominant frequency (purple), and one with a high dominant frequency (orange). The y-coordinate is an arbitrary value to separate each star’s frequencies, and black pluses indicate the dominant frequency in each star. We highlight the locations of these stars in the upper panels with correspondingly colored star markers.
Paper: The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Trevor Z. Dorn-Wallenstein, Emily M. Levesque, James R. A. Davenport, Kathryn F. Neugent, Brett M. Morris, K. Azalee Bostroem
Figure caption: Progenitor properties of 13 SNe II-P/II-L compiled by Smartt (2015) in filled red circles, and five SNe IIb, with properties inferred by pre-explosion imaging and compiled by Yoon et al. (2017, and references therein) in open purple squares, and properties from detailed binary stellar evolution modeling from Gilkis & Arcavi (2022) in open blue triangles. Black dashed lines link the properties of the progenitors of individual SNe inferred by each method. The stars we identify as FYPS are plotted as green stars, with the minimum FYPS luminosity of ﹩\mathrm{log}L/{L}_{\odot }=5.0﹩ shown as a dashed goldenrod line. The properties of supernovae progenitors and the transition from SNe II-P/II-L to SNe IIb compare favorably with the minimum luminosity of FYPS.
Paper: The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Trevor Z. Dorn-Wallenstein, Emily M. Levesque, James R. A. Davenport, Kathryn F. Neugent, Brett M. Morris, K. Azalee Bostroem
Figure caption: Similar to Figure 4, showing the distribution of contaminant objects in our sample. Left panel: the contaminant fraction f cont shown as a function of location in the HR diagram, with f cont increasing from blue to yellow. Right panel: an estimate of the statistical significance of the structures seen in the left panel. The fraction of simulated f cont values drawn from 10,000 bootstrap simulations whose value is less than the true value of f cont, ﹩{f}_{\lt {f}_{\mathrm{cont}}}﹩, with ﹩{f}_{\lt {f}_{\mathrm{cont}}}﹩ increasing from red to blue. Regions in dark blue/red are statistically significant under/overdensities of contaminant objects.
Paper: The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Trevor Z. Dorn-Wallenstein, Emily M. Levesque, James R. A. Davenport, Kathryn F. Neugent, Brett M. Morris, K. Azalee Bostroem
Figure caption: (a) Lightcurves and residual power spectra for LMC stars identified as FYPS. The top panels show the normalized TESS PDCSAP lightcurve as black points, with a 10 minute rolling median in green. The bottom panels show the corresponding Lomb–Scargle periodogram, normalized by Equation (1) using best-fit parameters derived following Dorn-Wallenstein et al. (2020). Frequencies identified via prewhitening are shown as vertical dashed lines; frequencies associated with nearby contaminants are shown in red, while frequencies associated with the star itself are shown in gray. 1 of 2 images
Paper: The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Trevor Z. Dorn-Wallenstein, Emily M. Levesque, James R. A. Davenport, Kathryn F. Neugent, Brett M. Morris, K. Azalee Bostroem
Figure caption: Top: histogram showing the number of FYPS from which a given number of frequencies have been extracted. Bottom: number of frequencies extracted via prewhitening vs. the highest (blue) and lowest (orange) extracted frequency, with lines connecting points belonging to the same star. Stars with only one frequency are shown as black points. The majority of FYPS have 10 or fewer frequencies spanning approximately 0.1–10 day−1.
