adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Gravitational-wave Bursts from Black Hole Binaries in the Galactic Center with LISA
Authors: Alan M. Knee, Jess McIver, Smadar Naoz, Isobel M. Romero-Shaw, Bao-Minh Hoang, Evgeni Grishin
Figure caption: Period and eccentricity recovery for two simulated 30 M ⊙ + 20 M ⊙ BHBs orbiting a Sgr A*-like SMBH at the Galactic center, assuming different outer orbit inclinations relative to the line of sight. The initial outer orbit for the system in the top (bottom) row is given by a out = 100 au (a out = 250 au) and e out = 0.01, and the initial inner orbit is given by a = 0.15 au (a = 0.2 au), e = 0.5 (e = 0.7), and ι = 85° (ι = 86°). The left panels show periodograms of the Q-transform triggers obtained for each source, where the dashed vertical lines are the inner orbital period. The right panels are the estimated eccentricities if the orbital period is inferred from the highest peak in the respective periodogram. The dashed black curves show the true eccentricity evolution.
Paper: Detecting Gravitational-wave Bursts from Black Hole Binaries in the Galactic Center with LISA
Authors: Alan M. Knee, Jess McIver, Smadar Naoz, Isobel M. Romero-Shaw, Bao-Minh Hoang, Evgeni Grishin
Figure caption: Eccentricity errors, ∣δ e∣ (Equation (6)), for simulated BHBs with masses m 1 = 30 M ⊙ and m 2 = 20 M ⊙ orbiting an M SMBH = 4 × 106 M ⊙ at the Galactic center. As before, the initial outer orbital parameters are a out = 100 au, e out = 0.01, and ι = 85° in all simulations. Each source is plotted at its maximum eccentricity, and ∣δ e∣ (marker colors) is averaged over a month of data centered on this time. For simulations with fewer than two detected bursts (black cross), we cannot measure the orbital period or eccentricity. The dashed gray contours are lines of constant peak GW frequency assuming a 30 M ⊙ + 20 M ⊙ BHB.
Paper: Detecting Gravitational-wave Bursts from Black Hole Binaries in the Galactic Center with LISA
Authors: Alan M. Knee, Jess McIver, Smadar Naoz, Isobel M. Romero-Shaw, Bao-Minh Hoang, Evgeni Grishin
Figure caption: Schematic diagram of a hierarchical triple system. The inner binary (blue ellipse), consisting of two masses m 1 and m 2, orbits around a tertiary mass M on a wide outer orbit (gray ellipse). The angle ι is the relative inclination between the inner and outer orbital planes. In this work, we focus on triples where the inner binary is a stellar-mass BHB and the tertiary body is an SMBH.
Paper: Glimmers in the Cosmic Dawn: A Census of the Youngest Supermassive Black Holes by Photometric Variability 
Authors: Matthew J. Hayes, Jonathan C. Tan, Richard S. Ellis, Alice R. Young, Vieri Cammelli, Jasbir Singh, Axel Runnholm, Aayush Saxena, Ragnhild Lunnan, Benjamin W. Keller, Pierluigi Monaco, Nicolas Laporte, Jens Melinder
Figure caption: Cosmic evolution of SMBH abundance. The comoving number density of SMBHs, n SMBH, is plotted vs. redshift, z. The observational constraint derived by counting z = 6–7 AGN in the HUDF variability survey is shown by the red open square, and the lower bound shows the Poisson uncertainty. The red open diamond corrects for variability incompleteness, and the red filled diamond is for luminosity incompleteness (see text). Previous observational estimates at z = 0 from local galaxies (Banik et al. 2019) and at z = 4–7 from broad emission line sources (Harikane et al. 2023) are shown with the black square and diamonds, respectively. For the z ∼ 4–7 sources, we are unable to make any correction for the fraction of nonaccreting SMBHs and leave all points as lower limits. Various Pop III.1 formation models (Banik et al. 2019; Singh et al. 2023) with isolation distance parameters, d iso, from 50 to 200 kpc (proper distance) are shown by the colored solid lines. At low redshifts, these decrease compared to the maximum value attained (dotted lines) due to mergers. The green dashed line shows SMBH seeding based on an HMT above a mass of 7.1 × 1010 M ⊙ (Vogelsberger et al. 2014), with the shaded region illustrating a factor of 2 variation in this mass scale. The magenta dashed line shows results from a model of SMBH formation via “direct collapse” (Chon et al. 2016).
