adsabs/AstroCLIMB huggingface dataset:
Paper: The CIViL* Survey: The Discovery of a C IV Dichotomy in the Circumgalactic Medium of L* Galaxies
Authors: Samantha L. Garza, Jessica K. Werk, Trystyn A. M. Berg, Yakov Faerman, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara L. Ellison
Figure caption: Measured C IV column densities vs. sSFR for CIViL⋆ and the additional literature sample, with star-forming galaxies (sSFR > 10−11 yr−1) colored in blue, while passive galaxies (sSFR ≤ 10−11 yr−1) are colored in red. For galaxies in the gray shaded area, we examine their spectra and morphology, in addition to sSFR for classification. Like the previous figure, nondetections (upper limits) are represented with open symbols and arrows pointing down, while saturated detections (lower limits) are represented as filled symbols with arrows pointing up. The horizontal line signifies the detection limit of the sample. Above log10NC IV/cm−2 = 13.5, the star-forming and passive galaxy sample have detection fractions of 72﹩{}_{-18}^{+14}﹩% [21/29] and 23﹩{}_{-15}^{+27}﹩% [3/13], respectively. Upper limits exceeding the threshold are excluded from the analysis.
Paper: The CIViL* Survey: The Discovery of a C IV Dichotomy in the Circumgalactic Medium of L* Galaxies
Authors: Samantha L. Garza, Jessica K. Werk, Trystyn A. M. Berg, Yakov Faerman, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara L. Ellison
Figure caption: C IV and O VI correlations with galaxy properties. If the marker is dark/bold, they are from galaxies where both ions were observed. These observations overlay lightly shaded O VI column densities from J. Tumlinson et al. (2011) and J. K. Werk et al. (2013) and C IV observations from the combined CIViL⋆ and literature sample. Similar coloring and limit convention as Figure 3. Top: log10NC IV/cm−2 and log10NO VI/cm−2 vs. log10sSFR/yr−1. Bottom: log10NC IV/cm−2 and log10NO VI/cm−2 vs. log10M⋆M⊙. The basic dichotomy observed between star-forming (“blue cloud”) and passive (“red sequence”) galaxies seen in O VI observations (J. Tumlinson et al. 2011; S. D. Johnson et al. 2015; F. S. Zahedy et al. 2019; K. Tchernyshyov et al. 2023) is also seen in observations of C IV.
Paper: The CIViL* Survey: The Discovery of a C IV Dichotomy in the Circumgalactic Medium of L* Galaxies
Authors: Samantha L. Garza, Jessica K. Werk, Trystyn A. M. Berg, Yakov Faerman, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara L. Ellison
Figure caption: Regions of the HST/COS continuum spectrum showing the C IV λλ 1548 1550 line absorption features of the CIViL⋆ QSO–galaxy pairs set in the rest frame of each individual galaxy. For lines of sight that have multiple components, the individual fits are shown as the dashed purple line where the sum of the components is shown as the solid purple line. The red line in each spectrum represents the continuum flux error. The bottom left corner has the QSO–galaxy IDs and the reduced χ2 fit for the absorption features.
Paper: Limiting Rotation Rate of Neutron Stars from Crust Breaking and Gravitational Waves
Authors: J. A. Morales, C. J. Horowitz
Figure caption: Maximum von Mises strain vs. rotational frequency Ω in units of the Keplerian (breakup) frequency ΩK. The solid curve is for a 1.4 M⊙ star, and the dashed curve is for a 2 M⊙ star.
Paper: Helical Magnetic Field in a Massive Protostellar Jet
Authors: A. Rodríguez-Kamenetzky, A. Pasetto, C. Carrasco-González, L. F. Rodríguez, J. L. Gómez, G. Anglada, J. M. Torrelles, N. R. C. Gomes, S. Vig, J. Martí
Figure caption: The HH 80-81 jet at 5 cm. We show natural-weighted images of the total intensity I and polarization degree p in color scale and polarization angle (vectors) with an angular resolution of 10″ × 6″, PA = 4∘. The location of the driving source of the jet, IRAS 1862-2048, is indicated by a star symbol. Left: total intensity map of the entire radio jet, with dotted arrows indicating its precessional path. Dashed lines delineate the studied region, magnified in the center and right panels. Herbig–Haro objects, marking strong jet–ambient medium shocks, are also labeled. Center: polarization vectors (white segments) over total intensity (color scale); polarization degree of the emission (color scale) and total intensity (gray contours, corresponding to [10, 1000] × the rms of the I image). Both, the polarization vectors and polarization degree are shown over a total intensity signal-to-noise (SNI) > 10 and a polarized emission signal-to-noise (SNP) > 4, where the rms = 3 μJy beam−1. The synthesized beam is shown at the bottom left. The physical scale of 0.4 pc corresponds to 60′. Right: we show the variation of the polarization degree and polarization angle as a function of wavelength squared at the emission peak of both the jet and the counterjet.