Paper: The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Trevor Z. Dorn-Wallenstein, Emily M. Levesque, James R. A. Davenport, Kathryn F. Neugent, Brett M. Morris, K. Azalee Bostroem
Figure caption: Similar to Figure B1 for FYPS identified in the SMC.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Evolution of the luminous X-ray AGN fraction from z = 0 to ∼3. The fractions at z = 0.25 are computed by Martini et al. (2013) from combining the sample of Martini et al. (2009) and Haines et al. (2012). The data point at z = 0.75 is computed by Martini et al. (2009). The data point at z = 1.26 is calculated by Martini et al. (2013). Points at z = 2.3 and 3.09 are AGN fractions in protocluster computed by Digby-North et al. (2010) and Lehmer et al. (2009). The green arrows and circle indicate the upper limits and values of X-ray AGN fractions of <2.7%, <4.4%, and 7.0﹩{}_{-3.0}^{+4.8}﹩% in our ELGs at z ∼ 0.24, 0.63, and 1.19, respectively.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: The BPT diagram of 42 Hα emitters covered by the zCOSMOS survey (Lilly et al. 2009). The black solid and dotted lines show the traditional BPT diagram separation lines (Baldwin et al. 1981; Kewley et al. 2006). The red, blue, and green colors are represented the BPT-selected star-forming galaxies, the composite sample, and the BPT-selected AGN, respectively.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Examples of measurement of Hβ, [O III], Hα, and [N II] emission lines derived from the zCOSMOS spectra. The integrating regions of each emission lines are marked in blue and green shadows.
Paper: On the Origin of the Strong Optical Variability of Emission-line Galaxies
Authors: Ruqiu Lin, Zhen-Ya Zheng, Weida Hu, Chunyan Jiang, Xiang Pan, Chenwei Yang, Fang-Ting Yuan, P. T. Rahna, Jian-Guo Wang, Yibo Wang, Ning Jiang, Shuairu Zhu
Figure caption: Image cutouts of five var-ELGs. All stamps are in a size of 5″ × 5″. Columns 1–2: NB816 and ﹩i^{\prime} ﹩ band with SC; Columns 3–4: NB816 and i band with HSC; Column 5: HST/F814W band. The circles with white dashed lines have 3″ diameters.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: The 33 GHz continuum luminosity of nuclei in GOALS-ES and BM17 vs. AGN diagnostics in the X-ray ((a) and (b)) and MIR ((c) and (d)). (a): X-ray hardness ratios (HRs) measured by Iwasawa et al. (2011) and Torres-Albà et al. (2018) using Chandra observations, defined as HR = (H − S)/(H + S), where H is the hard-band (2–7 keV) flux, and S is the soft-band (0.5–2 keV) flux. The dotted horizontal line marks the empirical threshold above which the nucleus is considered to host an AGN due to excess hard X-ray emission (pink shaded area). (b): X-ray luminosity at 2–10 keV from Iwasawa et al. (2011) and Torres-Albà et al. (2018), corrected for galactic extinction. The gray shaded area represents the radio/X-ray luminosity ratio range for radio-quiet AGNs from Panessa et al. (2019; i.e., ν L  ν /L 2–10 keV= 10−2–10−4, ν = 90–100 GHz), assuming the luminosities at 33 and 100 GHz are similar. The black dashed line represents the 1.4 GHz radio/X-ray luminosity ratio for star-forming galaxies from Ranalli et al. (2003; i.e., ﹩\mathrm{log}{L}_{2\mbox{--}10\,\mathrm{keV}}=\mathrm{log}{L}_{1.4}+11.12﹩), assuming α 1.4–33 ∼ α 15–33 ∼ −0.65, as measured among “AGN/SBnuc” in this work. (c): the 6.2 μm PAH equivalent widths (EWs) measured by Stierwalt et al. (2013) using Spitzer observations. The horizontal dotted line marks the empirical threshold, 0.27 μm, below which the MIR nuclear emission is considered to be dominated by AGNs (pink shaded area). The green shaded area represents the empirical range (0.27–0.54 μm) where the nuclear emission is considered to have some but nondominant AGN contribution, and nuclei in the yellow shaded area are considered to be starburst-dominated and have low to no AGN contribution on kiloparsec scales. (d): The MIR slope from Stierwalt et al. (2013), defined as the logarithmic flux density ratio between 30 and 15 μm. The gray shaded area represents the range spanned by the majority of LIRGs in GOALS. In all panels, filled symbols represent ULIRGs, and systems with [Ne V] 14.3 μm, Fe K 6.4 keV, and hard (>10 keV) X-ray detections reported in Petric et al. (2011), Iwasawa et al. (2011), Torres-Albà et al. (2018), and Ricci et al. (2021) are marked with square symbols in red, black, and blue, respectively, with increasing sizes. Nuclei with the highest L 33 also have higher observed L 2–10 keV, the smallest 6.2 μm PAH EW, and steepest MIR, suggesting (dust-obscured) AGN contribution to the 33 GHz emission in “AGN” and “AGN/SBnuc” regions.