adsabs/AstroCLIMB huggingface dataset:
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: The bMS, rMS, and uMS stars are labeled with solid blue circles, red diamonds, and green squares, respectively. The candidate binary or triplet system located near the equal-mass sequence (the dotted black line) is represented by a solid yellow triangle. The double-lined spectroscopic binary system is labeled with an open square. The magenta dashed line represents the best-fitting isochrone. The light-gray dots are other member stars for which we do not have spectra. In the left panel, we show the mean uncertainties for the G magnitudes and G BP − G RP colors of stars in each G-magnitude bin of 0.5 mag.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: CMD of NGC 2422 member stars (black dots) based on Gaia EDR3. Isochrones of ages ranging from 90 Myr to 170 Myr in steps of 20 Myr are shown as dashed lines. The magenta dashed line shows the best-fitting isochrone to the blue edge of the eMSTO, with an age 90 Myr, A V = 0.3 mag, Z = 0.0133, and a distance modulus (m − M)0 = 8.29 mag. Other isochrones are shown as green dashed lines. The black arrow represents the reddening vector, corresponding to ΔA V = 1.0 mag. The inset shows the MS region used to test for differential reddening, where the solid orange lines are obtained by shifting the best-fitting isochrone (dashed magenta line) by ±0.02 mag in color.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: Comparison of derived ﹩v\sin i﹩ values from CFHT and SALT spectra for 11 stars observed with both facilities (black dots). The error bars show the 2σ uncertainties presented in Table 1. The red dashed line is the equal-value track. The dotted green line shows the best-fitting line for the data points, representing the function of ﹩v\sin {i}_{\mathrm{SALT}}=1.07v\sin {i}_{\mathrm{CFHT}}+6.40\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, where ﹩v\sin {i}_{\mathrm{SALT}}﹩ and ﹩v\sin {i}_{\mathrm{CFHT}}﹩ denote the projected rotation rates measured from the spectra observed with SALT and CFHT, respectively.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: Two example spectra of a slowly rotating star (left), and a fast-rotating star (right), along with their best-fitting models (red solid lines). Best-fitting parameters are shown in each legend.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: Comparison of the split-MS regions of NGC 2422 (red dots) and NGC 2287 (black dots). To separate their split MSs, the CMD of NGC 2287 was shifted up by 1 mag along the ordinate. The gray area highlights the region where their split patterns are most evident.
Paper: The Role of Binarity and Stellar Rotation in the Split Main Sequence of NGC 2422
Authors: Chenyu He, 辰昱 贺, Weijia Sun, 唯佳 孙, Chengyuan Li, 程远 李, Lu Li, 璐 李, Zhengyi Shao, 正义 邵, Jing Zhong, 靖 钟, Li Chen, 力 陈, Richard de Grijs, Baitian Tang, 柏添 汤, Songmei Qin, 松梅 秦, Zara Randriamanakoto
Figure caption: CMD of the 47 stars with ﹩v\sin i﹩ measurements (color coded).
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: Intermittent pseudosinusoidal curves of simulated long-term observations for Kepler-438 b, TRAPPIST-1 g, and Proxima Centauri b. Every observation lasts for approximately 4 hr.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: Summed pseudosinusoidal relative frequency curves of long-term observations for uninterrupted random-generated zone RFI, narrowband RFI, CM broadband RFI, and SM broadband RFI.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: The situation in which observation time τ obs coincides with the phase of the peak or trough part. For a pseudosinusoidal curve, the monotonicity changes in the peak or trough part.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: A simulated short-term observation for a radio source with ﹩\dot{\nu }=-0.05\,\mathrm{Hz}﹩ s−1.