Paper: Helical Magnetic Field in a Massive Protostellar Jet
Authors: A. Rodríguez-Kamenetzky, A. Pasetto, C. Carrasco-González, L. F. Rodríguez, J. L. Gómez, G. Anglada, J. M. Torrelles, N. R. C. Gomes, S. Vig, J. Martí
Figure caption: Results of the rotation measure (RM) analysis in the HH 80-81 jet. The left image shows the streamline image (obtained through the line integral convolution technique) of the component of the magnetic field parallel to the plane of the sky, over the total intensity map. In the middle panel we show the streamline image of the magnetic field parallel to the plane of the sky, over the values of the Faraday rotation obtained from our modeling of the Stokes parameters q(λ2) and u(λ2). The color scale of the RM indicates the direction of the magnetic field along the line of sight, i.e., red, away from the observer, and blue, toward the observer. Both, the magnetic field streamlines and the RM maps are shown for pixels with a signal-to-noise ratio (S/N) > 7 in both, the total intensity and the polarized emission. The 12″ × 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 beam (PA = 7∘) is shown as a white ellipse in both panels. The right panel shows a scheme depicting the 3D configuration of the magnetic field, exhibiting a helical topology, as suggested by our analysis of the polarization properties.
Paper: Helical Magnetic Field in a Massive Protostellar Jet
Authors: A. Rodríguez-Kamenetzky, A. Pasetto, C. Carrasco-González, L. F. Rodríguez, J. L. Gómez, G. Anglada, J. M. Torrelles, N. R. C. Gomes, S. Vig, J. Martí
Figure caption: Comparison of the variation of polarization parameters (p, χ, q in red, and u in blue) as a function of wavelength squared, for the simple Faraday screen model (solid line) and the observations (dots). Residuals of q and u with respect to the model predictions are also shown. The Faraday screen model fitting was conducted pixel by pixel. Six representative pixels are shown along a cross section of the jet axis, intersecting the emission peaks of both the jet (NL) and counterjet (SL), with the central point corresponding to each peak (see the illustrative image on the left; angular resolution and intensity scale can be found in Figure 1, center). The top and bottom panels show the behavior of polarization parameters with the wavelength squared for pixels selected in the north and south lobes, respectively. Error bars are indicated when larger than the symbols.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: In the context of the Wind model, this figure displays the performance comparison for the shock velocity (Vsh, left panel), the mean γ (﹩\bar{\gamma }﹩, middle panel), and predicted luminosity at 230 GHz (right panel) with three sets of mass-loss rates, ﹩{\dot{M}}_{{\rm{w}}}=1{0}^{-7}{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ (red lines), 10−5M⊙ yr−1 (purple lines), and 10−3M⊙ yr−1 (blue lines), respectively. The left panel is the comparison of Vsh between our numerical code (solid lines, labeled as “This work”) and the formula in T. J. Moriya et al. (2013) (dashed black lines, labeled as “Moriya13”), confirming the validity of our model. The middle and right panels display the performance comparison between the calculation adopted in this work (solid lines, labeled as “This work”) and in M. Hu et al. (2023) (dashed lines, labeled as “Hu23”) for ﹩\bar{\gamma }﹩, and the predicted luminosity, respectively. The ejecta energy is 2 × 1051 erg for all calculations in this figure.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: The black lines are the mass-loss rate of the shocked CSM for the Wind model (upper panel) and the Eruptive model (lower panel), and the red lines are the corresponding optical depth of the free–free absorption. For the comparison, the gray lines are the predicted scaled luminosity at +230 GHz relating to ϵB = 0.001 for the Wind model and the Eruptive model, and the triangles are the upper limit of SN 2024ggi. The top axis (labeled as “Distance”) is the distance of the shocked region to the SN.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: The predicted luminosity at 230 GHz for the Wind model (left panels) and the Eruptive model (right panels) with two sets of ϵB as ϵB = 0.1 (upper panels) and ϵB = 0.001 (lower panels), respectively. The black triangles are the 3σ upper limits of SN 2024ggi obtained from ALMA observations.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: Continuum images of SN 2024ggi at 1.3 mm taken with ALMA at three epochs. The red circles, each with a diameter of 1″, indicate the location of SN 2024ggi at the coordinate R.A./decl. = 11:18:22.087, −32:50:15.27. A color bar on the right shows the value scaling in units of mJy beam−1. The synthesized beams are shown at the bottom left of each plot.