Paper: Glimmers in the Cosmic Dawn: A Census of the Youngest Supermassive Black Holes by Photometric Variability 
Authors: Matthew J. Hayes, Jonathan C. Tan, Richard S. Ellis, Alice R. Young, Vieri Cammelli, Jasbir Singh, Axel Runnholm, Aayush Saxena, Ragnhild Lunnan, Benjamin W. Keller, Pierluigi Monaco, Nicolas Laporte, Jens Melinder
Figure caption: Photometric variability of 1051264 at z = 2 (upper panels) and 1052126 at z = 3.2 (lower panels) sources. We show difference images of F105W and F140W to the left, where the earlier epoch is subtracted from the later. The color bar is symmetric around 0, so black objects get brighter with time and white objects become fainter. Panels to the right show the ACS/F606W image taken in 2005, averages of the F105W and F140W images over both epochs at which they were observed, and the JWST F277W image. Intensity images are calibrated in MJy Sr−1 with color bars shown to the side. Cutouts are 2.″4 × 2.″4.
Paper: Glimmers in the Cosmic Dawn: A Census of the Youngest Supermassive Black Holes by Photometric Variability 
Authors: Matthew J. Hayes, Jonathan C. Tan, Richard S. Ellis, Alice R. Young, Vieri Cammelli, Jasbir Singh, Axel Runnholm, Aayush Saxena, Ragnhild Lunnan, Benjamin W. Keller, Pierluigi Monaco, Nicolas Laporte, Jens Melinder
Figure caption: Light curve for object 1052123. The lower x-axis shows the year of observation, while the upper x-axis shows the time since 2008 accounting for (1 + z). The left axis shows the observed apparent magnitude, while the right axis shows the absolute magnitude for z = 6.74. Filters are shown in color.
Paper: Glimmers in the Cosmic Dawn: A Census of the Youngest Supermassive Black Holes by Photometric Variability 
Authors: Matthew J. Hayes, Jonathan C. Tan, Richard S. Ellis, Alice R. Young, Vieri Cammelli, Jasbir Singh, Axel Runnholm, Aayush Saxena, Ragnhild Lunnan, Benjamin W. Keller, Pierluigi Monaco, Nicolas Laporte, Jens Melinder
Figure caption: JWST/NIRISS spectra of the sources shown in Figure 1. The three different wavelength regions show the F115W, F150W, and F200W filters, while the two spectra per wavelength range show extractions when the spectra are dispersed in the direction of rows or columns.
Paper: Glimmers in the Cosmic Dawn: A Census of the Youngest Supermassive Black Holes by Photometric Variability 
Authors: Matthew J. Hayes, Jonathan C. Tan, Richard S. Ellis, Alice R. Young, Vieri Cammelli, Jasbir Singh, Axel Runnholm, Aayush Saxena, Ragnhild Lunnan, Benjamin W. Keller, Pierluigi Monaco, Nicolas Laporte, Jens Melinder
Figure caption: Same as Figure 1 for the z = 6–7 sources.
Paper: Glimmers in the Cosmic Dawn: A Census of the Youngest Supermassive Black Holes by Photometric Variability 
Authors: Matthew J. Hayes, Jonathan C. Tan, Richard S. Ellis, Alice R. Young, Vieri Cammelli, Jasbir Singh, Axel Runnholm, Aayush Saxena, Ragnhild Lunnan, Benjamin W. Keller, Pierluigi Monaco, Nicolas Laporte, Jens Melinder
Figure caption: Same as Figure 1 for the probable supernovae.
