adsabs/AstroCLIMB huggingface dataset:
Paper: Limits on Fast Radio Burst–like Counterparts to Gamma-Ray Bursts Using CHIME/FRB
Authors: Alice P. Curtin, Shriharsh P. Tendulkar, Alexander Josephy, Pragya Chawla, Bridget Andersen, Victoria M. Kaspi, Mohit Bhardwaj, Tomas Cassanelli, Amanda Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Jane F. Kaczmarek, Adam E. Lanmnan, Calvin Leung, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, Masoud Rafiei-Ravandi, Scott M. Ransom, Kaitlyn Shin, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Same as in Figure 4, except for the radio-to-high-energy fluence ratio limits for the LGRBs within our sample that are detected by Swift/BAT.
Paper: Limits on Fast Radio Burst–like Counterparts to Gamma-Ray Bursts Using CHIME/FRB
Authors: Alice P. Curtin, Shriharsh P. Tendulkar, Alexander Josephy, Pragya Chawla, Bridget Andersen, Victoria M. Kaspi, Mohit Bhardwaj, Tomas Cassanelli, Amanda Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Jane F. Kaczmarek, Adam E. Lanmnan, Calvin Leung, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, Masoud Rafiei-Ravandi, Scott M. Ransom, Kaitlyn Shin, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Same as in Figure 4, except for the LGRBs within our sample that are detected by Fermi/GBM.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Initial magnetic-to-fluid pressure ratio β −1 with magnetic field line geometry overlaid. We show models lo-B (left) and hi-B (right) in a slice through the magnetic dipole axis (y = 0 plane), soon after the magnetic field is turned on at t = 0 ms. This magnetic field configuration was added onto an unmagnetized PNS wind solution previously evolved for about 176 ms to steady state. For model hi-B, magnetic pressure dominates over fluid pressure in the polar regions above the PNS surface out to ≈60 km.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Snapshots showing the outflow properties as a cross section through the magnetic dipole axis (y = 0 plane) at t ≈ 55 ms after B-field initialization for models no-B (unmagnetized, left) and lo-B (weakly magnetized, right). From top to bottom: specific entropy s, electron fraction Y  e , and radial velocity v  r . The green contour represents the α-particle formation surface (X  α  = 0.5), around which r-process seed nuclei begin to form, while the red contour represents the location of the neutrinosphere (﹩{\tau }_{{\bar{\nu }}_{e}}=1﹩ surface).
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Magnetic power spectra obtained by MDI and HMI synoptic magnetograms for CR 2097 (left) and CR 2101 (right). (a)–(b) Synoptic maps; the magnetic fields are saturated at 53 G and 100 G, respectively. (c)–(d) Power spectra of the HMI map (red), the MDI map (blue), and the calibrated HMI map (black). (e)–(f) Power spectra for ﹩{l}_{\max }=20﹩. The blue dotted lines are the power spectra of the MDI maps multiplied by a factor of 0.8 on polar fields. (g)–(h) The results of the supergranule identification based on the spectrum from l = 6 to l = 250. The location of the peak or knee is marked with the vertical gray dotted lines.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: Top row: The separatrix (transparent orange surfaces), the last close field lines (red lines), and the particles that produce the highest 95% of the total γ-ray emission (black points) for the separatrix zone model number 6, ﹩\dot{{ \mathcal E }}\approx {10}^{38}\,\mathrm{erg}\,{{\rm{s}}}^{-1}﹩, and for the indicated α values. Bottom row: The same model cases as those presented in the top row but from a point of view that is located along the rotational axis. The red arrows denote the particle velocities, i.e., photon direction. For α = 15°, no high-emitting particles appear inside the LC. For α = 45°, high-emitting particles start appearing inside the LC near the rotational equator, which implies that the Y point in that region is formed inside the LC. This effect increases gradually with α. Thus, for α = 75° the Y point, i.e., the origin of reconnection, near the rotational equator, is located well inside the LC, at ≈0.8R LC. High-emitting particles inside the LC introduce additional features in the sky maps, e.g., ring-type structures, that result in secondary peaks of the γ-ray light curves. Nonetheless, for the separatrix zone model, the relative number of particles outside the LC is higher compared to the extended separatrix zone model (see Figures 19 and 18), which suppresses the corresponding four-peaked pulse profiles.
