adsabs/AstroCLIMB huggingface dataset:
Paper: Tilted Dark Halos Are Common and Long-lived, and Can Warp Galactic Disks
Authors: Jiwon Jesse Han, Vadim Semenov, Charlie Conroy, Lars Hernquist
Figure caption: Evolution of Halo 533060. In the top panel, we plot the tilt angle of the dark (stellar) halo in blue (red) dots with 1σ error bars estimated from jackknifing. X-marks indicate where the tilt angle uncertainties are larger than 10°. The colored shaded lines are cubic spline interpolations of the data, sampled from their statistical errors. In the bottom panel, we show the major-to-intermediate and the major-to-minor ratios of the dark/stellar halo, which we refer to as the “flattening parameters.” We gray out the regions in which both flattening parameters are close to 1, indicating that the halo is near spherical. In this region, the tilt angle is not well defined. Once the halo becomes aspherical around 5 Gyr ago, the tilt angle steadily decreases from 60° to 20° at present day.
Paper: Tilted Dark Halos Are Common and Long-lived, and Can Warp Galactic Disks
Authors: Jiwon Jesse Han, Vadim Semenov, Charlie Conroy, Lars Hernquist
Figure caption: Relationship between the dark halo and the stellar halo tilt angles. Each point shows the dark halo and stellar halo tilt angle at one snapshot, spanning all of the halos and lookback times from Figure 1. The pink shaded region marks the measured Galactic stellar halo tilt from Han et al. (2022a), and the blue histogram on the right panel shows the marginal distribution of the Milky Way’s dark halo. The blue horizontal line shows the most likely value of the Galactic dark halo to be 20°.
Paper: Tilted Dark Halos Are Common and Long-lived, and Can Warp Galactic Disks
Authors: Jiwon Jesse Han, Vadim Semenov, Charlie Conroy, Lars Hernquist
Figure caption: Correspondence between the warp amplitude and the dark halo tilt. On the top panel we plot the evolution of the dark halo tilt as in Figure 3. On the bottom panel we plot the amplitude of the disk warp measured at twice the scale radius. When the tilt angle is zero, the warp amplitude is also zero. After the tilt angle rises to its maximum, the disk responds by warping in a Gyr or so. The warp amplitude is stable, and slowly declines over 4 Gyr with the declining tilt angle of the dark halo.
Paper: Tilted Dark Halos Are Common and Long-lived, and Can Warp Galactic Disks
Authors: Jiwon Jesse Han, Vadim Semenov, Charlie Conroy, Lars Hernquist
Figure caption: Stellar disk of Halo 533060 plotted at four snapshots. The tilt of the dark halo settles at around 5 Gyr (see Figure 3). Z denotes the vertical height of the star, and R denotes the cylindrical radius with positive (negative) sign where the angles are ±90° within the positive (negative) vertical extremum of the warp. We overplot an analytic fit to the warp (power law in radius and sinusoid in azimuth) in blue, with dotted regions marking 1σ uncertainties of the fit. A strong warp persists over >4 Gyr.
Paper: Quasi-simultaneous Optical Flux and Polarization Variability of the Binary Super Massive Black Hole Blazar OJ 287 from 2015 to 2023: Detection of an Anticorrelation in Flux and Polarization Variability
Authors: Alok C. Gupta, Pankaj Kushwaha, Mauri J. Valtonen, Sergey S. Savchenko, Svetlana G. Jorstad, Ryo Imazawa, Paul J. Wiita, Minfeng Gu, Alan P. Marscher, Zhongli Zhang, Rumen Bachev, G. A. Borman, Haritma Gaur, T. S. Grishina, V. A. Hagen-Thorn, E. N. Kopatskaya, V. M. Larionov, E. G. Larionova, L. V. Larionova, D. A. Morozova, T. Nakaoka, A. Strigachev, Yulia V. Troitskaya, I. S. Troitsky, M. Uemura, A. A. Vasilyev, Z. R. Weaver, A. V. Zhovtan
Figure caption: Simultaneous optical flux and polarization light curves of OJ 287 from 2015 to 2023, with the R magnitudes at the bottom and the PD and PA in the middle and upper panels, respectively.