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: 33 GHz luminosity L 33 (left) and surface density ﹩{{\rm{\Sigma }}}_{{L}_{33}}﹩ (right) vs. effective radius for 95 native regions from GOALS-ES (filled symbols) and of additional 23 native regions characterized using observations of the most luminous U/LIRGs from Barcos-Muñoz et al. (2017, hereafter BM17; unfilled symbols). In both panels, we show “AGN” (magenta triangle), “AGN/SBnuc” (green circles), “SBnuc” (yellow diamonds), and “SF” regions (blue squares). Regions classified as “Jet” or “Ud” are not shown for simplicity. Upper limits in size measurements are indicated with arrows. Dashed gray curves are models for a steady-state radiation feedback-supported maximal starburst disk from Thompson et al. (2005) with assumed molecular gas fraction f  g  = 0.1, 0.3, and 1.0 and stellar velocity dispersion σ = 200 km s−1, as well as for f  g  = 1.0 and σ = 300 km s−1. Solid gray curves show the same models with a modified term to include supernovae feedback, as adopted in Barcos-Muñoz et al. (2017). Compared to “SF” and “SBnuc” regions, “AGN” and “AGN/SBnuc” regions have higher L 33 and ﹩{{\rm{\Sigma }}}_{{L}_{33}}﹩ by up to 3 dex across the entire size range probed, but only the “AGN” in Mrk 231 clearly exceeds the predicted L 33 and ﹩{{\rm{\Sigma }}}_{{L}_{33}}﹩ for a maximally star-forming nuclear disk.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: The 15–33 GHz spectral indices (α 15–33) measured for matched regions identified in nearby star-forming galaxies from the SFRS and local U/LIRGs from GOALS-ES. Left: α 15–33 vs. effective radii, R  e , of the region area used to measure α 15–33. SFRS regions are in gray, and GOALS-ES regions are colored in yellow (“SBnuc”) and blue (“SF”), with extranuclear “SF” regions shown by nonfilled symbols. Upper limits in size are indicated with arrows. Right: distribution of α 15–33 for GOALS-ES regions (hatched black) and for SFRS regions (filled gray). In both panels, the median values for the SFRS (−0.08 ± 0.27) and GOALS-ES regions (−0.46 ± 0.29) are shown in solid gray and dashed black lines, respectively. Overall, α 15–33 spans a wide range for star-forming regions in both local U/LIRGs and normal galaxies, especially at R  e  < 100 pc. Regions in U/LIRGs have steeper median α 15–33 compared with those in nearby normal galaxies, suggesting more dominant nonthermal contribution at 33 GHz.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: The fraction of systems hosting different region types (upper) and nuclear luminosity distribution (lower) vs. merger stage classification of the host system: “a” pre-merging, “b” early-merger, “c” mid-merger, “d” late-merger, and “N” non-merger (Stierwalt et al. 2013). Upper: for each merger stage, the number of galaxies hosting each region type is normalized by the total number of galaxies with the specific merger classification, shown in parentheses on the horizontal axis. Galaxies often host more than one type of region; therefore, the normalized galaxy counts at each merger stage do not add to 1. All native regions identified at 15 or 33 GHz from GOALS-ES are accounted for, excluding “Ud” and “Bg.” Lower: individual values are color-coded by the nuclear region types (“AGN”—magenta, “AGN/SBnuc”—green, and “SBnuc”—yellow), and median values and uncertainties at each merger stage are represented by the solid black lines. The number of systems included at each merger stage is shown in parentheses on the horizontal axis. Only nuclei identified at 33 GHz from GOALS-ES are included. Overall, “AGN” and “AGN/SBnuc” are more frequently found and are more luminous at 33 GHz in the final merger stages.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: SFRs and surface densities vs. effective radii for “SF” and “SBnuc” regions characterized in local U/LIRGs in this work, as well as for star-forming regions in nearby normal galaxies from the SFRS characterized using the same methods outlined in Section 3. Values derived for the SFRS sample are in gray circles. We show values derived both from the total 33 GHz flux ((a) and (b)) and thermal free–free only flux based on the measured 15–33 GHz spectral indices ((c) and (d)). Star-forming clumps and starburst nuclei in the GOALS-ES have up to 3 dex higher SFRs and surface densities compared with star-forming clumps in the SFRS on ∼ 100 pc scales.