adsabs/AstroCLIMB huggingface dataset:
Paper: First Evidence of Intrinsic Alignments of Red Galaxies at z > 1: Cross Correlation between CFHTLenS and FastSound Samples
Authors: Motonari Tonegawa, and Teppei Okumura
Figure caption: Forecast of the angular power spectrum of GG (solid) and GI (lower dashed) terms. The redshift distribution of the shape sample is used to compute them. The GI power spectrum is based on the best-fitting NLA model. The maximum contribution of the GI spectrum within the 95% confidence level is shown as the dotted line.
Paper: First Evidence of Intrinsic Alignments of Red Galaxies at z > 1: Cross Correlation between CFHTLenS and FastSound Samples
Authors: Motonari Tonegawa, and Teppei Okumura
Figure caption: Projected correlation functions ﹩{w}_{g+}({\bar{r}}_{p})﹩ measured with different settings as a diagnosis for systematics. The solid red line is identical to that in Figure 1. The dashed blue line is obtained by using the estimator (3). The dotted red line is the same as the solid red line except that the ellipticity of the shape sample is shuffled.
Paper: A Robust Estimation of Lorentz Invariance Violation and Intrinsic Spectral Lag of Short Gamma-Ray Bursts
Authors: Shuo Xiao, Shao-Lin Xiong, Yue Wang, Shuang-Nan Zhang, He Gao, Zhen Zhang, Ce Cai, Qi-Bin Yi, Yi Zhao, You-Li Tuo, Xin-Qiao Li, Xiang-Yang Wen, Zheng-Hua An, Wen-Xi Peng, Shi-Jie Zheng, Fan Zhang, Li-Ming Song, and Ti-Pei Li
Figure caption: (Top left panel) The Δtobs/(1 + z) as a function of K(z). The yellow region is obtained by fitting Δtobs/(1 + z) = ΔtLIV/(1 + z) + b = aLIVK(z) + b. (Top right panel) The corresponding fit results obtained by MCMC. The correlation coefficient between aLIV and b is −0.996. (Bottom left panel) The yellow region is obtained by fitting Δtobs/(1 + z) = b (i.e., assuming no LIV). (Bottom right panel) The corresponding fit result obtained by MCMC assuming no LIV effect.
Paper: A Robust Estimation of Lorentz Invariance Violation and Intrinsic Spectral Lag of Short Gamma-Ray Bursts
Authors: Shuo Xiao, Shao-Lin Xiong, Yue Wang, Shuang-Nan Zhang, He Gao, Zhen Zhang, Ce Cai, Qi-Bin Yi, Yi Zhao, You-Li Tuo, Xin-Qiao Li, Xiang-Yang Wen, Zheng-Hua An, Wen-Xi Peng, Shi-Jie Zheng, Fan Zhang, Li-Ming Song, and Ti-Pei Li
Figure caption: Spectral lags of SGRBs observed jointly by BAT-GBM are shown in the left panel. The right panel shows the spectral lags of the LGRBs observed by BAT-GECAMB and BAT-GBM. Both are 15–70 keV compared to 120–250 keV in the source rest frame.
Paper: Pulse Peak Migration during the Outburst Decay of the Magnetar SGR 1830-0645: Crustal Motion and Magnetospheric Untwisting
Authors: George Younes, Samuel K Lander, Matthew G. Baring, Teruaki Enoto, Chryssa Kouveliotou, Zorawar Wadiasingh, Wynn C.G. Ho, Alice K. Harding, Zaven Arzoumanian, Keith Gendreau, Tolga Güver, Chin-Ping Hu, Christian Malacaria, Paul S. Ray, and Tod E. Strohmayer
Figure caption: The 0.8–7 keV pulse profile evolution of SGR 1830−0645 with time. The black dotted–dashed, dark-gray dotted, and light-gray solid lines represent the Gaussian centroids of the three peaks during the first day of outburst. A shift, toward the right for the two weaker peaks and the left for the brightest peak, is evident. This shift produces a simpler, nearly sinusoidal, pulse shape four months after outburst onset. The numbers to the right indicate the intervals, in days from outburst onset, that were used to derive each pulse. Adapted from Y21.
