adsabs/AstroCLIMB huggingface dataset:
Paper: A New Covariant Formalism for Kinetic Plasma Simulations in Curved Spacetimes
Authors: Tyler Trent, Pierre Christian, Chi-kwan Chan, Dimitrios Psaltis, Feryal Özel
Figure caption: The trajectory of a charged particle moving in a magnetic dipole in a Schwarzschild spacetime, calculated by solving the full equations of motion (red line) as well as the equations of the guiding center derived here (blue line). The particle experiences mirroring between the two magnetic poles and an azimuthal drift. Even for the exaggerated conditions shown here, where the gyration is clearly visible in the trajectory of the particle, the guiding center equations describe accurately the drift of the particle motion.
Paper: A New Covariant Formalism for Kinetic Plasma Simulations in Curved Spacetimes
Authors: Tyler Trent, Pierre Christian, Chi-kwan Chan, Dimitrios Psaltis, Feryal Özel
Figure caption: Fractional difference between the average azimuthal drift velocity calculated in the guiding center limit and using the full equation of motion of a charge in a magnetic dipole in flat and Schwarzschild spacetimes (see Figure 2 for the setup). Other details as in Figure 3. In this configuration, the truncation error depends quadratically on gyroradius.
Paper: SN 2023emq: A Flash-ionized Ibn Supernova with Possible C III Emission
Authors: M. Pursiainen, G. Leloudas, S. Schulze, P. Charalampopoulos, C. R. Angus, J. P. Anderson, F. Bauer, T.-W. Chen, L. Galbany, M. Gromadzki, C. P. Gutiérrez, C. Inserra, J. Lyman, T. E. Müller-Bravo, M. Nicholl, S. J. Smartt, L. Tartaglia, P. Wiseman, D. R. Young
Figure caption: Photometric qualities of SN 2023emq. Top: the multiband light curve of SN 2023emq. Open markers refer to nondetections (5σ). The spectral epochs are highlighted with dashed lines. The interpolated o-band GP light curve is shown over the data, and the decline rate of 56Co is drawn for comparison. The late-time decline rate is significantly faster than the 56Co rate, and the decline continued fast until the SN was no longer detected at +78 and +95 days. Bottom left: the ATLAS o-band light curve of SN 2023emq in comparison to r-band light curves of example fast events. The light curves are collected from ZTF via the Alerce broker (Förster et al. 2021) except for AT 2018cow, where data presented in Prentice et al. (2018) and Perley et al. (2019) were used. Bottom middle: absolute magnitude vs. decline rate of fast-evolving transients. Values of Type Icn SNe (Pellegrino et al. 2022a), cow-like transients (Prentice et al. 2018; Perley et al. 2019, 2021; Ho et al. 2020; Yao et al. 2022), and SN 2023emq were obtained by fitting the first 20 days of postpeak r-band light curves linearly. The values for RETs are taken from Pursiainen et al. (2018), and the used bands (g, r, i, or z) were chosen to be the closest to the rest-frame r band. Type Ibn SNe are collected from Hosseinzadeh et al. (2017), where data are presented mostly in the R band. On the top histogram we show the number (N) of transients per decline rate with SN 2023emq highlighted with a dashed red line. No Type Icn SNe and only 2/22 Type Ibn SNe are faster than SN 2023emq. Bottom right: the best-fitting combined CSM and nickel decay model (Chatzopoulos et al. 2012, 2013) to the bolometric light curve of SN 2023emq. The derived CSM and ejecta masses are similar, but smaller in comparison to other Type Ibn/Icn SNe as expected given the fast light-curve evolution near peak. The nickel mass is comparable to fast-evolving Type Ibn/Icn SNe.