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Composition and thermodynamic evolution of the blue tracer particle shown in Figure 7, which produces a high mass fraction of 44Ti. The dotted vertical lines indicate the times picked for the snapshots in Figure 7. The top panel displays the temperature and density history of the particle. The bottom panel shows the corresponding evolution of the mass fractions of several isotopes as obtained by the postprocessing of this trajectory. The nonmonotonic temperature evolution, in particular the peaks at around 3.7 and 4.8 s, increases the 44Ti mass fraction.
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Time series of 2D slices of the entropy in the 3D SN model. Markers indicate the current positions of a number of tracer particles and lines illustrate the projection of the path of the particles onto the plane of the slice within 200 ms around the time of the snapshot. One particle that very efficiently produces 44Ti (see Figure 6) is highlighted in blue. The temperature at the location of the highlighted particle as well as the time after core bounce are shown above each panel. The times of the snapshots are also indicated in Figure 6. Only the highlighted particle is always located in the plane of the slice, which is rotated slightly from the initial orientation, as indicated by the tripod in each panel. The other particles that are shown in black are projected onto this slice. In the last panel, all particles are within 1000 km of the plane.
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Yields of 44Ti and 56Ni obtained in this study (red star) compared to examples of 1D calculations from Sukhbold et al. (2016) for their calibrations N20+Z9.6 and W18+Z9.6 and from Curtis et al. (2019) for their “s” and “w” progenitor sets. There is a clear enhancement of 44Ti for the same 56Ni mass due to the characteristics of the 3D model. The blue star indicates the result we obtain from the extrapolation of the tracer particles after the first ∼2 s of the simulation (see Section 3.4).
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Distribution of the 44Ti mass fraction in matter that is ejected until 2 s. Nucleosynthesis calculations extrapolating the tracer particle evolution after 2 s are compared to the results based on the long-time hydrodynamic evolution of the same ejected particles until 7 s. Contributions from tracer particles that give the same results in both cases are on the diagonal, which is indicated as a black dotted line. The visible shift toward the lower right reflects the trend of higher mass fractions of 44Ti in the long-time simulation.
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Histogram of the distribution of the ejecta mass as a function of the Ti/Fe ratio. Here, “Fe” represents the Fe group, including all isotopes of Fe, Co, and Ni.
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Distribution of the ejecta vs. entropy and Y e, evaluated for each tracer particle when it cools down to 8 GK.
Paper: Production of 44Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae
Authors: Andre Sieverding, Daniel Kresse, Hans-Thomas Janka
Figure caption: Production factors of stable isotopes after radioactive decay relative to the solar abundances from Asplund et al. (2009). The isotope 45Sc is co-produced with Fe-group elements.
Paper: The Puzzling Properties of the MACS1149-JD1 Galaxy at z = 9.11
Authors: Massimo Stiavelli, Takahiro Morishita, Marco Chiaberge, Claudio Grillo, Nicha Leethochawalit, Piero Rosati, Stefan Schuldt, Michele Trenti, Tommaso Treu
Figure caption: Ratio of ﹩\mathrm{log}([{\rm{O}}\,{\rm\small{III}}]\lambda 88\,\mu {\rm{m}}/[{\rm{O}}\,{\rm\small{III}}]\lambda 5007)﹩ as a function of the electron temperature for a set of our cloudy models. Triangles are for n  e  = 100, squares for n  e  = 300, and stars for n  e  = 1000. The red square with an error bar is for JD1 and the blue square for ERO S04590. The inset shows the change of ﹩\mathrm{log}([{\rm{O}}\,{\rm\small{III}}]\lambda 88\,\mu {\rm{m}}/[{\rm{O}}\,{\rm\small{III}}]\lambda 5007)﹩ as a function of electron density for an electron temperature of 16,000 K. The red lines give the measured value for JD1, and its errors and the blue lines highlight the inferred values of the electron density.
Paper: The Puzzling Properties of the MACS1149-JD1 Galaxy at z = 9.11
Authors: Massimo Stiavelli, Takahiro Morishita, Marco Chiaberge, Claudio Grillo, Nicha Leethochawalit, Piero Rosati, Stefan Schuldt, Michele Trenti, Tommaso Treu
Figure caption: Ratio of Hγ/Hβ (lower panel) and Hδ/Hβ (upper panel) as a function of the electron density. The red dashed line shows the measured value of the ratio for JD1 with the dotted lines showing the 1σ error bars. The green dashed line shows the Case B value of the ratio for 104 K, with the dotted lines showing the 5 × 103 K and 2 × 104 K Case B values. Black squares represent a multitude of cloudy models with varying properties, while the blue squares show the values for the ratio in Gutkin et al. (2016) models.