Paper: Large-amplitude Bidirectional Anisotropy of Cosmic-Ray Intensity Observed with Worldwide Networks of Ground-based Neutron Monitors and Muon Detectors in 2021 November
Authors: K. Munakata, M. Kozai, C. Kato, Y. Hayashi, R. Kataoka, A. Kadokura, M. Tokumaru, R. R. S. Mendonça, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, M. L. Duldig, J. E. Humble, I. Sabbah, P. Evenson, P.-S. Mangeard, T. Kuwabara, D. Ruffolo, A. Sáiz, W. Mitthumsiri, W. Nuntiyakul, J. Kóta
Figure caption: Response functions of a sample of four NMs and four vertical channels of MDs. Panel (a) shows the differential response functions R(x, Z, p), while panel (b) displays R(x, Z, p) integrated below p, each as a function of the primary GCR’s rigidity p. Black, blue, red, and purple dashed curves show the response functions of ATHN, THUL, PSNM, and SYOW, respectively, while the black, blue, red, and purple solid curves show functions of four vertical channels of the Nagoya, Hobart, São Martinho, and Syowa MDs, respectively. Note that the blue and purple curves of THUL and SYOW are overlapped due to similar P  c  and atmospheric depth at these NMs. All response functions are normalized and divided by the total integral of R(x, Z, p) over p (﹩{\int }_{{P}_{c}}^{\infty }R(x,Z,p){dp}﹩).
Paper: Accumulation of Elastic Strain toward Crustal Fracture in Magnetized Neutron Stars
Authors: Yasufumi Kojima
Figure caption: Contour map of stress tensor in crust. The left panel shows 2μ σ  θ ϕ , the middle 2μ σ  r ϕ , and the right the magnitude σ. They are normalized according to the maximum. Negative values are plotted using a dotted curve in the left panel. The magnitude σ in the right panel is shown in the outer small region near the surface, R − 0.1Δr ≤ r ≤ R.
Paper: Accumulation of Elastic Strain toward Crustal Fracture in Magnetized Neutron Stars
Authors: Yasufumi Kojima
Figure caption: Crust contour map of magnitude of stress tensor normalized using the maximum. The left panel for the in model shows σ ≈ σ  θ ϕ , whereas the right panel for the out model shows σ ≈ σ  r ϕ .
Paper: Accumulation of Elastic Strain toward Crustal Fracture in Magnetized Neutron Stars
Authors: Yasufumi Kojima
Figure caption: Energy distribution in crust as a function of the radius. Normalized energy density ε(r) is plotted for magnetic energy, which is denoted by a dotted curve, and elastic energy, denoted by a solid curve.
Paper: Accumulation of Elastic Strain toward Crustal Fracture in Magnetized Neutron Stars
Authors: Yasufumi Kojima
Figure caption: Color contour map of crust for the magnitude of the stress tensor σ normalized using the maximum; two models are compared.
Paper: Accumulation of Elastic Strain toward Crustal Fracture in Magnetized Neutron Stars
Authors: Yasufumi Kojima
Figure caption: Spatial distribution of magnetic energy (dotted curve) and elastic energy (solid curve) in the crust. Normalized energy densities ε(r) are plotted for two models.
Paper: Fast Neutrino Cooling in the Accreting Neutron Star MXB 1659-29
Authors: Melissa Mendes, Farrukh J. Fattoyev, Andrew Cumming, Charles Gale
Figure caption: Superfluid gap Δ (megaelectronvolt) and critical temperature T c (Kelvin) as a function of Fermi momentum k F (per femtometer) for the PS (top panel) and NT (bottom panel) gap models used in our calculations (see Ho et al. 2015 for details of the analytic fits and references for each gap model).
Paper: Fast Neutrino Cooling in the Accreting Neutron Star MXB 1659-29
Authors: Melissa Mendes, Farrukh J. Fattoyev, Andrew Cumming, Charles Gale
Figure caption: Three scenarios to explain the neutrino luminosity of MXB 1659-29. The shaded region indicates the part of the neutron star core undergoing active dUrca neutrino emission, indicated by the arrow. (a) No superfluidity in the region ρ > ρ dUrca. (b) A superfluid gap opens at a density ρ opening > ρ dUrca, suppressing dUrca in the center and leading to neutrino emission from a shell. (c) The superfluid gap opens before the onset of dUrca, ρ opening < ρ dUrca, but closes again at high density ρ closing < ρ  c , where ρ  c  is the central density. In this case neutrino emission is suppressed in the outer part of the core, reducing the size of the central emitting volume. Note that distances are not to scale in these diagrams; ρ boundary, ρ crust, and ρ  c  represent the surface, crust-core boundary, and central densities, respectively. An example of case b (case c) is the 1.6 M ⊙, L = 70 MeV (2.01 M ⊙, L = 50 MeV) star with the NT SYHHP gap shown in Figure 5.