Paper: Swift J1727.8–1613 Has the Largest Resolved Continuous Jet Ever Seen in an X-Ray Binary
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Steve Prabu, Thomas D. Russell, Pikky Atri, Francesco Carotenuto, Diego Altamirano, Sara E. Motta, Lucas Hyland, Cormac Reynolds, Stuart Weston, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, Simone Migliari, David M. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: Intensity profile along the northern and southern jets as a function of separation from the core in the VLBA observation of Swift J1727.8–1613 shown in Figure 2. The intensity profiles are calculated by fitting one-dimensional Gaussians perpendicular to the jet axis at intervals of ∼1 mas. The dashed line shows the contribution from the core, calculated by multiplying the intensity of the core by the profile of the restoring beam along the jet axis, with the shaded region showing its uncertainty (derived from the fit).
Paper: Swift J1727.8–1613 Has the Largest Resolved Continuous Jet Ever Seen in an X-Ray Binary
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Steve Prabu, Thomas D. Russell, Pikky Atri, Francesco Carotenuto, Diego Altamirano, Sara E. Motta, Lucas Hyland, Cormac Reynolds, Stuart Weston, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, Simone Migliari, David M. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: Constraints on the intrinsic speed and inclination of the extended and discrete jets seen in the VLBA observation in Figure 2. The solid lines show the nominal values and the shaded areas show the 1σ uncertainties. We derive these constraints from the brightness ratio of the approaching and receding arms of the extended jet (Equation (1)) and the proper motion of the southern jet knot (Equation (5)). The brightness ratio puts an upper limit on the jet inclination and a lower limit on the intrinsic speed of the continuous jet.
Paper: Swift J1727.8–1613 Has the Largest Resolved Continuous Jet Ever Seen in an X-Ray Binary
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Steve Prabu, Thomas D. Russell, Pikky Atri, Francesco Carotenuto, Diego Altamirano, Sara E. Motta, Lucas Hyland, Cormac Reynolds, Stuart Weston, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, Simone Migliari, David M. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: Comparison of polarization angles and the position angle of the resolved jet of Swift J1727.8–1613. The background image is the same as shown in Figure 2. We plot the polarization measured by the Sub-Millimeter Array at 1.3 mm (SMA; Vrtilek et al. 2023), the Australia Telescope Compact Array (ATCA) at 5.5 and 9 GHz (Ingram et al. 2023), and the Imaging X-ray Polarimetry Explorer (IXPE; Dovciak et al. 2023; Ingram et al. 2023; Veledina et al. 2023). The shaded arcs represent the reported 1σ error intervals, with the lines showing their nominal values. The polarization observations span the hard and hard-intermediate states and are consistent with the north–south orientation of the resolved jet in our VLBI observations.
Paper: Swift J1727.8–1613 Has the Largest Resolved Continuous Jet Ever Seen in an X-Ray Binary
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Steve Prabu, Thomas D. Russell, Pikky Atri, Francesco Carotenuto, Diego Altamirano, Sara E. Motta, Lucas Hyland, Cormac Reynolds, Stuart Weston, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, Simone Migliari, David M. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: First VLBI image of Swift J1727.8–1613 with the VLBA. The contours mark ﹩\pm \sigma \times {\sqrt{2}}^{n}﹩ mJy beam−1, where n = 3, 4, 5, …, and σ is the rms noise shown in the lower left of the image. The ellipse in the lower-right corner shows the synthesized beam. The image shows a bright core with highly resolved (∼40 mas) apparently asymmetric bipolar jets extending in the north–south direction, and a discrete jet knot to the south at a separation of 66.7 ± 0.2 mas from the core at a position angle of 179.4° ± 0.15° east of north.
Paper: Swift J1727.8–1613 Has the Largest Resolved Continuous Jet Ever Seen in an X-Ray Binary
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Steve Prabu, Thomas D. Russell, Pikky Atri, Francesco Carotenuto, Diego Altamirano, Sara E. Motta, Lucas Hyland, Cormac Reynolds, Stuart Weston, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, Simone Migliari, David M. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: MAXI light curve of the evolution of Swift J1727.8–1613 at the beginning of its 2023 outburst. The times of our four VLBI observations are marked by the vertical lines, and their details are given in Table 1.