Paper: SN 2023emq: A Flash-ionized Ibn Supernova with Possible C III Emission
Authors: M. Pursiainen, G. Leloudas, S. Schulze, P. Charalampopoulos, C. R. Angus, J. P. Anderson, F. Bauer, T.-W. Chen, L. Galbany, M. Gromadzki, C. P. Gutiérrez, C. Inserra, J. Lyman, T. E. Müller-Bravo, M. Nicholl, S. J. Smartt, L. Tartaglia, P. Wiseman, D. R. Young
Figure caption: The spectroscopic time series of SN 2023emq (in colors) in comparison to the Type Icn SNe 2019hgp (Gal-Yam et al. 2022) and 2021csp (Perley et al. 2022) and the Type Ibn SNe 2015U (Shivvers et al. 2016) and 2014av (Pastorello et al. 2016) in gray. Spectral epochs are presented with respect to peak brightness. The first spectrum resembles that of SN 2015U, and the latest spectrum is virtually identical to SN 2014av. As already noted by Perley et al. (2022), the continuum emission of SN 2021csp at late times is very similar to the continuum seen in Type Ibn SNe including SN 2023emq. The most prominent He I features are marked with dashed lines, other strong features with solid lines, and tellurics are shown in gray bands. Note that the spectrum of the highly reddened SN 2015U is artificially dereddened for visual comparison.
Paper: SN 2023emq: A Flash-ionized Ibn Supernova with Possible C III Emission
Authors: M. Pursiainen, G. Leloudas, S. Schulze, P. Charalampopoulos, C. R. Angus, J. P. Anderson, F. Bauer, T.-W. Chen, L. Galbany, M. Gromadzki, C. P. Gutiérrez, C. Inserra, J. Lyman, T. E. Müller-Bravo, M. Nicholl, S. J. Smartt, L. Tartaglia, P. Wiseman, D. R. Young
Figure caption: The host environment of SN 2023emq in the VLT/FORS2 R-band observation taken at +95 days (2023 July 12) when the SN was already undetectable (see Table 1). The location of the SN (red circle) is on top of a bright region of the host galaxy.
Paper: The Large Magellanic Cloud’s ∼30 kpc Bow Shock and Its Impact on the Circumgalactic Medium
Authors: David J. Setton, Gurtina Besla, Ekta Patel, Cameron Hummels, Yong Zheng, Evan Schneider, Munier Salem
Figure caption: The simulated LMC shock system presented in this work (as in Figure 1 for T > 106 K) shown with observed Hα contours measured with WHAM (Smart et al. 2023). We show integrated Hα contours encompassing 0.1, 0.5, 5, and 50 R intensity integrated between −130 and 110 km s−1 in the LMC frame of reference. We suggest that the diffuse Hα structure leading the LMC disk may be associated with the shock, providing a clear explanation for the Hα structure that is more extended and follows a different morphology than the neutral H I gas.
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: An example of reconstruction of one of many test synthetic models. Respective values of magnesium, aluminum, argon, silicon, sulfur, calcium, iron, and nickel abundances; temperatures; and emission measures in the whole 150 element population (in gray) in each iteration step are presented. Blue dots represent the values from the best solution corresponding to the given iteration step. The red color represents the assumed input values of parameters. The illustration is for the case of a two-temperature plasma model (T 1, T 2; EM1, EM2).
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: Variation of temperature, emission measure, and elemental abundance values (Mg, Al, Si, and S) for the flare on 2020 April 6 (SOL2020-04-06T05:48). Results obtained using the DE method (red) and the values adopted from Mondal et al. (2021) (blue) are plotted. The dashed and solid horizontal lines show the values of coronal (Feldman 1992) and photospheric (Asplund et al. 2009) abundances, respectively.
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: Schematic representation of individual element of the population consisting of “genes” (boxes) that have been used in the DE analysis.
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: Time evolution of electron density (lower limit), and thermal energy content for the p = constant case of the flare of 2021 May 7.
Paper: A New Covariant Formalism for Kinetic Plasma Simulations in Curved Spacetimes
Authors: Tyler Trent, Pierre Christian, Chi-kwan Chan, Dimitrios Psaltis, Feryal Özel
Figure caption: The physical conditions encountered in plasmas in a variety of astrophysical settings; ρ denotes the radius of gyromotions, λ mfp the collisional mean-free path of particles, and R the macroscopic scale of each system. A fluid approach is applicable for modeling systems in the gray shaded region. The conditions in the blue shaded region necessitate a kinetic approach. The guiding center formalism developed here enables accurate integrations of charged particle trajectories in all the systems in the white region. Dashes outline systems for which general relativistic effects require a covariant formulation.