Paper: Fast Neutrino Cooling in the Accreting Neutron Star MXB 1659-29
Authors: Melissa Mendes, Farrukh J. Fattoyev, Andrew Cumming, Charles Gale
Figure caption: Top panel: neutron star mass that reproduces the neutrino luminosity of MXB 1659-29 as a function of L for neutron star models without pairing. The blue shaded region corresponds to the 1σ uncertainty in neutrino luminosity from Brown et al. (2018). The dUrca threshold and maximum neutron star mass allowed by the EOS are shown by the dashed orange and dashed blue lines, respectively. Bottom panel: percentage of the core volume involved in unsuppressed dUrca reactions. The shaded region corresponds to the 1σ blue shaded region in the top panel.
Paper: Fast Neutrino Cooling in the Accreting Neutron Star MXB 1659-29
Authors: Melissa Mendes, Farrukh J. Fattoyev, Andrew Cumming, Charles Gale
Figure caption: Mass vs. radius curves of EOS with L = 47, 60, 80, and 112.7 MeV, from left to right. Observational constraints for PSR J0030+0451 (Miller et al. 2019) and PSR J0740+6620 (Miller et al. 2021) indicated with error bars and maximum-mass neutron star observed to date, MSP J0740+6620 (Cromartie et al. 2019), with the shaded region.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Optical and MIR time domain data of our sample and analysis. (a) CRTS V-band and ZTF g-band LCs of three typical galaxies: J0040+0823 (black) represents a galaxy without optical variability, while J0950+5128 (blue) and J1301+2127 (red) are two variable galaxies. For clarity, we display the monthly binned ZTF LCs by adding constants. (b) The apparent variability amplitude vs. the rms of the photometric errors for the CRTS V-band and ZTF g-band observations. (c) WISE W 2-band LCs of the three galaxies. (d) Similar to (b), but using WISE/W 2 data.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Distributions of the radio transients in the P  j /L bol − λ Edd plane, from our sample (red dots), Nyland et al. (2020; green dots) and Wołowska et al. (2021; cyan dots). For comparison, we also show the distributions of young radio sources (YRS) from Wójtowicz et al. (2020) and Liao & Gu (2020), and other types of AGNs analyzed by Rusinek et al. (2017), including FR type II narrowline radio galaxies (NLRG FRII), broadline radio galaxies (BLRG FRII), and radio-loud quasars (RLQ FRII, right density plot). The FR type I radio galaxies from Capetti et al. (2017) are shown in the left density plot. The typical errors on P  j /L bol and λ Edd for our sample are shown in the left corner (see Section 5.4 for the details).
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Left: the extinction-corrected rest-frame u − r colors vs. total stellar masses. Both are derived from the SED fitting to the combined SDSS and WISE photometry using MAGPHYS (Chang et al. 2015). The contours show the densities of the SDSS spectroscopic galaxies, which display the bimodal distribution. The red circles display our sample, while the blue triangles show the optical TDEs compiled in van Velzen et al. (2021), for comparison. Right: plot of the Hα EW emission lines vs. the Lick Hδ A indices. The SDSS galaxies are represented by the gray dots. The radio transients in our sample and the optical TDEs are shown with the same symbols as the left panel.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: A comparison of the BH mass distributions for our sample (dark yellow) and the UV/optical TDE galaxies from Wevers et al. (2017). Both sets of BH masses are derived using stellar velocity dispersions. The error bars represent 1σ Poisson uncertainties, i.e., ﹩{\sigma }_{{\rm{k}}}=\sqrt{{N}_{{\rm{k}}}}﹩, where N k is the number of measurements falling in the kth bin of M BH.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: From left to right, SDSS optical spectrum of the host galaxy, SDSS r-band image, FIRST image, VLASS epoch I image, and VLASS epoch II image. The red circle has a radius of r = 2.″5, comparable to the beam size of the VLASS images. The red cross represents the center of the radio emission from the VLASS epoch I observations. Each image cutout has a size of 30″ × 30″.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Histogram of the radio spectral index between 888 MHz and 3 GHz for the RTSs in our sample and those in Nyland et al. (2020). For comparison, we also show the optically thick spectral indices (α thick) for the latter sample, which were derived by fitting a power-law model to the quasi-simultaneous flux densities at 1.4 GHz and 3 GHz. The error bars represent 1σ Poisson uncertainties.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Left: the variability amplitude of the radio flux between the VLASS epoch I and epoch II observations for our sample (upper panel) and the sample presented by Nyland et al. (2020; lower panel). Right: the same as the left, but comparing with the sample presented by Wołowska et al. (2021).