Paper: Swift J1727.8–1613 Has the Largest Resolved Continuous Jet Ever Seen in an X-Ray Binary
Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Steve Prabu, Thomas D. Russell, Pikky Atri, Francesco Carotenuto, Diego Altamirano, Sara E. Motta, Lucas Hyland, Cormac Reynolds, Stuart Weston, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, Simone Migliari, David M. Russell, Craig L. Sarazin, Gregory R. Sivakoff, Roberto Soria, Alexandra J. Tetarenko, Valeriu Tudose
Figure caption: VLBI images of the resolved jet of Swift J1727.8–613 during the hard state. The contours mark ﹩\pm \sigma \times {\sqrt{2}}^{n}﹩ mJy beam−1, where n = 3, 4, 5, …, and σ is the rms noise shown in the lower-left of each image. The ellipse in the lower-right corner of each image shows the synthesized beam. The observation parameters can be found in Table 1 and the image parameters can be found in Table 2. The jet is resolved over multiple epochs during the hard state, but appears less extended as the source moves toward the hard-intermediate state.
Paper: Observations of Locally Excited Waves in the Low Solar Atmosphere Using the Daniel K. Inouye Solar Telescope
Authors: Shah Mohammad Bahauddin, Catherine E. Fischer, Mark P. Rast, Ivan Milic, Friedrich Woeger, Matthias Rempel, Peter H. Keys, Thomas R. Rimmele
Figure caption: A local wave front originating from a subsurface source in the simulated solar photosphere. Top row: the wavefield is discernible in the pressure field, yet its visibility is limited in DKIST/VBI-resolution synthesized G-band, blue-continuum, and Ca II K (NLTE) channels due to weak SNR. Bottom row: to improve visibility, three-difference temporal filtering (Bahauddin & Rast 2021, 2023) is applied to denoise the images. Even in the temporal-difference images, the wavefield remains absent in the Ca II K channel. In both rows, green arrows highlight the location of the wave fronts.
Paper: Observations of Locally Excited Waves in the Low Solar Atmosphere Using the Daniel K. Inouye Solar Telescope
Authors: Shah Mohammad Bahauddin, Catherine E. Fischer, Mark P. Rast, Ivan Milic, Friedrich Woeger, Matthias Rempel, Peter H. Keys, Thomas R. Rimmele
Figure caption: Four local wave fronts identified during a 15 minute observation window by DKIST/VBI in a ∼5 × 5 arcsec2 field of view. Green arrows mark the spatial location of these wave fronts.
Paper: Trojan Globular Clusters: Radial Migration via Trapping in Bar Resonances
Authors: Adam M. Dillamore, Stephanie Monty, Vasily Belokurov, N. Wyn Evans
Figure caption: Present day energy E vs. z-component of angular momentum L  z  for GCs (left-hand panel), stars with [Fe/H] < −1 (middle panel), and our test particle simulation with a rotating bar (right-hand panel). In each panel the large red points mark the 10 selected GCs with the largest mean changes in L  z  due to the slowing bar. The black dotted line in the left-hand panel marks the boundary between accreted (higher E) and in situ (lower E) GCs according to Belokurov & Kravtsov (2023, 2024), and the Sun is marked with a ⊙ symbol.
Paper: Trojan Globular Clusters: Radial Migration via Trapping in Bar Resonances
Authors: Adam M. Dillamore, Stephanie Monty, Vasily Belokurov, N. Wyn Evans
Figure caption: Energy E vs. angular momenta L  z  of GCs in our sample. The black dotted line marks the boundary between in situ (lower E) and accreted (higher E) clusters. The colors indicate mean change in energy ΔE as the bar’s pattern speed slows from Ωb = 80 to 35 km s−1 kpc−1. Most of the GCs with ΔE > 0 are located around L  z  ∼ 1000 kpc km s−1 and E ∼ −0.7 × 105 km2 s−2.
Paper: Trojan Globular Clusters: Radial Migration via Trapping in Bar Resonances
Authors: Adam M. Dillamore, Stephanie Monty, Vasily Belokurov, N. Wyn Evans
Figure caption: Changes in the orbits of the 10 GCs in a slowing barred potential. The top and bottom rows show the present day t = 0 and t = t 0 ≈ −5.24 Gyr, at which the pattern speeds are Ωb = 35 and 80 km s−1 kpc−1, respectively. The left- and right-hand columns show energy vs. angular momentum and apocenter vs. pericenter, respectively. Each of the 10 clusters is on average at lower energy and angular momentum at the earlier time. In some cases (e.g., M22) the pericenters are also considerably smaller than their current values.