Paper: Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H
Authors: E. M. May, Ryan J. MacDonald, Katherine A. Bennett, Sarah E. Moran, Hannah R. Wakeford, Sarah Peacock, Jacob Lustig-Yaeger, Alicia N. Highland, Kevin B. Stevenson, David K. Sing, L. C. Mayorga, Natasha E. Batalha, James Kirk, Mercedes López-Morales, Jeff A. Valenti, Munazza K. Alam, Lili Alderson, Guangwei Fu, Junellie Gonzalez-Quiles, Joshua D. Lothringer, Zafar Rustamkulov, Kristin S. Sotzen
Figure caption: Retrieval results including ground-based observations of GJ 1132 b. Top: retrieved transmission spectra for the atmosphere (Section 4.4.1) and starspot (Section 4.4.2) scenarios for JWST NIRSpec G395H Visit 1, but now including the LDSS-3C observations from Diamond-Lowe et al. (2018). Both retrievals include a free offset between the ground-based and JWST data. Overplotted are the ground-based observations of GJ 1132 b with no offset applied (gray data points), including the median retrieved offset from the starspot scenario (341 ppm; orange data points), and including the median retrieved offset from the atmosphere scenario (155 ppm; green data points). Bottom: posterior distributions including the ground-based data (green/orange for the atmosphere/starspot scenarios) compared to the results from Figure 4 with only JWST data (purple/blue for the atmosphere/starspot scenarios). The retrieval results minimally change when adding the ground-based observations.
Paper: Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H
Authors: E. M. May, Ryan J. MacDonald, Katherine A. Bennett, Sarah E. Moran, Hannah R. Wakeford, Sarah Peacock, Jacob Lustig-Yaeger, Alicia N. Highland, Kevin B. Stevenson, David K. Sing, L. C. Mayorga, Natasha E. Batalha, James Kirk, Mercedes López-Morales, Jeff A. Valenti, Munazza K. Alam, Lili Alderson, Guangwei Fu, Junellie Gonzalez-Quiles, Joshua D. Lothringer, Zafar Rustamkulov, Kristin S. Sotzen
Figure caption: Comparison of Eureka! and FIREFLy transmission spectra from binning before and after light-curve fitting. In yellow are the Eureka! reductions and in pink are the FIREFLy reductions. For both, the shaded circles are the reductions that are first binned to R ∼ 100 and then fit (prebinned) and the darker triangles are the reductions that are fit at the native resolution and then binned to R ∼ 100 (postbinned). In the bottom panels we show the differences between the Eureka! and FIREFLy reductions for both cases in units of σ, with the solid thicker line showing the prebinned case and the thinner dashed line showing the postbinned case. The shaded regions denote ±1σ and ±2σ to guide the eyes. The Eureka! and FIREFLy prebinned spectra are clearly more consistent with each other (always within a ±1σ difference) than the postbinned case, suggesting that fitting at the native resolution is not always appropriate.
Paper: Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H
Authors: E. M. May, Ryan J. MacDonald, Katherine A. Bennett, Sarah E. Moran, Hannah R. Wakeford, Sarah Peacock, Jacob Lustig-Yaeger, Alicia N. Highland, Kevin B. Stevenson, David K. Sing, L. C. Mayorga, Natasha E. Batalha, James Kirk, Mercedes López-Morales, Jeff A. Valenti, Munazza K. Alam, Lili Alderson, Guangwei Fu, Junellie Gonzalez-Quiles, Joshua D. Lothringer, Zafar Rustamkulov, Kristin S. Sotzen
Figure caption: 2D light curves for all reductions from Visit 1 and Eureka! white light curves for both visits. In the top panel we show the 2D light curves for all three reductions, including the data (left), models (middle), and residuals (right) at the R ∼ 100 resolution. FIREFLy trims extra data from the start of the NRS1 data due to a temporal ramp. In the bottom panel we show the Eureka! white light curves and models for NRS1 and NRS2 (left), the residuals (middle), and a histogram of the residuals for both NRS1 and NRS2 (right) for both Visits 1 and 2. There is no evidence of occulted starspots in any of the white light curves.