Paper: The Puzzling Properties of the MACS1149-JD1 Galaxy at z = 9.11
Authors: Massimo Stiavelli, Takahiro Morishita, Marco Chiaberge, Claudio Grillo, Nicha Leethochawalit, Piero Rosati, Stefan Schuldt, Michele Trenti, Tommaso Treu
Figure caption: (Left) Spectral energy distribution of JD1 inferred by gsf (orange solid line; Section 7). Observed NIRCam + HST photometric fluxes (red circles; inverted triangles for 2σ upper limits) and NIRSpec MSA G235M+G395M spectra (black lines) are included in the fit. Note that the observed fluxes are presented with 2σ uncertainties and not corrected for magnification. (Right) Zoomed-in plots of the continuum-subtracted spectra around strong emission lines. The blue diamonds are the fitted spectrum (orange line) convolved with the filter passbands.
Paper: The Puzzling Properties of the MACS1149-JD1 Galaxy at z = 9.11
Authors: Massimo Stiavelli, Takahiro Morishita, Marco Chiaberge, Claudio Grillo, Nicha Leethochawalit, Piero Rosati, Stefan Schuldt, Michele Trenti, Tommaso Treu
Figure caption: Direct oxygen metallicity measurement vs. the R 23 ratio for JD1, ERO S04590 (blue) and other objects (cyan points) with auroral based measurements (Laseter et al. 2023; Nakajima et al. 2023). For reference, the vertical color lines are for Gutkin et al. (2016) models with increasing ionization parameter U from bottom to top.
Paper: The Puzzling Properties of the MACS1149-JD1 Galaxy at z = 9.11
Authors: Massimo Stiavelli, Takahiro Morishita, Marco Chiaberge, Claudio Grillo, Nicha Leethochawalit, Piero Rosati, Stefan Schuldt, Michele Trenti, Tommaso Treu
Figure caption: Stamp images of MACS1149-JD1 in HST F160W and NIRCam filters (2.″4 × 2.″4). The MSA slits of the four visits (#20–23) are overlaid in the F277W stamp image. The pseudo two-color image using the F356W (blue) and F444W (red) filters, which corresponds to the Balmer break, is shown (right bottom).
Paper: Quasi-simultaneous Optical Flux and Polarization Variability of the Binary Super Massive Black Hole Blazar OJ 287 from 2015 to 2023: Detection of an Anticorrelation in Flux and Polarization Variability
Authors: Alok C. Gupta, Pankaj Kushwaha, Mauri J. Valtonen, Sergey S. Savchenko, Svetlana G. Jorstad, Ryo Imazawa, Paul J. Wiita, Minfeng Gu, Alan P. Marscher, Zhongli Zhang, Rumen Bachev, G. A. Borman, Haritma Gaur, T. S. Grishina, V. A. Hagen-Thorn, E. N. Kopatskaya, V. M. Larionov, E. G. Larionova, L. V. Larionova, D. A. Morozova, T. Nakaoka, A. Strigachev, Yulia V. Troitskaya, I. S. Troitsky, M. Uemura, A. A. Vasilyev, Z. R. Weaver, A. V. Zhovtan
Figure caption: Variation of PD and PA with respect to R-band magnitude for different segments of light curves of OJ 287 from 2015 to 2023. Symbols of different colors are as in Figure 1.
Paper: Quasi-simultaneous Optical Flux and Polarization Variability of the Binary Super Massive Black Hole Blazar OJ 287 from 2015 to 2023: Detection of an Anticorrelation in Flux and Polarization Variability
Authors: Alok C. Gupta, Pankaj Kushwaha, Mauri J. Valtonen, Sergey S. Savchenko, Svetlana G. Jorstad, Ryo Imazawa, Paul J. Wiita, Minfeng Gu, Alan P. Marscher, Zhongli Zhang, Rumen Bachev, G. A. Borman, Haritma Gaur, T. S. Grishina, V. A. Hagen-Thorn, E. N. Kopatskaya, V. M. Larionov, E. G. Larionova, L. V. Larionova, D. A. Morozova, T. Nakaoka, A. Strigachev, Yulia V. Troitskaya, I. S. Troitsky, M. Uemura, A. A. Vasilyev, Z. R. Weaver, A. V. Zhovtan
Figure caption: Enlargements of portions of the observations shown in Figure 1, divided into eight segments in which segment 3 is divided into two subsegments. Symbols of different colors are the same as in Figure 1.