Paper: Trojan Globular Clusters: Radial Migration via Trapping in Bar Resonances
Authors: Adam M. Dillamore, Stephanie Monty, Vasily Belokurov, N. Wyn Evans
Figure caption: Final snapshots of the tidal tail simulations of 47 Tuc in the axisymmetric (left-hand panel), steadily rotating barred (middle panel), and slowing barred (right-hand panel) MW potentials. The particles are shown in on-sky coordinates centered on the cluster, marked by the black cross. The two black circles indicate the radial range (95–308 pc) of the diffuse extended halo observed by Piatti (2017). The right-hand panel shows the projected density of the stripped stars as a function of projected radius, with the two radii again marked. The bar causes the tidal tails to be much more diffuse, creating an extended halo around the cluster with a flat density profile.
Paper: Trojan Globular Clusters: Radial Migration via Trapping in Bar Resonances
Authors: Adam M. Dillamore, Stephanie Monty, Vasily Belokurov, N. Wyn Evans
Figure caption: Cluster core radii taken from Baumgardt & Hilker (2018) as a function of the average change in position between our initial and final snapshots (initial—present day). Note the possible trend of increasing core radius (reflecting little internal dynamical evolution) as a function of decreasing change in position (change in tidal forces) among our trapped GCs. The only outliers to the trend are the young, metal-rich GC Pal 11 (discussed in Section 4.1) and the ancient, metal-poor GC NGC 4372 (Section 4.3). Possible explanations for both are given in the corresponding sections.
Paper: Trojan Globular Clusters: Radial Migration via Trapping in Bar Resonances
Authors: Adam M. Dillamore, Stephanie Monty, Vasily Belokurov, N. Wyn Evans
Figure caption: Orbits of the 10 selected GCs in the Sormani et al. (2022) potential rotating with a constant pattern speed of Ωb = 35 km s−1 kpc−1. The frame shown is corotating with the bar (gray ellipse), and the current positions of the Sun and the GCs are shown with the ⊙ and red points, respectively. In all, 6 of the 10 GCs (e.g., 47 Tuc) orbit close to the CR, since they remain on one side of the bar.
Paper: Observation of a Fully-formed Forward–Reverse Shock Pair due to the Interaction between Two Coronal Mass Ejections at 0.5 au
Authors: Domenico Trotta, Andrew P. Dimmock, Xochitl Blanco-Cano, Robert J. Forsyth, Heli Hietala, Naïs Fargette, Andrea Larosa, Noé Lugaz, Erika Palmerio, Simon W. Good, Juska E. Soljento, Emilia K. J. Kilpua, Emiliya Yordanova, Oreste Pezzi, Georgios Nicolaou, Timothy S. Horbury, Rami Vainio, Nina Dresing, Christopher J. Owen, Robert F. Wimmer-Schweingruber
Figure caption: Overview of some available remote-sensing observations of the 2022 March CME–CME interaction event. Coronagraph observations of (a) CME1 and (b) CME2 from the (top) SOHO and (bottom) STEREO-A viewpoints. The rightmost panels show the GCS wireframe projected onto each plane-of-sky view. (c) Time–elongation map built using data from the COR2, HI1, and HI2 cameras on board STEREO-A. The tracks of CME1 and CME2 are indicated with teal and magenta arrows, respectively, and the combined track after interaction is shown by orange arrows. The time-dependent elongation angles of Solar Orbiter and Earth are highlighted via light blue and green dashed lines, respectively. (d) Orbit plot showing the relative positions of Solar Orbiter, Earth, and STEREO-A during 2022 March 7. The propagation directions of the two CMEs according to the GCS results are shown with arrows, while the dashed lines indicate the fields of view of the SoloHI (blue), HI1-A (red), and HI2-A (orange) heliospheric imagers.