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Composite SDSS gri color images of the RTS host galaxies. Each panel has a size of 30″ × 30″.
Paper: Large-amplitude Bidirectional Anisotropy of Cosmic-Ray Intensity Observed with Worldwide Networks of Ground-based Neutron Monitors and Muon Detectors in 2021 November
Authors: K. Munakata, M. Kozai, C. Kato, Y. Hayashi, R. Kataoka, A. Kadokura, M. Tokumaru, R. R. S. Mendonça, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, M. L. Duldig, J. E. Humble, I. Sabbah, P. Evenson, P.-S. Mangeard, T. Kuwabara, D. Ruffolo, A. Sáiz, W. Mitthumsiri, W. Nuntiyakul, J. Kóta
Figure caption: Best-fit cosmic-ray parameters in 2021 November 3–5. Panel (a) shows the GCR density (black circles) on the left vertical axis and amplitudes of the first-order (blue circles) and second-order (red circles) anisotropies on the right vertical axes, each at 15 GV, which is the representative P  m  for NMs. Note an identical extent (7%) of the left and right vertical axes. We calculate these amplitudes (A 1 and A 2) as ﹩{A}_{1}=\sqrt{{\sum }_{m=0}^{1}\{{\xi }_{c}^{1,m}{(t)}^{2}+{\xi }_{s}^{1,m}{(t)}^{2}\}}﹩ and ﹩{A}_{2}=\sqrt{{\sum }_{m=0}^{2}\{{\xi }_{c}^{2,m}{(t)}^{2}+{\xi }_{s}^{2,m}{(t)}^{2}\}}﹩. In panel (b), black (blue) solid circles display the GSE longitude (latitude) of the orientation of the maximum intensity in the first-order anisotropy on the left (right) vertical axis. Panel (c) also displays the GSE longitude and latitude of the second-order anisotropy in the same manner as (b). In panels (b) and (c), the black and blue solid curves display the longitude and latitude of the IMF orientation, respectively. For the second-order anisotropy, there are two directions of maximum intensity; we plot the direction that is closer to the IMF orientation. Panel (d) shows the power-law indices of rigidity spectra of the density (black), first-order anisotropy (blue), and second-order anisotropy (red). Panel (e) shows GCR density and anisotropy amplitudes at 65 GV, which is the representative P  m  for MDs, in the same manner as (a).
Paper: Large-amplitude Bidirectional Anisotropy of Cosmic-Ray Intensity Observed with Worldwide Networks of Ground-based Neutron Monitors and Muon Detectors in 2021 November
Authors: K. Munakata, M. Kozai, C. Kato, Y. Hayashi, R. Kataoka, A. Kadokura, M. Tokumaru, R. R. S. Mendonça, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, M. L. Duldig, J. E. Humble, I. Sabbah, P. Evenson, P.-S. Mangeard, T. Kuwabara, D. Ruffolo, A. Sáiz, W. Mitthumsiri, W. Nuntiyakul, J. Kóta
Figure caption: Best-fit performance. In each panel of Figure 2(a), black solid circles with statistical error bars and gray curves show the observed and the fit to cosmic-ray data, respectively, for a sample of four NMs (ATHN, THUL, PSNM, and SYOW) in the upper panels and four vertical channels of MDs (Nagoya, Hobart, São Martinho, and Syowa) in the lower panels. PSNM data in the left panel of (a) are multiplied by 3. Also shown in each panel are the individual contributions from the GCR density (black thin curve), the first-order anisotropy (blue thin curve), and the second-order anisotropy (red thin curve). The gray curve is the sum of the three thin curves in each panel. The purple curve at the bottom of each panel is the contribution to χ 2 from that channel. In Figure 2(b), the coefficient of determination R 2 (left panel) and the reduced χ 2 (right panel) are shown as functions of time. The reduced χ 2 is calculated by dividing χ 2 in Equation (7) by the number of degrees of freedom N dof (see Section 2.2).