Paper: Quasi-simultaneous Optical Flux and Polarization Variability of the Binary Super Massive Black Hole Blazar OJ 287 from 2015 to 2023: Detection of an Anticorrelation in Flux and Polarization Variability
Authors: Alok C. Gupta, Pankaj Kushwaha, Mauri J. Valtonen, Sergey S. Savchenko, Svetlana G. Jorstad, Ryo Imazawa, Paul J. Wiita, Minfeng Gu, Alan P. Marscher, Zhongli Zhang, Rumen Bachev, G. A. Borman, Haritma Gaur, T. S. Grishina, V. A. Hagen-Thorn, E. N. Kopatskaya, V. M. Larionov, E. G. Larionova, L. V. Larionova, D. A. Morozova, T. Nakaoka, A. Strigachev, Yulia V. Troitskaya, I. S. Troitsky, M. Uemura, A. A. Vasilyev, Z. R. Weaver, A. V. Zhovtan
Figure caption: Variation of PD and PA with flux using the simultaneous optical flux and polarization data (within < 15 minutes) of OJ 287 from 2015 to 2023. Symbols of different colors are the same as in Figure 1.
Paper: Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group 
Authors: Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Figure caption: Top left: CMD of the stellar population of Pavo from the IMACS imaging. The blue and green isochrones indicate the main-sequence and HeB phases of 150 and 500 Myr old populations, respectively. The metallicity in both cases is set to [M/H] = −1.5 to roughly match that of Leo P. The orange isochrone shows the location of an ancient and metal-poor (10 Gyr and [M/H] = −2.5) RGB. Top middle: background CMD created by downsampling the CMD of the full field of view (minus the region containing Pavo) to an area equal to the white dotted ellipse in Figure 2. Top right: CMD of the stellar population within the orange dashed ellipse (Figure 2). The RGB isochrone from the left panel is reproduced here. In all three top panels, the dashed line indicates the 50% completeness limit, the dotted line indicates the 90% limit, and the error bars on the left indicate the typical photometric uncertainties in bins of 0.5 mag in the r band. Bottom left: binned version of the CMD of the NW region of Pavo (0.1 mag bins). Bottom middle: same CMD with the background contribution subtracted. Bottom right: binned CMD of the background over the entire field of view (with Pavo excluded), weighted by five times the area of the region used in the bottom left and middle CMDs (to make it more clearly visible on the same scale). The 10 Gyr, [M/H] = −2.5 PARSEC isochrone (at a distance of 1.99 Mpc) is overlaid in orange.
Paper: Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group 
Authors: Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Figure caption: IMACS g + r color image of Pavo. The central and SE portions of its irregular stellar body are dominated by blue stars, but it also extends to the NW, where older, redder stars become the dominant population. The white dotted ellipse shows the region used to produce the full CMD of Pavo (Figure 3, top left), and the orange dashed ellipse shows the region dominated by redder stars (Figure 3, top right). The field contains many foreground stars, and the apparent central cluster of Pavo is actually a superimposed foreground star with detectable proper motion. We have marked this star with a red cross.
Paper: Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group 
Authors: Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Figure caption: Map of the positions of blue, g − r < 0 (blue points), and RGB (orange points) stars (both) brighter than m  r  = 26. The gray points show the locations of bright stars from Gaia DR3 (m  G  < 19.5) with point sizes scaled by apparent brightness. The dashed black ellipse indicates the half-light radius of Pavo (Table 1). It is the same ellipse as in Figure 2.
Paper: Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group 
Authors: Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Figure caption: Pavo on the size–luminosity relation with various other Local Volume dwarfs included for comparison. Note that Pavo is at the upper limit of the scatter in effective radius (for its magnitude), while all of the highlighted comparison dwarfs are at the lower limit of the scatter.
Paper: Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group 
Authors: Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Figure caption: Supergalactic XY (top) and YZ (bottom) projections showing objects in the nearby galaxies catalog (Karachentsev & Kaisina 2019). Pavo is shown with a blue star. Several other notable dwarf galaxies that we refer to are highlighted for comparison.
Paper: Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group 
Authors: Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Figure caption: DECaLS DR10 gri cutout of Pavo, similar to that used for the original classification.
