adsabs/AstroCLIMB huggingface dataset:
Paper: Hi-C 2.1 Observations of Reconnection Nanojets
Authors: Ritesh Patel, Vaibhav Pant
Figure caption: Multiwavelength AIA observations of two nanojets, N4 and N7, observed in Hi-C FOV. The jet N8, being small, could not be distinguished from the background in AIA resolution. The upper and lower panels correspond to the two jets observed in AIA 304, 171, and 193 Å, respectively, from left to right. (c) The jet N3 is barely visible in 193 Å but no sign for jet N7 could be seen in (f) for the same channel.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Point-spread function (PSF) in 30° × 30° maps at 166 MHz. The four maps show the field center and 25°, 50°, 75° away from the field center. The white area in the 75° plot is beyond the horizon. The full width at half maximum of the synthesized main beam at the field center is 50–60 arcminutes, close to the diffraction limit defined by the longest baseline. Grating lobes are seen in hexagonal patterns, which are distorted as we move away from the field center, especially in the 75° away map. As shown, DOM provides direction-dependent PSF information across the sky. The grating lobes cause the difference between the original and the convolved GSM08 in Figure 5. The peak values change because of the primary-beam attenuation at the four pixels. The color bars saturate at 10% of the peak values to illustrate faint sidelobe structures.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Validation-characterized effects: horizon source and array coplanarity. Both maps are centered on the zenith. Left: a point source, with a typical flux density (0.2 Jy at 166 MHz), is added 85° away from the zenith. The source signal is picked up by the sidelobes of the primary beam and leaks into the zenith field via grating lobes at the 10−4 level. Right: noncoplanarity residual. Comparing to the original map in Figure 5, the difference increases to 5% of the original map with the GSM08 sky model.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: An example of the weight map defined in Equation (13). The map spans two hours in R.A. The fact that there is more effective weight on the left side of the region is due to lower noise (higher weighting) when observing that region, which results from longer integration time and lower intrinsic sky noise.
Paper: Direct Optimal Mapping for 21 cm Cosmology: A Demonstration with the Hydrogen Epoch of Reionization Array
Authors: Zhilei Xu, 智磊 徐, Jacqueline N. Hewitt, Kai-Feng Chen, Honggeun Kim, Joshua S. Dillon, Nicholas S. Kern, Miguel F. Morales, Bryna J. Hazelton, Ruby Byrne, Nicolas Fagnoni, Eloy de Lera Acedo, Zara Abdurashidova, Tyrone Adams, James E. Aguirre, Paul Alexander, Zaki S. Ali, Rushelle Baartman, Yanga Balfour, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, Carina Cheng, David R. DeBoer, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Randall Fritz, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Jack Hickish, Daniel C. Jacobs, Austin Julius, MacCalvin Kariseb, Joshua Kerrigan, Piyanat Kittiwisit, Saul A. Kohn, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, Anita Loots, Yin-Zhe Ma, David Harold Edward MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Tshegofalang Mosiane, Steven G. Murray, Abraham R. Neben, Bojan Nikolic, Hans Nuwegeld, Aaron R. Parsons, Nipanjana Patra, Samantha Pieterse, Jonathan C. Pober, Nima Razavi-Ghods, James Robnett, Kathryn Rosie, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter Van Van Wyngaarden, Peter K. G. Williams, Haoxuan Zheng
