adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: Left-hand panel: (a): The inferred l = 2, m = 0 periods with LLS fitting, with the assumed period spacing of 20.58 s. Panel (b): The deviations between the fitted and observed periods. Right-hand panel: Distribution of the resulting fits on 1000 permutations of l = 2 modes. The lower and upper bounds represent the 16% and 84% of the distribution, respectively, indicated by vertical dashed lines in red and blue. The derived mean period spacing represents the 50% of the distribution, denoted by a vertical green line.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: The seismic analysis indicates the position of EPIC 248705247, which is denoted by a red triangle, while positions obtained from spectroscopic analysis and Gaia EDR3 photometry are depicted with blue and green dots, respectively. The 50 known DBVs are represented by black filled circles. The boundaries established by the TDC and energy leakage criteria are depicted by blue and red dashed lines. The black dashed lines represent the cooling tracks of DB stars.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: Panel (a): The inferred l = 1, m = 0 periods with LLS fitting, with the assumed period spacing of 35.88 ± 1.66 s. Panel (b): The deviations between the fitted and observed periods. Panel (c): The average splittings for each radial order, with the error bar indicating the deviation from the average l = 1 frequency splitting.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: I-V (upper panel), K-S (middle panel), and F-T (bottom panel) significance tests to search for a constant period spacing in the case of EPIC 248705247. The tests are applied to the pulsation periods listed in Table 1. A period spacing of ΔΠ1 ≈ 36 s is found to be evident.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The E  p –T 90 plane (left) and the HR–T 90 plane (right). The colors of the data points from red to blue represent the probability of classification as LGRB from 0% to 100%. The dashed line is the cutoff where the probability of LGRBs is 50%. The lime, violet, crimson, and light sea green squares represent the Group A, B, C, and D GRBs and MGFs, respectively.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: Left-hand panel: Contours of 1/χ 2 on the M/M ⊙ vs. T eff plane. Right-hand panels: Upper right-hand panel (a): Chemical composition profiles of oxygen, carbon, and helium as a function of the outer mass fraction from our best-fit model. Lower right-hand panel (b): The corresponding logarithm of the squared Brunt–Väisälä frequency.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: Parameterization of the oxygen abundance profile to the spectroscopic measurements of EPIC 248705247.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: Period spacing diagram for EPIC 248705247.
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: Long-term light curve of the blazar 4FGL J2139.4−4235, where the purple dashed line is the result of fitting the light curve with a sinusoidal function. Top panel: 30 day-binned Fermi-LAT light curve at 0.3–300 GeV from 2008 August 4 to 2023 December 10, with test statistic >9. Middle panel: the red positive triangles and green inverted triangles represent the V-band light curves from CRTS observations and ASAS-SN observations, respectively. Bottom panel: Gaia light curve at G band from 2014 September 15 to 2017 May 21, spanning ∼979 days.