Paper: Large-amplitude Bidirectional Anisotropy of Cosmic-Ray Intensity Observed with Worldwide Networks of Ground-based Neutron Monitors and Muon Detectors in 2021 November
Authors: K. Munakata, M. Kozai, C. Kato, Y. Hayashi, R. Kataoka, A. Kadokura, M. Tokumaru, R. R. S. Mendonça, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, M. L. Duldig, J. E. Humble, I. Sabbah, P. Evenson, P.-S. Mangeard, T. Kuwabara, D. Ruffolo, A. Sáiz, W. Mitthumsiri, W. Nuntiyakul, J. Kóta
Figure caption: Solar wind parameters and cosmic-ray data during 2021 November 3–5. Panels (a)–(d) show 1 minute solar wind data: (a) solar wind velocity, (b) plasma density and temperature on the left and right vertical axes, respectively, (c) IMF magnitude and its fluctuation, on the left and right vertical axes, respectively, and (d) GSE longitude and latitude of IMF orientation, on the left and right vertical axes, respectively. Panels (e) and (f) show hourly count rates of a sample of four NMs (ATHN, THUL, PSNM, and SYOW) and four vertical channels of MDs (Nagoya, Hobart, São Martinho, and Syowa). PSNM data in (e) are multiplied by 3 to show the variation more clearly. The vertical orange line indicates the IP-shock arrival, while a pair of purple vertical lines delimit the MFR period defined in this paper.
Paper: Large-amplitude Bidirectional Anisotropy of Cosmic-Ray Intensity Observed with Worldwide Networks of Ground-based Neutron Monitors and Muon Detectors in 2021 November
Authors: K. Munakata, M. Kozai, C. Kato, Y. Hayashi, R. Kataoka, A. Kadokura, M. Tokumaru, R. R. S. Mendonça, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, M. L. Duldig, J. E. Humble, I. Sabbah, P. Evenson, P.-S. Mangeard, T. Kuwabara, D. Ruffolo, A. Sáiz, W. Mitthumsiri, W. Nuntiyakul, J. Kóta
Figure caption: Intensity map of the best-fit anisotropy at 15 GV in GSE coordinates. From the left, each column shows the intensity in the first-order (n = 1), second-order (n = 2), and total (n = 1 and n = 2) anisotropies, each as a color map in the GSE longitude and latitude space, while from the top each row shows the anisotropy in four hours between 18:30 and 21:30 of November 4 when the large-amplitude anisotropy is observed. The solid and open circles indicate the orientations parallel and antiparallel to the IMF, respectively, while the solid curve indicates the magnetic equator. The X mark indicates the orientation of maximum intensity.
Paper: Phase Mixing and the 1/f Spectrum in the Solar Wind
Authors: Norbert Magyar, Tom Van Doorsselaere
Figure caption: The sum of the Alfvén speed and background flow in a slice at x = 0, for the Kolmogorov 2D noise map, for the Alfvén wave setup. The spatial extent along the y-direction is multiplied by s.
Paper: Phase Mixing and the 1/f Spectrum in the Solar Wind
Authors: Norbert Magyar, Tom Van Doorsselaere
Figure caption: The Alfvén wave solutions of Equation (6) in a slice at x = 0 for the Kolmogorov 2D noise map. Left: f = 0.5 mHz or T = 2000 s. Right: f = 2 mHz or T = 500 s. The spatial extent along the y-direction is multiplied by s.
Paper: Phase Mixing and the 1/f Spectrum in the Solar Wind
Authors: Norbert Magyar, Tom Van Doorsselaere
Figure caption: Alfvén wave perpendicular energy spectra at different heights, for the pink 2D noise map. Left: f = 0.5 mHz. Right: f = 2 mHz. The two dashed lines represent spectral slopes of −1 and 1.
Paper: Phase Mixing and the 1/f Spectrum in the Solar Wind
Authors: Norbert Magyar, Tom Van Doorsselaere
Figure caption: Alfvén wave perpendicular energy spectra at different heights, for the Brownian 2D noise map. Left: f = 0.5 mHz. Right:  f = 2 mHz. The two dashed lines represent spectral slopes of −2 and 1.