Figure caption: Diagram of the direct optimal mapping. The two major modules, data conditioning and mapping, are displayed on the left; the detailed steps are shown in the flowchart. More details of each step are described in Section 3.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: The upper panel displays a 4170 Å continuum image of the full ROSA field of view in proper heliocentric coordinates. The green box outlines the quiescent region used for the calculation of intensity thresholds that are used to define the pore boundaries, the blue box highlights the region of interest displayed in the lower panel, and the red box contains the reference magnetic structure (yellow). The lower panel shows the five pores, labeled in ascending order from left to right, with pore 1 (P1) being blue, pore 2 (P2) orange, pore 3 (P3) green, pore 4 (P4) yellow, and pore 5 (P5) red.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Temporally and spatially averaged Ca II 8542 Å profile for the full field of view (including pores, small-scale magnetic elements, and quiet-Sun locations). The blue line illustrates the calculated line core for these observations (8542.03 Å), with the red dashed lines highlighting the percentage line depths used to calculate the corresponding bisector velocities.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Left: select spatial probability distribution cross sections, using a charge 2 VFN. The three panels are plotted on the same color scale. Middle: select spatial probability distribution cross sections, using a charge 2 PLN. The three panels are plotted on the same color scale. The parameters closest to that of the injected planet are marked with orange stars. Right: probability distributions of the FR, marginalized over the spatial dimensions. The FR of the injected planet is marked by the red line. The model fitting shows that the PLN can provide better constraints on planet model parameters compared to the VFN.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Spatial probability distributions given the correctly identified FR of 2.15 × 10−6 (the panels are plotted on the same color scale). Planets at a separation of 1.25 λ/D are injected at a variety of injected position angles (marked by the orange stars). At position angles other than 0 and π/2, additional solutions exist beyond the two guaranteed by the instrumental symmetry. However, an observing strategy that involves taking data with multiple rotations of the instrument relative to the sky will reduce the number of best-fit position angle solutions to the fundamental two.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Example ROC curves at different separations in the presence of photon noise, assuming wavefront error averages to a baseline null depth. For both vortex charges, the inclusion of other ports of the PLN provides detection gains relative to the VFN. The gray areas indicate FPRs which are not well sampled as they involve fewer than three data sets with false detections.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Mean coupling calculated over 590 frames of WFE residuals from the KPIC PyWFS, for the no vortex (left), charge 1 (middle), and charge 2 (right) configurations. The ports on the bottom axis are (from left to right): LP01, LP11a, LP11b, LP21a, LP21b, and LP02. Coupling values for ports that are not considered nulled are depicted in light gray. Off-axis planet coupling (where it is expected based on the coupling maps) remains higher than the stellar coupling in the presence of these WFE realizations.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Left: mean focal-plane PSF in the presence of WFE as measured by the KPIC PyWFS. Middle: unaberrated focal-plane PSF. Right: difference between the aberrated and ideal PSFs. A reminder that these are not simulations of the Keck PSF, but of the measured wavefront error residuals propagated through a system with an ideal circular aperture.
Paper: Efficient Detection and Characterization of Exoplanets within the Diffraction Limit: Nulling with a Mode-selective Photonic Lantern
Authors: Yinzi Xin, Nemanja Jovanovic, Garreth Ruane, Dimitri Mawet, Michael P. Fitzgerald, Daniel Echeverri, Jonathan Lin, Sergio Leon-Saval, Pradip Gatkine, Yoo Jung Kim, Barnaby Norris, Steph Sallum
Figure caption: Coupling calculated over 590 frames of WFE residuals from the KPIC PyWFS, with no vortex (top), a charge 1 vortex (middle), and a charge 2 vortex (bottom). Off-axis planet coupling (where it is expected based on coupling maps) remains higher than the stellar coupling in the presence of these WFE realizations.