Paper: Observation of a Fully-formed Forward–Reverse Shock Pair due to the Interaction between Two Coronal Mass Ejections at 0.5 au
Authors: Domenico Trotta, Andrew P. Dimmock, Xochitl Blanco-Cano, Robert J. Forsyth, Heli Hietala, Naïs Fargette, Andrea Larosa, Noé Lugaz, Erika Palmerio, Simon W. Good, Juska E. Soljento, Emilia K. J. Kilpua, Emiliya Yordanova, Oreste Pezzi, Georgios Nicolaou, Timothy S. Horbury, Rami Vainio, Nina Dresing, Christopher J. Owen, Robert F. Wimmer-Schweingruber
Figure caption: Summary of Solar Orbiter observations. Energetic ion differential fluxes (in E2 · cm−2 s−1 sr−1 MeV) as measured by (a) EPD’s Sun-directed Electron Proton Telescope (EPT) and (b)Supra Thermal Electron Proton (STEP) sensor. (c) MAG normal mode magnetic field magnitude and components in spacecraft-centered Radial–Tangential–Normal (RTN) coordinates (Fränz & Harper 2002). (d)–(e) Proton bulk flow speed, proton density, and temperature as measured by SWA Proton Alpha Sensor (PAS). (f) Plasma total pressure (﹩{{\rm{P}}}_{\mathrm{tot}}={{\rm{n}}}_{p}\ {{\rm{k}}}_{B}\ {{\rm{T}}}_{p}+\tfrac{{{\rm{B}}}^{2}}{2{\mu }_{0}}﹩, where k B  and μ 0 are the Boltzmann constant and the vacuum magnetic permeability, respectively). (g) One-dimensional energy flux (in cm−2s−1 eV) measured by PAS. (h) Element abundance ratios measured by the SWA Heavy Ion Sensor (HIS). (i) Integrated pitch angle distributions for electrons with energies larger than 100 eV as measured by SWA Electron Analyser Sensor (EAS; in cm−2 s−1 eV). The continuous, dashed–dotted and dashed lines show the times at which Solar Orbiter crosses the CME1 wave and the forward and reverse shocks, respectively.
Paper: Observation of a Fully-formed Forward–Reverse Shock Pair due to the Interaction between Two Coronal Mass Ejections at 0.5 au
Authors: Domenico Trotta, Andrew P. Dimmock, Xochitl Blanco-Cano, Robert J. Forsyth, Heli Hietala, Naïs Fargette, Andrea Larosa, Noé Lugaz, Erika Palmerio, Simon W. Good, Juska E. Soljento, Emilia K. J. Kilpua, Emiliya Yordanova, Oreste Pezzi, Georgios Nicolaou, Timothy S. Horbury, Rami Vainio, Nina Dresing, Christopher J. Owen, Robert F. Wimmer-Schweingruber
Figure caption: (a)–(g) Zoom on the interaction region as in Figure 1 without the energetic particles spectrogram. The vertical orange shaded regions correspond to reconnection exhaust crossings. (h) Simplified sketch representing the event assuming head-on interaction with the identified areas within the interaction and the Solar Orbiter trajectory (spacecraft model: https://www.esa.int/Science_Exploration/Space_Science/Solar_Orbiter). (i) Three-dimensional plot of magnetic field vectors in RTN for the event. Yellow, red, and blue arrows are measurements taken in CME1, interaction, and CME2 regions, respectively. The magenta/orange planes represent the forward–reverse shock pair.
Paper: Observation of a Fully-formed Forward–Reverse Shock Pair due to the Interaction between Two Coronal Mass Ejections at 0.5 au
Authors: Domenico Trotta, Andrew P. Dimmock, Xochitl Blanco-Cano, Robert J. Forsyth, Heli Hietala, Naïs Fargette, Andrea Larosa, Noé Lugaz, Erika Palmerio, Simon W. Good, Juska E. Soljento, Emilia K. J. Kilpua, Emiliya Yordanova, Oreste Pezzi, Georgios Nicolaou, Timothy S. Horbury, Rami Vainio, Nina Dresing, Christopher J. Owen, Robert F. Wimmer-Schweingruber
Figure caption: Wind observations of the event at 1 au (shaded area). From top to bottom: magnetic field magnitude and components in RTN (a), proton bulk flow speed and tangential flows ((b), (c)), protons density and temperature (d). The magenta line marks the forward shock crossing.