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: The resulting PSD analysis for the γ-ray light curve of 4FGL J2139.4−4235. The black line represents the source periodogram, while the red circle, orange square, and blue solid line represent the best-fit PSD for the power law, broken power law, and bending power law, respectively. The purple horizontal dashed line is the Poisson noise level. The inset in the panel shows the probability distribution calculated by the PSRESP method with spectral indices ranging from 0.0 to 2.0 in steps of 0.1. The solid red line is the result of fitting a Gaussian function to the data.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The E  p,z –E iso plane, including the trajectories of Group A and C GRBs and LGRBs without z (top) and Group B and D GRBs and SGRBs without z (bottom). The red and blue solid lines are the best-fit lines for SGRBs and LGRBs fitted by the Markov Chain Monte Carlo method, respectively, and both are ﹩{E}_{p{,}z}\propto {E}_{\mathrm{iso}}^{0.37}﹩. The gold solid line is the translation of ﹩{E}_{p{,}z}\propto {E}_{\mathrm{iso}}^{0.37}﹩. The blue dashed lines are the 2σ confidence regions. The lime, violet, crimson, light sea green, gold, royal blue, dark magenta, coral, and gray dashed lines are the trajectories that change with redshift (gradually increasing from the left to the right) of Group A, B, C, and D GRBs, MGFs, GRB 100816026, GRB 161001045, GRB 180618030, and LGRBs/SGRBs, respectively. The gold, royal blue, dark magenta, coral, and gray rings are MGFs, GRB 100816026, GRB 161001045, and GRB 180618030 at their corresponding redshifts. The red points are SGRBs. The blue points and rings are LGRBs and LL-LGRBs, respectively. The green squares and rings are Type I LGRBs and their MEs.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The L iso–τ 31,z  plane. The black solid line is the possible dividing line. The red solid line is the best-fit line for Type I GRBs/SGRBs. The red dashed lines are the confidence regions of 2σ. The redshift increases gradually from the bottom right to the top left.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The ε–T 90,z  plane. The gray dotted lines are ε = 0.03 and T 90,z  = 5 s. The red rings and points are SGRBs and Type I GRBs. The blue rings and points are LGRBs and Type II GRBs. The redshift increases gradually from the bottom right to the top left.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The EH–T 90,z  plane. The gray dotted line is EHD = 2.6. The redshift increases gradually from the top right to the bottom left.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The redshift distributions of all GRBs with known redshift (left) and their CDFs (right). The red dotted line represents the best fit with a log-normal function.
Paper: Unveiling the Progenitors of a Population of Likely Peculiar Gamma-Ray Bursts
Authors: Si-Yuan Zhu, Pak-Hin Thomas Tam
Figure caption: The τ 31 distributions of Group A, B, C, and D GRBs, Type I GRBs, and Type II GRBs.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: SFHs of 14 massive quiescent galaxies grouped into Group-1: early formation and early quenching (left column); Group-2: early formation and recent quenching (middle column); and Group-3: recent formation and recent quenching (right column). The green and yellow–green shades include 1σ and 2σ of the posteriors at each SFH time bin, and the green line shows the 50th percentile of the posteriors at each time bin. The dashed black line shows the SFH from MAP. The blue and orange arrows indicate the formation (z form) and quenching epoch (z quench), and the sky-blue and orange bars show the 16th to 84th percentiles of z form and z quench, respectively. The red dashed slope shows the quenching speed, v quench (see the text for the definition). The 3D-HST IDs and light-weighted stellar age are shown at the upper right corner of each panel. We classify 14 massive quiescent galaxies into three groups based on their formation and quenching histories (early/recent formation and early/recent quenching) and identify five galaxies in Group-1, five galaxies in Group-2, and four galaxies in Group-3.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: (a) SFR averaged over the most recent 30 Myr shown as a function of galaxy stellar mass. Galaxies are color-coded by light-weighted ages. The error bar indicates the 16th and 84th percentiles of the SFR. The different symbols indicate the different Prospector setups used: fitting only photometry (crosses) and fitting both photometry and NIRSpec data (circles). The purple dotted line shows the SFMS at z ∼ 2 from K. E. Whitaker et al. (2014), and the blue dashed line shows the SFMS at z ∼ 2.46 (median redshift of the Blue Jay sample) from J. Leja et al. (2022). We select 14 quiescent galaxies located 1 dex below the SFMS from J. Leja et al. (2022) at their respective redshifts (the gray shaded region shows 1 dex below the SFMS at z = 2.46 for a visual guide). Most of our quiescent galaxies also satisfy sSFR < 0.2/t univ(z), which is shown as the red dashed line. (b) Fraction of quiescent galaxies as a function of galaxy stellar mass. The error bar includes the 1σ confidence interval from the binomial distribution (e.g., E. Cameron 2011). We find that the mass trend of the quenched fractions in the Blue Jay sample is consistent with other observations of large photometric samples at similar redshifts.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Prospector fitting results of an example Blue Jay galaxy, COSMOS-11142. (a) Observed photometry is shown with circles (blue: HST/ACS+WFC3; green: JWST/NIRCam). The best-fit SED model is shown in red. (b) NIRSpec data (in arbitrary units) is shown as a blue line, and the best-fit spectrum is again shown as a red line. (c) Nonparametric SFH derived from fitting using the continuity SFH prior. The green and yellow–green shades include 1σ and 2σ of the posteriors at each SFH time bin. The green line shows the 50th percentile of the posteriors at each time bin, and the dashed black line shows the SFH from MAP. (d) Posterior distribution of the stellar and dust parameters: (1) redshift (z spec); (2) stellar mass (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })﹩); (3) stellar velocity dispersion (σ ⋆); (4) metallicity ([Fe/H]); (5) light-weighted stellar ages (agelight); (6) optical depth for the diffuse dust component (τ old); (7) optical depth for the birth-cloud component (τ young); and (8) the power-law modifier to the shape of the D. Calzetti et al. (2000) dust attenuation curve (n).