Paper: Pulse Peak Migration during the Outburst Decay of the Magnetar SGR 1830-0645: Crustal Motion and Magnetospheric Untwisting
Authors: George Younes, Samuel K Lander, Matthew G. Baring, Teruaki Enoto, Chryssa Kouveliotou, Zorawar Wadiasingh, Wynn C.G. Ho, Alice K. Harding, Zaven Arzoumanian, Keith Gendreau, Tolga Güver, Chin-Ping Hu, Christian Malacaria, Paul S. Ray, and Tod E. Strohmayer
Figure caption: Upper-left panel. The SGR 1830−0645 pulse profile, shown as black points with corresponding uncertainties as solid vertical bars, derived from the first day of NICER observations at outburst onset (i.e., 2020 October 10). The red solid line represents the best-fit four-Gaussian model to the data. Lower-left panel. Residuals from the best-fit model in terms of σ. Right panel. Temporal evolution of the best-fit Gaussian centroids to the three peaks in the SGR 1830−0645 pulse profiles (the corresponding 68% uncertainties are smaller than the symbol size). All three peaks follow a similar linear trend with an absolute rate of about (1.5 ± 0.1) × 10−3 cycle day−1. Note the opposite motion of peak 3, the brightest, compared to the other two. See text for more details.
Paper: Pulse Peak Migration during the Outburst Decay of the Magnetar SGR 1830-0645: Crustal Motion and Magnetospheric Untwisting
Authors: George Younes, Samuel K Lander, Matthew G. Baring, Teruaki Enoto, Chryssa Kouveliotou, Zorawar Wadiasingh, Wynn C.G. Ho, Alice K. Harding, Zaven Arzoumanian, Keith Gendreau, Tolga Güver, Chin-Ping Hu, Christian Malacaria, Paul S. Ray, and Tod E. Strohmayer
Figure caption: Sample dynamic spectral profiles of SGR 1830−0645 derived by fitting 50 phase bins with an absorbed double-blackbody model. Panel tetrads show the integrated fluxes (upper panels) and the νFν photon flux contours in the phase-energy diagram (lower panels) for the warm BB (left) and hot BB (right) spectral components. The time interval for each is noted in the upper-right corner as days from outburst onset. The vertical lines indicate the best-fit Gaussian centroids to the count pulse peaks for each interval. The last row is for two intervals during the post-Sun-constrained period. The analysis is performed for 20 phase bins to increase  S/N. See text for more details.
Paper: Pulse Peak Migration during the Outburst Decay of the Magnetar SGR 1830-0645: Crustal Motion and Magnetospheric Untwisting
Authors: George Younes, Samuel K Lander, Matthew G. Baring, Teruaki Enoto, Chryssa Kouveliotou, Zorawar Wadiasingh, Wynn C.G. Ho, Alice K. Harding, Zaven Arzoumanian, Keith Gendreau, Tolga Güver, Chin-Ping Hu, Christian Malacaria, Paul S. Ray, and Tod E. Strohmayer
Figure caption: Hot BB vs. warm BB fluxes derived from our phase-resolved spectroscopic analysis, color-coded by time interval (in days) during which the analysis is performed. An obvious linear correlation exists between the fluxes of each component throughout the outburst following Fhot BB ∝ 2 × Fwarm BB, shown as a dashed gray line.
Paper: Pulse Peak Migration during the Outburst Decay of the Magnetar SGR 1830-0645: Crustal Motion and Magnetospheric Untwisting
Authors: George Younes, Samuel K Lander, Matthew G. Baring, Teruaki Enoto, Chryssa Kouveliotou, Zorawar Wadiasingh, Wynn C.G. Ho, Alice K. Harding, Zaven Arzoumanian, Keith Gendreau, Tolga Güver, Chin-Ping Hu, Christian Malacaria, Paul S. Ray, and Tod E. Strohmayer
Figure caption: Temporal evolution of the warm BB (left panels) and hot BB (right panels) for each of the three peaks in the SGR 1830−0645 pulse profile. The upper panels show the 1–10 keV flux decay while the lower panels display their corresponding area evolution. The lines are best-fit linear decay trends. Note that the vertical axes of the upper panels are logarithmic. The constant separations between the lines indicate a similar fractional change in each peak. See text for more details.