Paper: Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H
Authors: E. M. May, Ryan J. MacDonald, Katherine A. Bennett, Sarah E. Moran, Hannah R. Wakeford, Sarah Peacock, Jacob Lustig-Yaeger, Alicia N. Highland, Kevin B. Stevenson, David K. Sing, L. C. Mayorga, Natasha E. Batalha, James Kirk, Mercedes López-Morales, Jeff A. Valenti, Munazza K. Alam, Lili Alderson, Guangwei Fu, Junellie Gonzalez-Quiles, Joshua D. Lothringer, Zafar Rustamkulov, Kristin S. Sotzen
Figure caption: Comparison between a proposed H2-dominated spectrum of GJ 1132 b and our best-fitting model. The best-fitting H2O-dominated atmosphere spectrum from the POSEIDON retrieval (pink curve), which we fit to only the JWST NIRSpec G395H data (black circles), is more consistent with the HST WFC3 reduction from Libby-Roberts et al. (2022; black triangles) than the reduction from Swain et al. (2021; gray stars). The best-fit model from Swain et al. (2021; purple solid curve), extrapolated out to 5 μm with PICASO (purple dashed curve), is inconsistent with our JWST NIRSpec data.
Paper: Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H
Authors: E. M. May, Ryan J. MacDonald, Katherine A. Bennett, Sarah E. Moran, Hannah R. Wakeford, Sarah Peacock, Jacob Lustig-Yaeger, Alicia N. Highland, Kevin B. Stevenson, David K. Sing, L. C. Mayorga, Natasha E. Batalha, James Kirk, Mercedes López-Morales, Jeff A. Valenti, Munazza K. Alam, Lili Alderson, Guangwei Fu, Junellie Gonzalez-Quiles, Joshua D. Lothringer, Zafar Rustamkulov, Kristin S. Sotzen
Figure caption: Allan variance plots for the Eureka! reduction. Left panel: variation of the NRS1 and NRS2 detector white light-curve precision (rms) with longer bin timescales (more integrations). As seen in previous works (e.g., Moran et al. 2023), correlated noise emerges around timescales of 0.5–5 minutes (5–50 integrations) and is likely due to thermal cycling (Rigby et al. 2023). Right panel: same, for the spectroscopic light curves. The individual spectroscopic light curves show no evidence of correlated noise.
Paper: Stars Bisected by Relativistic Blades
Authors: Marcus DuPont, Andrew MacFadyen
Figure caption: Snapshots at 3 s depicting the lab frame density in the northern hemisphere and pressure in the southern hemisphere where the radial boundary is at 0.2R ⊙. The density color stretch is identical to panel (a) in Figure 1. The pressure color map is chosen such that the direction of increasing pressure gets brighter. Upper: the beam propagation for θ 0 = 0.005. In the equatorial plane, the beam path is evacuated and the pressure is slightly laterally stratified. Lower: the same variables as in the upper wedge, but with injection angle θ = 0.01. The cocoon tail is fatter in this instance and the jet head lags behind the thinner beam. In both cases, there exist no clear knots or pinching as usually seen for collimation shocks in classical jets.
Paper: Stars Bisected by Relativistic Blades
Authors: Marcus DuPont, Andrew MacFadyen
Figure caption: The cumulative isotropic-equivalent kinetic energy as a function of polar angle θ at 4 s. The solid, dashed, dotted, and dashed–dotted lines mark the Γβ > {1, 10, 15, 30} cutoffs, respectively. The inset is a zoom in around some small solid angle near the stellar equatorial plane. Some of the relativistic material is forced to spread laterally, as shown by the area under the Γβ > 1 curve, but as we discriminate toward higher velocities, the bulk lamina structure (Γβ > 10) is focused in the stellar equator into a thin layer with E  k,iso ∼ 5 × 1052 erg. At the simulation end, only a small amount of material is accelerated near the maximum Lorentz factor, with E  k,iso(>30) ∼ 2 × 1051 erg.
Paper: Stars Bisected by Relativistic Blades
Authors: Marcus DuPont, Andrew MacFadyen
Figure caption: Snapshots of the lamina jet with injection angle θ 0 = 0.005. The left half shows the four-velocity and the right shows the lab frame density D = Γρ. Panel (a) shows the interior beam zoomed in to 0.1R ⊙ at the boundary. We see the development of Kelvin–Helmholtz instabilities as the beam tunnels through the dense core with the region nearest the jet head experiencing a few collimation shocks. In panel (b), the lamina breaks out of the star successfully with a Γ ≥ 30. The white-dashed line marks the radius of the progenitor at 0.5R ⊙.