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: SFHs of the same 14 massive quiescent galaxies derived using the bursty SFH prior, in the same format as Figure 4. The empty orange arrow and the hatched bar indicate the first (earliest) quenching epoch (the median and 16th to 84th percentiles) that happened more than 1 Gyr before the “main” quenching event (see the text in Section 3 for how the first/second and main quenching events are defined). We find that the SFHs overall look consistent for galaxies in Group-1 and Group-3. However, the galaxies in Group-2, with stellar ages of ∼1 Gyr, show different SFHs when different SFH priors are used: steady formation with nearly constant SFRs until recent quenching (continuity prior) vs. repeated bursts and rapid quenching (bursty prior). Broadly, the formation and quenching epochs and the stellar ages derived from continuity and bursty priors are consistent (see also Figure A5).
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption:  Fourteen Blue Jay massive quiescent galaxies in the plane of formation (﹩{t}_{\mathrm{form}}^{\mathrm{lbt}}﹩) and quenching epochs (﹩{t}_{\mathrm{quench}}^{\mathrm{lbt}}﹩), both in lookback time in Gyr. We classify them into three groups based on these two epochs. Group-1 (red region): galaxies that are early formed and early quenched. Group-2 (green region): galaxies that are early formed and recently quenched. Group-3 (blue region): galaxies that are recently formed and recently quenched. We identify five galaxies in Group-1, five in Group-2, and four in Group-3.
Paper: Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Song Wang, Xue Li, Henggeng Han, Jifeng Liu
Figure caption: Comparison of photospheric FUV emission estimated using the method presented in this paper and that from S. Crandall et al. (2020).
Paper: Benchmarking Dielectronic Recombination Rate Coefficients for Carbon-like Ca14+ 
Authors: C. Y. Zhang, B. S. Yan, K. Wang, R. Si, K. Yao, W. L. Ma, Z. K. Huang, W. Q. Wen, X. W. Ma, L. F. Zhu, C. Y. Chen, N. R. Badnell
Figure caption: Comparison of the rate coefficients for Ca14+ from the old FAC (W. Q. Wen et al. 2020), old AS (W. Q. Wen et al. 2020), and new FAC multi-n CI calculations. The measured recombination spectrum (W. Q. Wen et al. 2020) is also presented. The strong resonance peaks are labeled based on the new FAC multi-n CI calculation, and the core electrons 1s 2 are omitted.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: Fermi gamma-ray SED of RCW 38. For each data point, the error bar reflects the statistical uncertainty caused by the effective area. The blue dashed line represents the best-fit PL model, which has a photon index of Γ = 2.34 ± 0.04. The total photon flux produced by the best-fit model in the 0.1–500 GeV band is ﹩{{\rm{\Phi }}}_{\gamma }^{\gt 100\mathrm{MeV}}=(2.35\pm 0.17)\times {10}^{-8}﹩ ph cm−2 s−1, corresponding to a gamma-ray luminosity of L  γ  = (2.66 ± 0.92) × 1034 erg s−1 for a distance of 1.7 kpc.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: Multiwavelength image of RCW 38, with 3.6 μm IR Spitzer image in red (S. J. Wolk et al. 2006), the Chandra broadband X-ray (0.5−7.0  keV) in green, and the background-subtracted 2−300 GeV Fermi-LAT counts map in blue. The gamma-ray emission region is coincident with the IR and X-ray emission.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: Counts map of the 6° × 6° region centered on 4FGL J0859.2−4729 in the 0.2–300 GeV band. The green circle shows the extension of the Vela Jr SNR. The two X's show the position of PSR J0855−4644 and PSR J0855−4658, which are present within 1° of J0859.2−4729.