Paper: High-frequency Magnetic Fluctuations in Space Plasmas and the Role of Electron Landau Damping
Authors: Vincenzo Carbone, Daniele Telloni, Fabio Lepreti, and Antonio Vecchio
Figure caption: Examples of magnetic energy density spectra obtained from three different 30 minute long samples selected from the data set of the Cluster spacecraft (the referenced time interval which identifies each sample is reported on the different panels). The fit with relation (3), beyond the ionic break, is shown in red and best-fit parameters are reported on the plots. As a reference, we also plot the power laws ω−5/3 in the inertial range, and ω−(1+μ) beyond the ionic break, respectively. The value of the frequency γ is shown with the green arrows.
Paper: High-frequency Magnetic Fluctuations in Space Plasmas and the Role of Electron Landau Damping
Authors: Vincenzo Carbone, Daniele Telloni, Fabio Lepreti, and Antonio Vecchio
Figure caption: Distributions of 1 + μ (left panel) and γ (right panel) obtained through a fit of Equation (3) to the magnetic energy density spectra obtained from N = 631 samples of the data set of the Cluster spacecraft.
Paper: High-frequency Magnetic Fluctuations in Space Plasmas and the Role of Electron Landau Damping
Authors: Vincenzo Carbone, Daniele Telloni, Fabio Lepreti, and Antonio Vecchio
Figure caption: Scatter plot of the density of points in the plane (βe, γ) for the N = 631 samples selected by the data set of the Cluster spacecraft. A power law ﹩{\beta }_{e}^{-3/2}﹩ is reported as a dashed red line. The 400 Hz noise floor (Alexandrova et al. 2012) is marked by a blue dashed horizontal line: points corresponding to γ values above (below) it are displayed as open (filled) signs. The γ values have been obtained for all samples from best fits of Equation (3). For each γ, the corresponding value of βe is measured from the parameters of the sample. In the inset figure we plot the plane (βe, γ) by using only a density of points ≥20.
Paper: Deep XMM-Newton Observations of an X-ray Weak Broad Absorption Line Quasar at z = 6.5
Authors: Jinyi Yang, Xiaohui Fan, Feige Wang, Giorgio Lanzuisi, Riccardo Nanni, Massimo Cappi, George Chartas, Mauro Dadina, Roberto Decarli, Xiangyu Jin, Charles R. Keeton, Bram P. Venemans, Fabian Walter, Ran Wang, Xue-Bing Wu, Minghao Yue, and Ann Zabludoff
Figure caption: The XMM-Newton EPIC image (100″ × 100″) of J0439+1634, combined from the pn, MOS1, and MOS2 images, in the 0.2–0.5 keV (left), 0.5–2 keV (middle), and 2–10 keV (right) X-ray bands. The central crosses represent the optical coordinates of this quasar (i.e., J043947.08+163415.7, Fan et al. 2019). The quasar is detected in the 0.5–2 keV (rest-frame 3.8–15 keV) and 2–10 keV (rest-frame 15–75 keV) bands, but not in the 0.2–0.5 keV band (rest-frame 1.5–3.8 keV).