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: Left panel: the early-time millimeter-band observations of core-collapse SNe, including SN 1993J (J. A. Phillips et al. 1993; K. W. Weiler et al. 2007), SN 2008D (A. M. Soderberg et al. 2008; J. Gorosabel et al. 2010), SN 2011dh (A. Horesh et al. 2013), iPTF13bvn (Y. Cao et al. 2013), SN 2018ivc (K. Maeda et al. 2023), SN 2020oi (K. Maeda et al. 2021), SN 2023ixf (upper limits, E. Berger et al. 2023), and SN 2024ggi (3σ upper limits). The corresponding luminosity is shown in the right panel.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: The dashed and solid black lines are the mass-loss rate vs. CSM distance for the Wind model (dashed line) and the Eruptive model (solid line), respectively. The corresponding optical depth of free–free absorption is shown in red lines.
Paper: Early-time Millimeter Observations of the Nearby Type II SN 2024ggi
Authors: Maokai Hu, Yiping Ao, Yi Yang, Lei Hu, Fulin Li, Lifan Wang, Xiaofeng Wang
Figure caption: In the context of the Wind model, this figure shows the likelihood distribution of the parameter mass-loss rate ﹩{\dot{M}}_{{\rm{w}}}﹩ with ϵB = 0.1 (the red line) and ϵB = 0.001 (the cyan line), respectively.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: 1D slice of the domain along y through an X-point, for the simulation with zero guide field. The top panel shows the z-component of the nonideal electric field in units of B0; the middle panel shows the resistivity; and the bottom panel shows the electric current Jz (in blue), the number density nt (in orange), and the drift speed vdr,z/c ≃ Jz/entc (in green). In the top and middle panels, we present in blue the ground truth obtained directly from our simulation, while other colors show various choices for ηeff, as described in the legend. Our prescription for resistivity (Equation (10)) is shown as η(α, pbest) and η(α, phigh) for the values of p defined in Section 4 and corresponding α values. Regions where ∣E∣ > ∣B∣ are shaded in blue.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: A comparison between the measured nonideal electric field ﹩{E}_{z}^{* }﹩ (top left) and its reconstruction ηeffJz based on different choices of ηeff: ηS23,kin (Equation (3)) in top right, ηB24 (Equation (7)) in bottom left, and ηS23,MHD (Equation (5)) in bottom right. All panels are normalized to B0. Within each panel, horizontal black lines separate different time snapshots: the first one is taken when the reconnection rate shown in Figure 4 first settles into a steady state, and the others follow after 450, 810, and 1080 ﹩{\omega }_{p}^{-1}﹩, respectively. The horizontal axis is measured with respect to the center of the portion of domain that is displayed. The derivatives in Equations (3), (5), and (7) are computed as numerical derivatives on cells downsampled by a factor of 2.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Spatial distribution of the particle number density nt (top row; in units of n0) of the magnetic energy density (middle row; in units of ﹩{B}_{0}^{2}/8\pi ﹩) and of the z-component of the nonideal electric field as defined in Equation (2) (bottom row; in units of B0), for simulations with Bg/B0 = 0 (left) and Bg/B0 = 1 (right). The snapshots are taken at a representative time to show the nonideal electric field and plasmoid structure after the simulations have achieved a quasi-steady state. We define x = 0 as the edge of the simulation domain (so, the plot only shows a portion of the domain), while y = 0 in the midplane.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Reconnection rate (i.e., the plasma inflow velocity normalized by c) over time for each guide field case, as indicated in the legend. The reconnection rate is measured as the mean inflow velocity in the region y = [−672, 672]c/ωp. In the same color, we show with the shaded area the acceptable ranges of α/2 of our resistivity prescription, which we define in Section 3.2.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: A comparison between the measured nonideal electric field ﹩{E}_{z}^{* }﹩ (left column) and its reconstruction ηeffJz based on our prescription in Equation (10), for the whole range of guide fields we explored. The middle column shows ηeff(α, pbest)Jz (here, α is the value corresponding to pbest based on the linear fit in Table 2), while the right column shows ηeff(α, phigh)Jz (α is the value corresponding to phigh). All panels are normalized to B0. Within each panel, horizontal black lines separate different time snapshots: the first one is taken when the reconnection rate shown in Figure 4 first settles into a steady state, and the others follow after 450, 810, and 1080 ﹩{\omega }_{p}^{-1}﹩ respectively. The horizontal axis is measured with respect to the center of the portion of domain that is displayed (which is a small fraction of the composite domain used to determine the best-fit values of α and p).