Paper: First Metis Detection of the Helium D3 Line Polarization in a Large Eruptive Prominence
Authors: Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Figure caption: Plot of the observed ratios Q/I and U/I. Theoretical ratios due to Thomson scattering are also shown for two deviations from the Metis PoS.
Paper: First Metis Detection of the Helium D3 Line Polarization in a Large Eruptive Prominence
Authors: Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Figure caption: Electron column densities (per square centimeter) and the ratio of orthohelium density to electron density for two extreme solutions within the northern prominence arm.
Paper: Spatial Extent of Molecular Gas, Dust, and Stars in Massive Galaxies at z ∼ 2.2–2.5 Determined with ALMA and JWST
Authors: Ken-ichi Tadaki, Tadayuki Kodama, Yusei Koyama, Tomoko L. Suzuki, Ikki Mitsuhashi, Ryota Ikeda
Figure caption: The JWST 4.4 μm images (4″ × 4″) for our sample of 10 massive SFGs (left and center columns in each panel). Magenta contours display the 870 μm flux densities in the ALMA 0.″2-resolution images, plotted for every 4σ. Cyan contours do the velocity-integrated flux of CO J = 3 − 2 emission in the same image, plotted for every 4σ. The right columns in each panel show the residual 4.4 μm images after the best-fit model is subtracted. Magenta, cyan, and black filled ellipses at the bottom-left corner correspond to the FWHM of PSF in the 870 μm, CO, and 4.4 μm images, respectively. Green lines show the regions masked in measuring the effective radii of the 4.4 μm emission. White crosses show the central position of the best-fit model in the JWST 4.4 μm image.
Paper: Irregular Proton Injection to High Energies at Interplanetary Shocks
Authors: Domenico Trotta, Timothy S. Horbury, David Lario, Rami Vainio, Nina Dresing, Andrew Dimmock, Joe Giacalone, Heli Hietala, Robert F. Wimmer-Schweingruber, Lars Berger, Liu Yang
Figure caption: Event overview. (a) EPD-Electron Proton Telescope (EPT) particle flux (sunward aperture). (b) EPD-STEP particle flux (magnet channel averaged over the entire field of view). (c) Pitch-angle distributions for ions with an energy of 0.011–0.019 MeV in the spacecraft frame. (d) Time profile of the STEP energy flux in the 0.012–0.015 MeV energy channel at full resolution (blue) and time-averaged using a 1 minute window. (e) SWA-PAS ion energy flux (Owen et al. 2020). (f) SWA-PAS proton density. (g) MAG burst magnetic field data in Radial-tangential-normal (RTN) coordinates (Horbury et al. 2020). The magenta line marks the shock crossing, and the black rectangle in panel (b) highlights the dispersive energetic particle enhancements observed by STEP. Differential fluxes are in E 2 · cm−2 s−1 sr−1 MeV for the EPD instruments and centimeters squared per second eV for PAS.
Paper: Irregular Proton Injection to High Energies at Interplanetary Shocks
Authors: Domenico Trotta, Timothy S. Horbury, David Lario, Rami Vainio, Nina Dresing, Andrew Dimmock, Joe Giacalone, Heli Hietala, Robert F. Wimmer-Schweingruber, Lars Berger, Liu Yang
Figure caption: Left: spectrogram of the irregular signal in seconds from shock vs. 1/v axes, with the velocity dispersion shown by the solid magenta line (top). Time series showing the local θ Bn(t) angle. The red and gray dashed lines represent the average θ Bn and a 90° angle, respectively (bottom). Right: cartoon showing the corrugated shock front with local shock normal, trajectory of a reflected particle ,and the SoLO trajectory (SolO model: esa.com).
Paper: Irregular Proton Injection to High Energies at Interplanetary Shocks
Authors: Domenico Trotta, Timothy S. Horbury, David Lario, Rami Vainio, Nina Dresing, Andrew Dimmock, Joe Giacalone, Heli Hietala, Robert F. Wimmer-Schweingruber, Lars Berger, Liu Yang
Figure caption: (a) Simulation snapshot of proton density (color map). The inset shows a zoom around the shock transition (gray), and the local shock position is superimposed, with a color map corresponding to the local θ Bn. (b) Density map of upstream suprathermal protons (color map) and magnetic field lines (magenta) computed at the same simulation time as (a). The inset shows the upstream particle energy spectrum, with the dashed blue lines indicating the suprathermal energy range considered.