Paper: Deep XMM-Newton Observations of an X-ray Weak Broad Absorption Line Quasar at z = 6.5
Authors: Jinyi Yang, Xiaohui Fan, Feige Wang, Giorgio Lanzuisi, Riccardo Nanni, Massimo Cappi, George Chartas, Mauro Dadina, Roberto Decarli, Xiangyu Jin, Charles R. Keeton, Bram P. Venemans, Fabian Walter, Ran Wang, Xue-Bing Wu, Minghao Yue, and Ann Zabludoff
Figure caption: The XMM-Newton EPIC spectra of quasar J0439+1634. The upper panel shows the observed counts from the pn camera (black), MOS1 (red), and MOS2 (blue). The solid lines represent the spectral fits using an absorbed power-law model consistent of a power-law model, Galactic absorption, and quasar intrinsic absorption, with the assumption of an intrinsic photon index of Γ = 1.9 (Nanni et al. 2017). The dashed lines denote the spectral fits with a free Γ (see details of spectral fitting in Section 3.2). The bottom panel shows the residuals, with filled circles for the fixed-Γ fits and open squares for the Γ-free fits. The spectral fitting is applied to the spectra grouped to one count per bin, and the data have been rebinned for plotting purpose here using XSPEC.
Paper: Deep XMM-Newton Observations of an X-ray Weak Broad Absorption Line Quasar at z = 6.5
Authors: Jinyi Yang, Xiaohui Fan, Feige Wang, Giorgio Lanzuisi, Riccardo Nanni, Massimo Cappi, George Chartas, Mauro Dadina, Roberto Decarli, Xiangyu Jin, Charles R. Keeton, Bram P. Venemans, Fabian Walter, Ran Wang, Xue-Bing Wu, Minghao Yue, and Ann Zabludoff
Figure caption: Optical-to-X-ray spectral slope αox vs. 2500 Å luminosity. Our measurement from J0439+1634 is shown in red, compared with values from quasar samples at similar redhsift and lower redshift. The two red triangles are the αox values accounting for the intrinsic absorption based on Γ-fixed (lower value) and Γ-free (upper value) model fitting. For high-redshift comparisons, we show individual measurements at 5.5 < z < 6 from Nanni et al. (2017), 6 < z < 6.5 from Vito et al. (2019), and z > 6.5 from Wang et al. (2021). We also include the new upper limit (black square) from a z = 6.515 quasar in Vito et al. (2021). The low-redshift SDSS quasar sample (gray dots) is generated based on the L2–10 keV from Timlin et al. (2020) and L2500 Å from Wang et al. (2021). The relations in the literature are plotted as black solid line (Nanni et al. 2017), gray solid line (Timlin et al. 2020), dashed line (Lusso & Risaliti 2017), dotted line (Just et al. 2007), and dashed–dotted line (Martocchia et al. 2017).The blue squares are the measurements for low-redshift BAL quasars from Luo et al. (2014). Among the sample in Luo et al. (2014), the quasar PG0043+03 is not detected, and it has been updated in Kollatschny et al. (2016) (blue filled circle). All measurements have been corrected to the cosmology adopted in this work.
Paper: Fundamental Electromagnetic Emissions by a Weak Electron Beam in Solar Wind Plasmas with Density Fluctuations
Authors: C. Krafft, and P. Savoini
Figure caption: Initial distribution of the background plasma density fluctuations δn/n0 in the plane (x, y), corresponding to the average level ﹩{\rm{\Delta }}N=\langle {(\delta n/{n}_{0})}^{2}{\rangle }^{1/2}\simeq 0.05﹩. The size of the box is ﹩{L}_{x}\times {L}_{y}=5792\times 2896{\lambda }_{D}^{2}﹩.
Paper: Fundamental Electromagnetic Emissions by a Weak Electron Beam in Solar Wind Plasmas with Density Fluctuations
Authors: C. Krafft, and P. Savoini
Figure caption: Distributions of the wave spectral magnetic energy density log10(∣Bzk(kx, ky)∣2) emitted around the frequency ωk ≃ ωp, for ΔN = 0.05 and the “large” simulation box of size ﹩{L}_{x}\times {L}_{y}=5792\times 2896{\lambda }_{D}^{2}﹩. The initial plasma density distribution is given in Figure 1. The spectra are shown at times ωpt = 145, 680, 940, 1485, 2020, and 3100. A green circle of radius kλD ≃ kthλD is superposed on the spectra at the first and last times. The same color bar holds for all plots. All variables are normalized.