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: Top left: GOES light curves (in red and dark blue) for the 2021 May 7 flare. The time intervals in which the XSM observations were investigated are marked in gray. Top middle: normalized STIX light curves in seven selected energy bands. The timescale corresponds to the dashed vertical lines from the top left panel. Top right: STIX image obtained during the rise phase of flare for 10 s time interval (∼18:52 UT) in the energy range from 5 to 6 keV. The red contours represent emissions from 22–25 keV. Bottom panels (from left to right): STIX images reconstructed in 4–10 keV energy range and for the integration times 25 s, 25 s, and 5 minutes at the rise, maximum, and decay phases of the flare, respectively. Contours indicate the levels of 30%, 50%, and 70% of maximum.
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: Top panels: temporal variations of temperature (left) and emission measure (middle) for the cooler (in blue) and hotter (in green) DEM components. Respective diagnostic diagrams (DDs) for cooler and hotter plasma components are plotted in the top right panel. Theoretical quasi-steady and switch-off states are annotated. Bottom panels: GOES temperature (left) and emission measure (middle) values obtained based on observed fluxes (in black) and “predicted” based on two-component emission measure distributions from XSM analysis (red and blue colors); see the text for details. The DDs from GOES observations (in black) and from temperature and emission measure “predicted” based on XSM spectra analysis (in orange) are plotted in the bottom right panel. Four characteristics times are marked by squares of different colors.
Paper: Investigations of Flaring Plasma Parameters during an M-class Flare Using the Differential Evolution Method and XSM/Chandrayaan-2 Observations
Authors: Anna Kępa, Marek Siarkowski, Arun Kumar Awasthi, Janusz Sylwester, Barbara Sylwester
Figure caption: The observed (blue) and fitted (red) spectra taken close to maximum of flare temperature together with residuals (below) and temporal variation of derived elemental abundances during the flare on 2021 May 7. Horizontal dotted and full lines represent coronal (Feldman 1992) and photospheric (Asplund et al. 2009) abundances of a given element, respectively.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Time evolution of μ, particle position in the z-direction (the direction of the mean magnetic field for M2) z/L inj, and 2MB 0/γ mu 2 corresponding to the test particle trajectory in Figure 3. Blue and orange lines represent the numerical measurements and their gyroaveraged results, respectively.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Trajectory of a test particle in M2 with r  L  = 0.01L inj and μ 0 = 0.05. The trajectory is color coded by magnetic field strength in (a) and time in (b). Trajectories in (a) and (b) are the same except that the trajectory in (a) is averaged over the gyroperiod Ω−1 to better illustrate the motion of the test particle. Arrows in (a) indicate the directions of mirror forces.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Gyroaveraged trajectory of a test particle in M2 with r  L  = 0.02L inj and μ 0 = 0.05. The trajectory is color coded by time, with a transition from mirror diffusion to scattering diffusion.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Time evolution of μ, position in the z-direction z/L inj, and 2MB 0/γ mu 2 for a test particle with r  L  = 0.04L inj and μ 0 ≈ 0.05 in M4. Blue and orange lines represent the numerical measurements and their gyroaveraged results, respectively.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Distribution of parallel displacement Δz measured for test particles with r  L  = 0.01L inj and different values of μ in M1. The bin size of Δz is about 0.05L inj. The vertical dotted lines indicate the mean values.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Averaged perpendicular separation of test particles ﹩\left\langle \sqrt{\langle \delta {\tilde{x}}^{2}\rangle }\right\rangle ﹩ vs. time for M1 (a), M2 (b), and M3 (c), with r  L  = 0.01L inj and initial pitch-angle cosine μ 0 = 0.10. l diss is indicated by the horizontal dashed line.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Parallel mean free path λ ∥/L inj for mirror diffusion measured at different μ for M1, M2, and M3. The vertical dashed lines indicate the estimated ﹩{\mu }_{\max }﹩, which is ≈0.52 (Equation (8)) for M1 and M2 and ≈0.67 (Equation (10)) for M3.
Paper: Numerical Testing of Mirror Diffusion of Cosmic Rays
Authors: Chao Zhang, Siyao Xu
Figure caption: Distributions of μ measured at different times for 5000 test particles with r  L  = 0.01L inj and μ 0 = 0.05 (indicated by the vertical dotted line) in M2. The bin size of μ is 0.05.