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: CR 2097 synoptic map as an example of the spherical harmonic expansion. An orthographic projection of the map centered at the equator and the longitude of 0° is adopted. (a) The original synoptic map. (b)–(d) Spherical harmonic reconstructions up to the maximum degrees ﹩{l}_{\max }=30,120﹩, and 539, respectively. The magnetic fields in panels (a)–(d) are saturated at 60, 8, 25, and 60 G, respectively.
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Spatial scale dependency of the calibration factor between the MDI and HMI spectral power. The black and gray dots are the observation data within and outside σ, the variance of the calibration factors for a given l, respectively. The blue line is the mean of the black dots and is fitted to give the scale-dependent calibration function r(l) (the red line).
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Comparison of HMI and MDI spectral power. The horizontal and vertical axes are the spectral power of HMI and MDI, respectively. The gray and black dots correspond to the spherical harmonical degrees l < 200 and l > 200, respectively. The red line represents the fixed calibration factor, 1.4, i.e., ﹩{B}_{{\rm{l}}-\mathrm{MDI}}^{2}=1.96{B}_{{\rm{l}}-\mathrm{HMI}}^{2}﹩ (1.4 for B  l ).
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: Representative particle orbits that contribute to the different sky-map components for the extended separatrix zone model of α = 75° and ﹩\dot{{ \mathcal E }}\approx {10}^{38}\mathrm{erg}\,{{\rm{s}}}^{-1}﹩. The orbits are plotted in the 3D space (left-hand column), on the projected x–y plane (middle column), while their traces on the corresponding sky map are shown in the right-hand column. The color progression along the orbits/traces denotes the time arrow (from blue to red). The green cylinder/circle in the left-hand and middle columns denote the LC.
Paper: The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: The same as Figure 2, but for CR 2098 (left) and CR 2099 (right).
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The sky maps for the extended separatrix zone model of α = 75° and for the indicated ﹩\dot{{ \mathcal E }}﹩ values.
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: From population synthesis, each combination of binary evolution prescription and disk instability model yields an observed LMXB mass distribution with a substantial fraction of mass-gap BHs (for ﹩{M}_{\mathrm{NS},\mathrm{birth}-\max }=3{M}_{\odot }﹩). Left: the detection probability-weighted fraction of LMXBs with mass gap BHs, f low(p detect), is presented against the unweighted fraction, f low−intrinsic, for each model (using either no transition to RIA, a sharp transition, or a smooth transition). For points that fall above the dashed black line, detection effects lead to a dearth of mass-gap BH detections relative to the intrinsic population. Right: the p discover detection-weighted fraction of LMXBs with a mass-gap BH is presented against the p transition-weighted fraction. This panel breaks down the two components of the LMXB detection probability: (i) being bright enough during outburst for discovery p discover and (ii) transitioning from outburst to quiescence during the survey p transition. Relative to p transition, weighting by p discover suppresses observation of mass-gap BHs.
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: Top: the detection-weighted fraction of LMXBs with a mass-gap BH f low(p detect) as a function of ﹩{M}_{\mathrm{NS},\mathrm{birth}-\max }﹩. Each color corresponds to a different RIA transition. For each panel, the results for no transition to RIA overlap with the results for a smooth transition to RIA. Bottom: the average number of detections of AIC LMXBs (over N trials = 5000 snapshots of the evolutionary tracks) with M BH < 4.5M ⊙ (as a solid line); the dashed horizontal line is the average number of detections of LMXB that formed with a BH and have M BH < 4.5M ⊙; the dotted horizontal line is the average number of detections of LMXB (from any formation channel) with M BH > 4.5M ⊙. The left column presents the results from the MESA grid, while the right column presents the results from the COSMIC grid. While MESA and COSMIC predict similar LMXB BH mass distributions when ﹩{M}_{\mathrm{NS},\mathrm{birth}-\max }=3{M}_{\odot }﹩, MESA produces a dearth of LMXBs with mass gap BHs relative to COSMIC if ﹩{M}_{\mathrm{NS},\mathrm{birth}-\max }\lesssim 2{M}_{\odot }﹩.
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: The detection-weighted fraction of LMXBs with a mass-gap BH f low(p detect) as a function of ﹩{M}_{\mathrm{NS},\ \mathrm{birth}-\max }﹩ for a selection of populations. Fractions for each population are calculated by averaging over all 5000 snapshots, and the uncertainties are taken from the 68% uncertainty across the snapshots. Lowering the maximum NS birth mass ﹩{M}_{\mathrm{NS},\ \mathrm{birth}-\max }﹩ reduces the occurrence of LMXB systems with M BH < 4.5M ⊙. The magnitude of this trend depends on the adopted accretion prescription; changing the magnetic braking prescription moderately affects the fraction of mass-gap BH detections, while modifying the adopted accretion physics significantly affects f low(p detect).