Paper: Statistical Plasma Properties of the Planar and Nonplanar ICME Magnetic Clouds during Solar Cycles 23 and 24
Authors: Zubair I. Shaikh, Anil N. Raghav
Figure caption: The top two (left and right) plots represent in situ observation of two ICMEs observed by the ACE spacecraft on 2013 July 12 (left) and 2014 August 19 (right), respectively. Each subpanel from top to bottom represents the flowing parameters, total IMF, B mag, B vec = B  x , B  y , B  z , elevation (θ) and azimuth (ϕ) angle, plasma speed (V  p ), plasma density (N  p ), plasma temperature (T  p ), and plasma beta (β). The colors cyan and blue denote the sheath and MC region. The bottom (left and right) plot represents the PMS analysis test, which shows the distribution of azimuth (ϕ) vs. the elevation (θ) angle of IMF in GSE coordinates for the above two MCs. The planarity, efficiency, and normal direction of the PMS is given by ﹩\tfrac{{\lambda }_{2}}{{\lambda }_{3}}﹩, ﹩\tfrac{\langle {B}_{n}\rangle }{B}﹩, and n. The inclination of the PMS plane w.r.t. the ecliptic plane i is denoted as ﹩{\theta }_{\max }﹩. The black dotted curve represents the fitting curve (Equation 2; Shaikh et al. 2020) to the measured (dotted colored plot) ϕ and θ data (Palmerio et al. 2016; Shaikh et al. 2020). The figure showing the normal direction is in the θ–ϕ plot.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Average phase differences (red crosses) between oscillations in the Ca II 8542 Å line-of-sight velocity, v LOS, and associated line-core intensities of the pixels contained within pore P3. The error bars (blue) represent the standard deviation of the measured I–V phases at each frequency, with horizontal dashed black lines highlighting the 0° and 90° phase angles for reference.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Phase differences for frequencies detected in the displayed bisector and the 10% lower line depth, where a negative phase angle indicates the wave is detected at the lower line depth first. The average phase difference is plotted in red, with the standard deviation of each height differential shown in blue.
Paper: Statistical Plasma Properties of the Planar and Nonplanar ICME Magnetic Clouds during Solar Cycles 23 and 24
Authors: Zubair I. Shaikh, Anil N. Raghav
Figure caption: Normalized distribution of the orientation (elevation/inclination: θ axes and azimuth: ϕ axes angle) of planar and nonplanar ICMEs axes. The vertical dashed line in the left plot separates the eastward and westward directions, whereas in the right plot it separates southward and northward inclined oriented ICME axes.
Paper: Statistical Plasma Properties of the Planar and Nonplanar ICME Magnetic Clouds during Solar Cycles 23 and 24
Authors: Zubair I. Shaikh, Anil N. Raghav
Figure caption: Same as Figure 1 for ICMEs observed by the ACE spacecraft on 2010 April 5 and 2012 July 14, respectively.
Paper: Statistical Plasma Properties of the Planar and Nonplanar ICME Magnetic Clouds during Solar Cycles 23 and 24
Authors: Zubair I. Shaikh, Anil N. Raghav
Figure caption: Normalized distribution of thickness, duration, density, and magnetic compressibility in planar and nonplanar ICMEs.
Paper: Statistical Plasma Properties of the Planar and Nonplanar ICME Magnetic Clouds during Solar Cycles 23 and 24
Authors: Zubair I. Shaikh, Anil N. Raghav
Figure caption: Normalized distribution of average magnetic field and plasma parameters in planar sheaths and nonplanar ICMEs.
Paper: Statistical Plasma Properties of the Planar and Nonplanar ICME Magnetic Clouds during Solar Cycles 23 and 24
Authors: Zubair I. Shaikh, Anil N. Raghav
Figure caption: Pearson CC between the IMF and different plasma parameters for planar and nonplanar MCs. Note that, Bz mn and Bz mx are the same as Bz min and Bz max.
Paper: Milky Way's Eccentric Constituents with Gaia, APOGEE, and GALAH
Authors: G. C. Myeong, Vasily Belokurov, David S. Aguado, N. Wyn Evans, Nelson Caldwell, James Bradley
Figure caption: Distribution of the Galaxy’s eccentric populations in chemodynamical spaces similar to Figure 2 but with the GALAH–Gaia sample. For the GALAH–Gaia sample 12-dimensional chemodynamical space is used for the GMM and the projections corresponding to Figure 2 are shown. The GS/E component is marked with green (see Section 4 for more details). Panel (d) shows [Y/Fe] vs. [Fe/H].