Paper: Fundamental Electromagnetic Emissions by a Weak Electron Beam in Solar Wind Plasmas with Density Fluctuations
Authors: C. Krafft, and P. Savoini
Figure caption: Distributions of the wave spectral magnetic energy densities log10(∣Bzk(kx, ky)∣2) emitted at the frequency ωk ≃ ωp, for (a) ΔN = 0 (upper row) and (b) ΔN = 0.05 (bottom row). The initial density distribution is given in Figure 1 of Krafft & Savoini (2021). The “smaller” box with size ﹩{L}_{x}\times {L}_{y}=1448\times 1448{\lambda }_{D}^{2}﹩ is used. The spectra are given at times ωpt = 145, 2020, 3100, 6430, and 7960. The same color bar holds for all plots. All variables are normalized.
Paper: Fundamental Electromagnetic Emissions by a Weak Electron Beam in Solar Wind Plasmas with Density Fluctuations
Authors: C. Krafft, and P. Savoini
Figure caption: Dispersion plots of the wave spectral magnetic energy densities log10(∣Bzk(ωk, kx)∣2) as a function of the normalized frequency ωk/ωp and parallel wave vector kxλD, for a homogeneous plasma with ΔN = 0 and a plasma with density fluctuations (ΔN = 0.05). The simulations used are the same as in Figures 2–3. Panel A: dispersion plots for ΔN = 0.05, at ωpt = 680, 2020, and 3100, computed with the “large” simulation box; a zoom of the frequency wave-number domain 0.9 < ωk/ωp < 1.2 and ∣kxλD∣ < 0.02 is shown for ωpt = 3100 in the bottom right corner. Panel B : dispersion plots obtained using the “smaller” box, at ωpt = 2020, for ΔN = 0 (left) and ΔN = 0.05 (right). Panel C: dispersion plots at asymptotic times for ΔN = 0 (left, ωpt = 7960) and ΔN = 0.05 (right, ωpt = 6340); the “smaller” simulation box is used. The same color bar holds for all plots of panels (A), (B), and (C). All variables are normalized.
Paper: Fundamental Electromagnetic Emissions by a Weak Electron Beam in Solar Wind Plasmas with Density Fluctuations
Authors: C. Krafft, and P. Savoini
Figure caption: Time variations of various energies W in logarithmic scales. (a) : ﹩{W}_{{ \mathcal L }h}﹩ and ﹩{W}_{{ \mathcal M }h}﹩ as well as ﹩{W}_{{ \mathcal L }}﹩ and ﹩{W}_{{ \mathcal M }};﹩ the presence (absence) of the subscript “h” refers to the case of the homogeneous plasma (inhomogeneous plasma with ΔN = 0.05); the subscripts “﹩{ \mathcal L }﹩” and “﹩{ \mathcal M }﹩” refer to the total Langmuir and the total electromagnetic energies, respectively. (b) : ﹩{W}_{{ \mathcal F }h}﹩ and ﹩{W}_{{ \mathcal F }};﹩ the subscript “﹩{ \mathcal F }﹩” refers to the electromagnetic energy at frequency ωk = ωp. (c) : ﹩{W}_{{ \mathcal M }h}﹩, ﹩{W}_{{ \mathcal H }h}﹩, and ﹩{W}_{{ \mathcal F }h}﹩ (solid, dashed, and dotted curves), for ΔN = 0; the subscript “﹩{ \mathcal H }﹩” refers to the electromagnetic energy at frequency ωk = 2ωp. (d) : ﹩{W}_{{ \mathcal M }}﹩, ﹩{W}_{{ \mathcal H }}﹩, and ﹩{W}_{{ \mathcal F }}﹩ (solid, dashed, and dotted curves), for ΔN = 0.05. (e) : ﹩{W}_{{ \mathcal F }h}/{W}_{{ \mathcal H }h}﹩ and ﹩{W}_{{ \mathcal F }}/{W}_{{ \mathcal H }}﹩. (f) : ﹩{W}_{{ \mathcal F }h}/{W}_{{ \mathcal L }h}﹩ and ﹩{W}_{{ \mathcal F }}/{W}_{{ \mathcal L }}﹩. All energies are normalized by the initial beam kinetic energy.