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: The differences in the orbital period and mass distributions between COSMIC and MESA both originate from the treatment of RLO mass accretion. Relative to COSMIC, evolving LMXBs with MESA leads to greater mass accretion by the BHs, and by extension, shorter orbital periods. Here, the evolution tracks of a single LMXB evolved with MESA (dashed lines) are presented against the evolution tracks when COSMIC is used (solid lines). The binary is initialized with M BH = 2.5M ⊙, M donor = 1.16M ⊙, and P = 0.413 days. For the COSMIC evolution tracks, the magnetic braking formulation of H02 and the State-dependent accretion efficiency were adopted.
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: X-ray outburst light curves for a typical LMXB system for a range of BH masses and transitions to RIA. On the left, we assume no transition to RIA and vary the BH mass with fixed orbital period and companion mass. On the right, we present the sharp and smooth transitions to RIA for fixed BH mass. Both panels assume M donor = 0.7M ⊙, P = 10 hr, and d = 8 kpc. The shaded gray region highlights where the X-ray luminosity drops below the detectable limit (10 mCrab). All luminosities have been converted to the 2–10 keV range by dividing the bolometric luminosity by f corr = 4.
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: The BH mass (upper panels) and orbital period (lower panels) distributions for a selection of synthetic Galactic LMXB samples. Detection probabilities are calculated with no transition to RIA. Each panel corresponds to a different set of binary evolution prescriptions. For each presented population α = 5, the minimum q at ZAMS follows the Lifetime-limited prescription, and ﹩{M}_{\mathrm{NS},\mathrm{birth}-\max }=3.0{M}_{\odot }﹩. The solid lines represent the average distribution across all 5000 snapshots of the evolution tracks, and the shaded regions demarcate the 16th–84th percentiles. AIC LMXBs are highlighted in purple. The detection-weighted BH mass and orbital period distributions of LMXBs from population synthesis are broadly insensitive to changes in the adopted binary evolution prescriptions.
Paper: Investigating the Lower Mass Gap with Low-mass X-Ray Binary Population Synthesis
Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry, Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera, Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra, Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing, Emmanouil Zapartas
Figure caption: The LMXB orbital period distribution for the MESA grid is presented in the left column, while the orbital period distributions of the COSMIC grids (which are generated with matching initial conditions) are presented on the right. Top: Monte Carlo sampled orbital period distributions are presented for three subpopulations of LMXBs: AIC LMXBs (purple), LMXBs with intrinsic BHs in the mass gap (gold), and LMXBs with intrinsic BHs above the mass gap (gray). Bottom: Monte Carlo sampled and detection-weighted orbital period distributions for the entire population of LMXBs are presented for either no transition to RIA (blue) or a sharp transition (teal); here, applying a smooth transition to RIA is nearly indistinguishable from applying no transition. LMXBs evolved using MESA typically occupy shorter orbital periods than LMXBs evolved with COSMIC.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: (a) SDO/HMI radial field magnetogram of the main sunspot. The black curve corresponds to the dark filament seen in the Hα image shown in (b) and the SDO/AIA 304 Å image in (c). (d) SDO/AIA 1600 Å image shown in reversed color scale (where black is bright). Two ribbons are marked, which are also outlined as green contours in (a). The red curve represents the magnetic polarity inversion line. (e) SDO/AIA 131 Å image shown in reversed color scale. The blue and red contours show radial magnetic fields of −500 G and 300 G, respectively. (f) EOVSA microwave source at multiple frequencies (50% contours) overlaid on SDO/AIA 171 Å image. They are colored from red to blue, according to the color bar on the right. The FWHM beam sizes at different frequencies used to restore the EOVSA images are shown at the bottom left corner in the same color scheme.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: Schematic of the solar jet event associated with escaping energetic electrons. (a) Before the jet eruption, a minifilament lies at the southwest side of the main sunspot, where an opposite magnetic polarity is present. (b) During the jet eruption, a bright flare arcade is formed due to magnetic reconnection trailing the erupting minifilament. Energetic electrons trapped in the arcade produce the high-frequency microwave (MW) source via incoherent gyrosynchrotron emission (the blue shade). The purple shaded region represents the complex interaction region between the erupting filament and different ambient magnetic field lines. Energetic electrons entering this region could have access to these field lines and escape with a wide opening angle (see the text for further discussion). As a result, a low-frequency microwave source is formed due to coherent plasma radiation (the red shade), which appears to subtend a much wider angle than that of the highly collimated EUV jet spire.