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Loss manifold computed with Equation (11) for Bg/B0 = 1, as a function of α and p. The red point marks the (α, p) combination of minimum loss. Many combinations in the dark blue valley produce losses very close to the global minimum. A correlation between the two parameters can also be seen.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: A comparison of the measured ﹩{E}_{z}^{* }﹩ and various reconstructions ηeffJz using different forms of the resistivity. Top row, from left to right: ground truth, Equation (3), and Equation (5). Bottom row, from left to right: Equation (7) and Equation (10) for both pbest and phigh (and their respective best-fit α values, calculated from the functions in Table 2). The simulation has zero guide field and a spatial resolution of c/ωp = 20 cells. All panels are normalized to B0. Within each panel, horizontal black lines separate different time snapshots: at the start of the quasi-steady phase and after 112.5, 202.5, and 270 ﹩{\omega }_{p}^{-1}﹩.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Same as Figure 7, but for the x-component of the nonideal field, which appears for nonzero guide field cases. The resistivity is based on Equation (10) and employs the same values of α and p as in Figure 7. Although our model was not developed using the x-component of E*, it is able to recover the basic structure of regions with significant ﹩{E}_{x}^{* }﹩. The magnitude of ﹩{E}_{x}^{* }﹩ is in units of B0, and the times shown are the same as in Figure 7.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: A comparison of the measured ﹩{E}_{z}^{* }﹩ and the reconstruction ηeffJz using Equation (10). We vary p beyond the range given in Table 1, and for each p, we use the optimal α value calculated from the functions presented in Table 2. The simulation has zero guide field, no cooling, and a spatial resolution of c/ωp = 5 cells (i.e., it is the reference run used in the main paper). All panels are normalized to B0. The time snapshots are the same as in Figures 3 and 7.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Same as Figure 9 but for standard resolution (c/ωp = 5 cells) and with the addition of synchrotron cooling losses, as quantified by γrad = 100 (weak cooling regime, since γrad > σ). Within each panel, horizontal black lines separate different time snapshots: at the start of the quasi-steady phase and after 450, 810, and 1080 ﹩{\omega }_{p}^{-1}﹩.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Best fit (pbest) and upper bound (phigh) as a function of guide field strength.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Same as Figure 9 but for standard resolution (c/ωp = 5 cells) and with the addition of synchrotron cooling losses, as quantified by γrad = 25 (strong cooling regime, since γrad < σ). We show the same time snapshots as in Figure 10.
Paper: Effective Resistivity in Relativistic Reconnection: A Prescription Based on Fully Kinetic Simulations
Authors: Abigail Moran, Lorenzo Sironi, Aviad Levis, Bart Ripperda, Elias R. Most, Sebastiaan Selvi
Figure caption: Same as Figure 7 but including all terms in the Ohm's law for resistive relativistic single-fluid MHD (Equation (1)) instead of the simplified form in Equation (2), which we used in the main paper. We still employ our prescription (Equation (10)) with the same α and p as discussed in the main text.