Paper: Evidence for Plasma Heating at Thin Current Sheets in the Solar Wind
Authors: Zilu Zhou, Xiaojun Xu, Pingbing Zuo, Yi Wang, Qi Xu, Yudong Ye, Jing Wang, Ming Wang, Qing Chang, Xing Wang, and Lei Luo
Figure caption: Occurrence distributions: (a) the ratios of the proton temperatures at current sheets to those outside current sheets, and (b) the ratios of the electron temperatures at current sheets to those outside current sheets. The dashed vertical lines denote the corresponding median number of each data set.
Paper: Evidence for Plasma Heating at Thin Current Sheets in the Solar Wind
Authors: Zilu Zhou, Xiaojun Xu, Pingbing Zuo, Yi Wang, Qi Xu, Yudong Ye, Jing Wang, Ming Wang, Qing Chang, Xing Wang, and Lei Luo
Figure caption: Median numbers of the ratios of (a) proton temperature and (b) electron temperature at different distance from the leading edge of current sheets to the proton/electron temperature at the leading edge of the current sheets in the slow wind (blue lines) and fast wind (red lines), respectively.
Paper: Evidence for Plasma Heating at Thin Current Sheets in the Solar Wind
Authors: Zilu Zhou, Xiaojun Xu, Pingbing Zuo, Yi Wang, Qi Xu, Yudong Ye, Jing Wang, Ming Wang, Qing Chang, Xing Wang, and Lei Luo
Figure caption: Superposed-epoch analysis of identified thin current sheets in fast wind (red lines) and slow wind (blue lines): (a) proton temperature in fast wind, (b) proton temperature in slow wind, (c) electron temperature in fast wind, (d) electron temperature in slow wind, (e) magnetic field intensity, (f) magnetic energy density, (g) magnetic field increment, and (h) Alfvén speed.
Paper: Three-Dimensional Anisotropy and Scaling Properties of Solar Wind Turbulence at Kinetic Scales in the Inner Heliosphere: Parker Solar Probe Observations
Authors: J. Zhang, S. Y. Huang, J. S. He, T. Y. Wang, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, S. B. Xu, Q. Y. Xiong, R. T. Lin, and L. Yu
Figure caption: 2D SFs in ﹩({l}_{| | },\sqrt{{l}_{\perp }^{2}+{L}_{\perp }^{2}})﹩ and (l⊥, L⊥) planes. The first, second, and third columns represent SFs of the total, perpendicular, and parallel magnetic-field fluctuations, respectively. The symbols (l∣∣, l⊥, L⊥) represent the spatial distances along the parallel, perpendicular, and displacement directions.
Paper: Three-Dimensional Anisotropy and Scaling Properties of Solar Wind Turbulence at Kinetic Scales in the Inner Heliosphere: Parker Solar Probe Observations
Authors: J. Zhang, S. Y. Huang, J. S. He, T. Y. Wang, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, S. B. Xu, Q. Y. Xiong, R. T. Lin, and L. Yu
Figure caption: The upper panels (a)–(c) represents the 1D SFs vs. L⊥, l⊥ and l∣∣, and the lower panels (d)–(f) shows the relation between L⊥, l⊥, and l∣∣. In the upper panels, the horizontal dashed red lines indicate the range to calculate the wave-vector anisotropy and the black lines mark two values of SFs for 3D visualization. In the lower panel, three typical relations are presented as gray dotted lines for reference and lines marked with “3/3” represent isotropic relations. The bold gray transparent solid lines are our fitting lines. The first, second, and third columns represent the SFs of the total, perpendicular, and parallel magnetic-field fluctuations, respectively.