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: PFSS model mapped to the synoptic HMI magnetogram for Carrington Rotation 2216. The blue, red, and purple dots denote the locations of the PSP, WIND, and STEREO-A spacecraft, ballistically mapped from 0.37 au, 1 au, and 1 au, respectively, to the source surface at 2.5 R ⊙ following the Parker spiral. They are all magnetically connected to AR 12738, as shown by the PSFF field lines (the green, red, and purple curves). However, while both WIND and PSP are well connected to the jet region (marked by the yellow open circle), STEREO-A is connected to the opposite side of the AR, far away from the jet region. The black solid line is the source surface magnetic neutral line mapped to the solar surface.
Paper: Alfvén Wave Connection between the Chromosphere and the Corona of the Sun: An Analytical Study
Authors: Jongchul Chae, Kyoung-Sun Lee
Figure caption: Illustration of a layer of finite extent where the Alfvén speed varies from v A,0 to v A,1. If the Alfvén speed varies with a constant gradient, this layer is a constant gradient layer. The transmission ﹩{ \mathcal T }﹩ of this layer can be determined by specifying the progressive integrated flux ﹩{{\mathfrak{F}}}_{\mathrm{in},{\rm{p}}}﹩ in the input layer of uniform medium (the region of s < s 0) and determining the output integrated flux ﹩{{\mathfrak{F}}}_{\mathrm{out}}﹩ in the output layer of uniform medium (the region of s > s 1).
Paper: The Solar Origin of an In Situ Type III Radio Burst Event
Authors: Meiqi Wang, 美祺 王, Bin Chen, 彬 陈, Sijie Yu, 思捷 余, Dale E. Gary, Jeongwoo Lee, Haimin Wang, Christina Cohen
Figure caption: Evolution of the multifrequency EOVSA microwave source from 1.6 GHz to 12 GHz, shown as 50% contours colored from red to blue for (a) the preflare phase and (c)–(e) during the peak time. All the background is an SDO/AIA 171 Å image. The corresponding times in (c)–(e) are shown as red arrows in the cross-power microwave dynamic spectrum in (b). The white curve shows the 1.6 GHz light curve. The two orange dashed lines in (b) show the initiation times of the interplanetary type III radio bursts discussed in Section 2.2. The EOVSA beam sizes are shown at the bottom left corner in (a).
Paper: Alfvén Wave Connection between the Chromosphere and the Corona of the Sun: An Analytical Study
Authors: Jongchul Chae, Kyoung-Sun Lee
Figure caption: Plots of transmission ﹩{ \mathcal T }﹩ on ω in the case of τ 1 = 2 in the constant gradient model and in the exponential model, respectively. The two models have the values of v A at the bottom and at the top.
Paper: Alfvén Wave Connection between the Chromosphere and the Corona of the Sun: An Analytical Study
Authors: Jongchul Chae, Kyoung-Sun Lee
Figure caption: Spatial variation of ρ 1/4 v  R  at a high frequency (left) and at a low frequency (right) in the cases of progressive waves (C = 1, D = 0, top) and regressive waves (C = 0, D = 1, bottom) in a constant gradient layer of thickness τ 1 = 2.
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: Plot of the average EUV flux series (black solid line) at 60Â°N as a function of time (day) in 2021. Panel (a) shows the original time series and its fitted polynomial curve (red dotted line), panel (b) shows the series after detrending, and panel (c) shows the series after bandpass filtering.
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: Gaussian fitting of the first secondary peak of autocorrelograms at 60°N (left panel) and 60°S (right panel) in 2021. The red scattered points are autocorrelation coefficients, and the blue solid line is the fitted Gaussian function curve. The black vertical dotted line goes from the peak point of the Gaussian curve to the horizontal coordinate.
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: The autocorrelogram of average EUV time series at latitude 60°N (top) and 60°S (bottom) in 2021. The dotted line represents the series before bandpass filtering, while the solid line represents the series after bandpass filtering.
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: The spectrograms of detrended average EUV flux series at 60°N in 2021. The top panel shows the series before bandpass filtering, while the bottom panel shows the series after bandpass filtering. The color bar represents amplitude, to which logarithmic calculation (20log(amplitude)) is applied.