Paper: Milky Way's Eccentric Constituents with Gaia, APOGEE, and GALAH
Authors: G. C. Myeong, Vasily Belokurov, David S. Aguado, N. Wyn Evans, Nelson Caldwell, James Bradley
Figure caption: Distribution of the Galaxy’s eccentric populations in the GALAH–Gaia sample in chemodynamical spaces similar to Figure 3 but for different two-dimensional projection of the original 12-dimensional chemodynamical space used for the GMM: (a) [Mn/Fe] vs. [Fe/H]; (b) [Na/Fe] vs. [Fe/H]; (c) [Mg/Cu] vs. [Na/Fe]; (d) [Ba/Fe] vs. [Fe/H]; (e) [Eu/Fe] vs. [Fe/H]; (f) [Ba/Eu] vs. [Fe/H].
Paper: Milky Way's Eccentric Constituents with Gaia, APOGEE, and GALAH
Authors: G. C. Myeong, Vasily Belokurov, David S. Aguado, N. Wyn Evans, Nelson Caldwell, James Bradley
Figure caption: Distribution of GMM-classified stars in the APOGEE–Gaia and GALAH–Gaia samples in chemical dimensions ([Ni/Fe], [Eu/Mg]) that are not used in the GMM. Since [Ni/Fe] and [Eu/Mg] are not used in the GMM, the GMM result does not contain the modeled mean, covariance, and σ for these dimensions. Instead, we use the GMM classified member stars for each component and fit a Gaussian representing their distribution in each projection. This fit is marked with a dashed line. The color schema follows Figures 2 and 3. (a) [Ni/Fe] vs. [Fe/H] for the APOGEE–Gaia sample; (b) [Eu/Mg] vs. [Fe/H] for the GALAH–Gaia sample; (c) [Mg/Cu] vs. [Na/Fe] for the GALAH–Gaia sample.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Evolution of current sheet at five different times. Panels from left to right show the configuration of magnetic field lines in the x-y plane, which correspond to the times (a) t = 0.45, (b) t = 1.13, (c) t = 1.43, (d) t = 1.71, and (e) t = 2.16, respectively. The units in x- and y-directions are L 0.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Typical trajectories and dynamics of randomly chosen sample of accelerated protons. Particles that start to be accelerated from different locations are displayed, and the initial position of each particle is denoted by the red filled circle. Electromagnetic fields are taken from the snapshot at t = 1.43. Panels (a), (b), and (c) show projections of proton trajectories onto the x-y, x-z, and z-y planes, respectively. Panels (d) and (e) display variations of proton energies vs. distance y and energies vs. time, respectively.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Case 1: enlarged view of the trajectory of a test proton trapped in a magnetic island at t = 1.43. (a) Projection of proton trajectory onto the x-y plane. The background image is the out-of-plane components of the electric field, with the contours showing the magnetic field lines. (b) Projections of proton trajectories onto the z-y plane. (c) The total energy as a function of its y position. (d) The evolution of particle total, parallel, and perpendicular energy of the test proton (black, red, and blue lines, respectively). The initial proton positions are shown by red circles.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Same as Figure 4, but for case 2. Motion of particles in two magnetic islands.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Same as Figure 2, but for electrons.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Correlation between the standard deviations of the solar wind parameters obtained from SWMF and OMNI observations at 1 au for CRs 1925, 1957, 1989, 2021, 2069, 2086, 2112, 2151, and 2164.
Paper: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Authors: Kalpa Henadhira Arachchige, Ofer Cohen, Andres Munoz-Jaramillo, Anthony R. Yeates
Figure caption: Comparison of the distributions for solar wind at 1 au. Shown are the SWMF results for solar wind parameters driven by real (red) and synthetic (blue) magnetogram data for CRs (a) 1925, (b) 1957, (c) 1989, (d) 2021, (e) 2069, (f) 2086, (g) 2112, (h) 2151, and (i) 2164.