Paper: Three-Dimensional Anisotropy and Scaling Properties of Solar Wind Turbulence at Kinetic Scales in the Inner Heliosphere: Parker Solar Probe Observations
Authors: J. Zhang, S. Y. Huang, J. S. He, T. Y. Wang, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, S. B. Xu, Q. Y. Xiong, R. T. Lin, and L. Yu
Figure caption: The upper panel: distributions of spectral indices at (a) the ion-to-electron scales and (b) the transition range in the (﹩{\phi }_{\delta {B}_{\perp }}﹩, θB) plane. The lower panel: SFs at (c) 0.7 di and (d) 2.6 di as a function of ﹩{\phi }_{\delta {B}_{\perp }}﹩ and θB.
Paper: Three-Dimensional Anisotropy and Scaling Properties of Solar Wind Turbulence at Kinetic Scales in the Inner Heliosphere: Parker Solar Probe Observations
Authors: J. Zhang, S. Y. Huang, J. S. He, T. Y. Wang, Z. G. Yuan, X. H. Deng, K. Jiang, Y. Y. Wei, S. B. Xu, Q. Y. Xiong, R. T. Lin, and L. Yu
Figure caption: The first, second, and third columns represent isosurfaces of SFs for the total, the perpendicular, and the parallel magnetic-field fluctuations. The upper panel shows isosurfaces at higher values of SF, and smaller values in the lower panel. These SFs are marked with black dashed lines on Figures 2(a)–(c). The colors indicate distances from the origin to help in visualizing the anisotropy.
Paper: What Seismic Minimum Reveals about Solar Magnetism below the Surface
Authors: Kiran Jain, Niket Jain, Sushanta C. Tripathy, and Mausumi Dikpati
Figure caption: Temporal evolution of frequency shifts (symbols) for (a) all modes, and the modes with lower turning points in (b) convection zone, (c) radiative zone, and (d) core. The errors in shifts are of the order of 10−6 μHz. An 11 point running mean of the frequency shifts is shown by the solid red line. Vertical dotted lines show the epochs of minima in frequency shifts. The horizontal lines represent the lowest values of the running mean during MIN 22/23 (brown), MIN 23/24 (green), and MIN 24/25 (blue). The variations in smoothed radio flux are shown by the black dashed line. Background colors depict solar cycles (from left to right) 22 (partial), 23, 24, and 25 (partial) where the boundaries of different cycles are based on the activity minima.
Paper: What Seismic Minimum Reveals about Solar Magnetism below the Surface
Authors: Kiran Jain, Niket Jain, Sushanta C. Tripathy, and Mausumi Dikpati
Figure caption: Same as Figure 1 but for modes with upper turning points in (a) high-ν, (b) mid-ν, and (c) low-ν ranges.
Paper: What Seismic Minimum Reveals about Solar Magnetism below the Surface
Authors: Kiran Jain, Niket Jain, Sushanta C. Tripathy, and Mausumi Dikpati
Figure caption: Temporal evolution of frequency shifts (symbols) near 3 solar minima for the modes with lower turning points in convection zone in three frequency ranges as marked in the leftmost panel of each row. An 11 point running mean of the frequency shifts is shown by the solid red line. The horizontal lines represent the lowest values of the running mean during MIN 22/23 (brown), MIN 23/24 (green), and MIN 24/25 (blue). The errors are smaller than the size of the symbols and shown by black. While boundaries of two background colors in each panel represent the activity minimum as marked on the top of each column, vertical dotted lines show the epochs of minima in frequency shifts.
Paper: What Seismic Minimum Reveals about Solar Magnetism below the Surface
Authors: Kiran Jain, Niket Jain, Sushanta C. Tripathy, and Mausumi Dikpati
Figure caption: Same as Figure 3 but for the modes with lower turning points in the radiative zone.
Paper: What Seismic Minimum Reveals about Solar Magnetism below the Surface
Authors: Kiran Jain, Niket Jain, Sushanta C. Tripathy, and Mausumi Dikpati
Figure caption: Same as Figure 3 but for the modes with lower turning points in core.