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: A comparison between radio continuum and Pa α/β as SFR tracer. Upper: continuum-subtracted HST Paα image of NGC 1614 (left) and Paβ image of IRAS F17138-1017 (right) from Larson et al. (2020). Black contours show 33 GHz radio continuum at matched resolutions with 15 GHz continuum, and the matched beams are shown in the lower left corners in black ellipses. Contour levels are 0.075, 0.15, 0.23, and 0.45 mJy beam−1 for NGC 1614, and 0.032, 0.065, and 0.13 mJy beam−1 for IRAS F17138-1017. Lime circles show the apertures used for measuring and comparing radio- and Paα/β-derived SFRs. Lower: the ratio between radio-derived and NIR-derived SFRs for nine U/LIRGs in the sample. The SFRs derived from thermal free–free radio continuum (filled) show better agreement with NIR-derived SFRs than those derived from total 33 GHz continuum (unfilled), and deviations from 1:1 relation (dashed line) are likely due to nuclear dust extinction.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: The distribution of the derived 33 GHz thermal fraction, f th, for 97 matched regions identified at both 15 and 33 GHz (in gray) excluding “Bg,” and for “AGN” (magenta), “AGN/SBnuc” (green), “SBnuc” (yellow), and “SF” regions (blue). The median values are ∼25%, 33%, 71%, and 62%, respectively, and shown in dashed lines. Results for “Jet” and “Ud” regions are not separately shown. While f th spans a wide range for all region types compared, “AGN” and “AGN/SBnuc” have lower median f th than “SBnuc” and “SF” regions.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: MCG +02-20-003. HST Paα image (left), displayed in arcsinh stretch with bilinear interpolation. The yellow square outlines the field of view of the 33 GHz VLA continuum observed with the B-configuration (right), showing bright clumpy nuclear star-forming structures.
Paper: Characterizing Compact 15–33 GHz Radio Continuum Sources in Local U/LIRGs
Authors: Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Muñoz, E. J. Murphy, E. Momjian, T. Díaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S.-Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
Figure caption: IRAS 05442+1732. Left: archival HST 110W image, displayed in arcsinh stretch with bilinear interpolation. The yellow square outlines the field of view of the 33GHz VLA continuum. Middle: 33 GHz VLA continuum observed with the B-configuration. Right: 15 GHz VLA continuum observed with the A-configuration.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Top: Cross correlation between the sample north and south hemispheric sunspot number time series generated by the bootstrap method. Bootstrap for the sunspot number. Bottom left: Histogram of bootstrap-generated cross correlations. Bottom right: Q–Q plot of the generated cross correlation data.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Top left: Morlet wavelet spectra of the northern hemispheric sunspot number data as derived from Figure 12 (top left) to study the nature and evolution of the QBOs (1.2–2.5 yr). Top right: GWPS of the Figure 13 (top left). Middle left: Same as top left, but for the southern hemisphere data. Middle right: GWPS of middle left. Bottom left: Same as top left, but for full-disk data. Bottom right: GWPS of bottom left plot.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Left: Nature of the QBOs (1.2–2.5 yr), isolated from the KO sunspot number data sets. Right: Same as left-side plot but for the KO sunspot group area time series. In both cases, the “blue” curve is for the northern hemisphere, the “green” curve is for southern hemisphere, and the “red” curve indicates the full solar disk.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Same as Figure 8, but for the southern hemisphere.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Same as Figure 8, but for the whole hemisphere.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Display of the QBO length and cycle strength.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Same as Figure 13, but for the sunspot group area data.