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: TS map of the 2–300 GeV band centered on RCW 38 with a pixel size of 0.05° × 0.05°. The green contours reflect the distribution of the 3.6 μm emission of the star-forming region observed by Spitzer (E. Winston et al. 2012), with the inner contour showing the extent of the star cluster powering RCW 38. The maximum TS value of ≈13 in the central two pixels is spatially coincident with the star cluster and corresponds to a ≈3.6σ detection in the 2–300 GeV band.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: Chandra X-ray spectra of RCW 38 with the best-fit model (which included a thermal and a PL component). The red points are the data points with error bars and the solid curves represent the best-fit models. From the thermal component, we derive the properties of the hot gas, including hot-gas temperature kT and electron number density n e.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: Hard X-rays (2−7 keV) from RCW 38 with point sources removed. The IRS 2 binary star system is highlighted by the magenta circle.
Paper: Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency Using Gamma-Ray Emission from the Star-forming Region RCW 38
Authors: Paarmita Pandey, Laura A. Lopez, Anna L. Rosen, Todd A. Thompson, Tim Linden, Ian Blackstone
Figure caption: Three-color image of RCW 38 combining Chandra broadband X-ray data (green), Fermi gamma-ray TS map of 1 degree (blue), and Spitzer IR data (red). The gamma-ray TS map represents the 2−300 GeV energy range with 0.05° spatial resolution.
Paper: Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, Y. J. Wang, X. W. Tan
Figure caption: Continuous wavelet power spectra of the IMFs of three typical examples of the daily radio flux at 245 (top panel), 2695 (middle panel), and 8800 (bottom panel) MHz during the time interval considered. The thick black contours represent the 99.9% confidence level, and the black dashed line depicts the cone of influence, where edge effects may distort the picture.
Paper: Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, Y. J. Wang, X. W. Tan
Figure caption: The temporal variation of the rotation cycle lengths for the daily radio flux at 245, 410, 610, 1415, 2695, 4995, and 8800 MHz during the time interval considered. In order to clearly compare the rotation cycle lengths of radio flux across different frequencies, the rotation cycle lengths for only two adjacent frequencies are displayed in a single panel. The rotation cycle lengths of different frequencies from low to high frequencies are arranged top to bottom.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Left: UNCOVER spectroscopy of three z ∼ 6.3 objects with bright [O III] emission; blue and red curves indicate the medium-band filters used to represent the continuum, while the green curve shows the filter containing the strong line. Center: three-color PSF-convolved images of each source. Right: continuum and line maps for each source. While ID 10522 appears pointlike in both continuum and line emission, both 12053 and 31282 exhibit complex morphologies, with three separate clumps at the same redshift, and clear spatial offsets between continuum and line emission.
Paper: Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, Y. J. Wang, X. W. Tan
Figure caption: Top panel: the radio flux at 245, 2695, and 8800 MHz during the year 2000. Bottom panel: the IMFs representing the signals of solar rotation cycle for solar radio flux at 245, 2695, and 8800 MHz during the same time interval.
Paper: Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, Y. J. Wang, X. W. Tan
Figure caption: Three typical examples of daily solar radio flux at 245, 2695, and 8800 MHz from 1989 January 1 to 2019 December 17 ranked from left to right.
Paper: Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
Authors: N. B. Xiang, X. H. Zhao, L. H. Deng, F. Y. Li, Y. J. Wang, X. W. Tan
Figure caption: Top panel: the IMFs representing the signals of solar rotation cycle for solar radio flux at 245, 410, and 610 MHz. Bottom panel: same as the top panel but for solar radio flux at 1415, 2695, 4995, and 8800 MHz.