Paper: Three-dimensional Global Hybrid Simulation of Magnetosheath Jets at Mercury
Authors: Jin Guo, San Lu, Quanming Lu, Junyi Ren, Jiuqi Ma, James A. Slavin, Weijie Sun, Jun Zhong, Xinliang Gao, Rajkumar Hajra, Rongsheng Wang
Figure caption: Characteristics of magnetosheath jets, cavities, upstream CSs, and SHFAs at t = 117.00 s. (a) Dynamic pressure (﹩{P}_{d}﹩), (b) dynamic pressure in x-direction (﹩{P}_{d,\,x}﹩), (c) ion density (﹩{N}_{i}﹩), (d) total ion velocity (﹩{V}_{t}﹩), (e) ion velocity x-component (﹩{V}_{x}﹩), (f) ion parallel temperature (﹩{T}_{\parallel }﹩), (g) ion perpendicular temperature (﹩{T}_{\perp }﹩), (h) total magnetic field (﹩{B}_{t}﹩), (i) ion beta (﹩{\beta }_{i}﹩), and ion temperature (﹩T﹩) at t = 104.42 (j), 112.81 (k), and 117.00 s (l). The green and red arrows indicate the magnetosheath cavities and SHFAs, respectively. The orange circles indicate the CSs in panels (a) and (h). The points “P1” and “P2” marked in panel (a) are the positions of two virtual satellites.
Paper: Three-dimensional Global Hybrid Simulation of Magnetosheath Jets at Mercury
Authors: Jin Guo, San Lu, Quanming Lu, Junyi Ren, Jiuqi Ma, James A. Slavin, Weijie Sun, Jun Zhong, Xinliang Gao, Rajkumar Hajra, Rongsheng Wang
Figure caption: Plasma and magnetic field parameters observed by two virtual satellites in the magnetosheath. (a), (g) Ion density (﹩{N}_{i}﹩), (b), (h) ion velocity MSO components (﹩{V}_{i,x}﹩, ﹩{V}_{i,y}﹩, and ﹩{V}_{i,z}﹩), (c), (i) magnetic field MSO components (﹩{B}_{x}﹩, ﹩{B}_{y}﹩, and ﹩{B}_{z}﹩), (d), (j) total magnetic field (﹩{B}_{t}﹩), (e), (k) dynamic pressure (﹩{P}_{d}﹩) and dynamic pressure x-component (﹩{P}_{d,x}﹩), and (f), (l) ion temperature at points ﹩P1=\left(1.75,\,-0.11,\,0.67\right){R}_{{\rm{M}}}﹩ (left panels) and ﹩P2=\left(1.71,\,-0.11,\,0.46\right){R}_{{\rm{M}}}﹩ (right panels). These two points are indicated in Figure 3(a). The blue-shaded (blue- and magenta-shaded) regions indicate the magnetosheath jet intervals, which are identified as the period when Pd, x > 0.25 Pd, sw (Pd > 0.25 Pd, sw). The dotted and dashed lines in panels (e) and (k) indicate 0.5 Pd, sw and 0.25 Pd, sw, respectively.
Paper: Three-dimensional Global Hybrid Simulation of Magnetosheath Jets at Mercury
Authors: Jin Guo, San Lu, Quanming Lu, Junyi Ren, Jiuqi Ma, James A. Slavin, Weijie Sun, Jun Zhong, Xinliang Gao, Rajkumar Hajra, Rongsheng Wang
Figure caption: Magnetopause dent formed by the magnetosheath jets at t = 112.81 s. (a) ﹩{P}_{d}﹩ in the plane ﹩z\,=\,0.4\,{R}_{{\rm{M}}}﹩ and distance from the center of Mercury to the magnetopause (﹩{R}_{{\rm{pause}}}﹩) at the magnetopause surface. The blue dashed circles indicate the magnetopause dent. (b) ﹩{R}_{{\rm{pause}}}﹩ at different azimuthal angles (﹩\phi ﹩). ﹩\phi =0﹩ is along the x-direction. The magenta-shaded and green-shaded regions indicate the ϕ intervals of the magnetosheath jets and cavity, respectively.
Paper: Three-dimensional Global Hybrid Simulation of Magnetosheath Jets at Mercury
Authors: Jin Guo, San Lu, Quanming Lu, Junyi Ren, Jiuqi Ma, James A. Slavin, Weijie Sun, Jun Zhong, Xinliang Gao, Rajkumar Hajra, Rongsheng Wang
Figure caption: Magnetosheath jets downstream of the bow shock near the meridian plane at t = 100.23, 104.42, 112.81, and 117.00 s under a radial IMF. The white lines and black dashed lines indicate the magnetopause and the bow shock, respectively.