adsabs/AstroCLIMB huggingface dataset:
Paper: Electron–Ion Heating Partition in Imbalanced Solar-wind Turbulence
Authors: Jonathan Squire, Romain Meyrand, Matthew W. Kunz
Figure caption: (a)–(c) 2D spectra of δ B ⊥, ﹩{{ \mathcal E }}_{{B}_{\perp }}({k}_{\perp },{k}_{\parallel })﹩, at t ≈ τ A (left), t ≈ 11τ A (around the time of the heating transition; middle), and t ≈ 18τ A (right). The dotted white lines show the critical-balance condition ﹩{k}_{\parallel }{v}_{{\rm{A}}}=2{k}_{\perp }{z}_{\mathrm{rms}}^{+}{({k}_{\perp }/{k}_{\perp 0})}^{-1/3}﹩. (d) E ICW for different ICW obliquities, which is the energy contained in the shaded regions of panel (b) (see text). (e)–(f) Frequency spectra at different times, using the same colors as Figure 3(a). A sharp drop in high-frequency δ n fluctuations, taken as a signature of oblique-ICW activity, matches the drop in ﹩{D}_{\perp \perp }^{E}﹩. In contrast, δ B ⊥ fluctuations, present in both parallel and oblique ICWs, drop less abruptly and at later times.
Paper: Electron–Ion Heating Partition in Imbalanced Solar-wind Turbulence
Authors: Jonathan Squire, Romain Meyrand, Matthew W. Kunz
Figure caption: (Top) Perpendicular spectra of the electric field (﹩{{ \mathcal E }}_{{E}_{\perp }};﹩ solid lines) and magnetic field (﹩{{ \mathcal E }}_{{B}_{\perp }};﹩ dashed lines) at a selection of times. The subpanel illustrates the local spectral slopes α, computed via a fit over range ﹩\pm {\mathrm{log}}_{10}({k}_{\perp })\approx 0.1﹩ around each point; the dotted lines indicate k ⊥ ρ  i  = 1 and the representative power laws ﹩{k}_{\perp }^{-5/3}﹩ and ﹩{k}_{\perp }^{-0.8}﹩. (Bottom) Evolution of the break scale ﹩{k}_{\perp }^{* }﹩ with imbalance 1 − σ  c , with the line color indicating the time as in the top panel. The dotted line shows the empirical scaling ﹩{k}_{\perp }^{* }{\rho }_{i}=2{(1-{\sigma }_{c})}^{1/4}﹩, which provides a good fit to the simulation until t ≈ 11τ A.
Paper: Electron–Ion Heating Partition in Imbalanced Solar-wind Turbulence
Authors: Jonathan Squire, Romain Meyrand, Matthew W. Kunz
Figure caption: (Top) Time evolution of ε  H /ε (purple), energy imbalance σ  c  (orange), and total fluctuation energy per unit volume E ⊥(t) (blue). (Bottom) Electron heating rate Q  e  = ε  η  (green) and ion heating rate Q  i  (red), with simple helicity-barrier expectations based on the forcing shown with dotted lines.
Paper: Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
Authors: K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, 一泽 董, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, Samuel Wyatt
Figure caption:                         (a) The evolution of the optical spectra of SN 2023ixf over the first ∼5.2 days, with the earliest epoch at the top of the figure. Spectra are color coded by the instrument used to observe them, normalized by a blackbody fit, and corrected for redshift. Emission lines are identified at their rest wavelengths with vertical lines and labeled at the top of the figure, while the most prominent telluric features are marked with the shaded gray region. Throughout this sequence, the spectra evolve from showing strong, narrow emission lines from high-ionization species to intermediate width features as the CSM is accelerated by the shock. The spectra evolve rapidly between 1.18 and 1.67 days, with the He I and N III (λλ4634.0,4640.6)/C III (λλ4647.5,4650.0) lines disappearing within the first 0.5 day from the first spectrum while He II (λ4685.5), N IV, and C IV gain strength. (b) Continuation of Figure 1 showing the evolution of the optical spectra of SN 2023ixf from days 5.2 to 14.5 with the earliest epoch at the top of the figure. Over the first 7 days, the spectra evolve from showing strong, narrow emission lines from high-ionization species to a nearly featureless spectrum with an intermediate with P Cygni profile in Hα. In the subsequent 7 days, broad P Cygni profiles develop in the higher-order Balmer features.
Paper: Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
Authors: K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, 一泽 董, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, Samuel Wyatt
Figure caption: A comparison of SN 2023ixf (black) to SN 1998S (teal; Leonard et al. 2000), SN 2013fs (blue; Yaron et al. 2017), SN 2013cu (green; Gal-Yam et al. 2014), SN 2014G (purple; Terreran et al. 2016), SN 2017ahn (mustard; Tartaglia et al. 2021), and SN 2020pni (pink; Terreran et al. 2022) ∼1, 3, 7, and 14 days after explosion. These SNe all have flash features that evolve over the first two weeks. The SN name and epoch are marked to the right of the plot. All spectra have been redshift and extinction corrected and then normalized by a blackbody fit to the continuum. Emission lines identified in the first spectrum are marked with vertical lines, which are labeled at the top of the figure. In the first epoch, SN 2023ixf closely resembles SNe 2020pni and 2017ahn, although at later epochs it more closely follows SN 2014G. SN 2013fs is considerably different in its evolution throughout the first two weeks. At later epochs, SN 2020pni and SN 1998S develop narrow P Cygni profiles that are not present in the spectra of other SNe.
Paper: Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
Authors: K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, 一泽 董, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, Samuel Wyatt
Figure caption: The SN luminosity and mass-loss rate derived by Boian & Groh (2020) for a sample of 17 SNe compared to the best model of SN 2023ixf (black). Upper limits on mass loss are shown with semitransparent markers and arrows, while determined values are solid. We determine a scaled mass-loss rate of ﹩\dot{M}\approx 4.5\times {10}^{-3}﹩                   M ⊙ yr−1 and a scaled luminosity of L ≈ 2.6 × 109 L ⊙ from the models of Boian & Groh (2019; with slight variation due to different surface abundances), which we plot as black stars. In practice, these are located at virtually the same location on this plot. We also include the mass-loss rates of the r1w4 and r1w6 models of Dessart et al. (2017) (﹩\dot{M}={10}^{-3}﹩                   M ⊙ yr−1, and ﹩\dot{M}={10}^{-2}﹩                   M ⊙ yr−1, respectively), which are shown as black triangles. Dessart et al. (2017) does not explore variations in luminosity, and we therefore use the luminosity derived from Boian & Groh (2019) solar abundance models and do not scale the mass-loss rates. The mass-loss rate of SN 2023ixf is in line with the lower end of the range of mass-loss rates in this sample.
Paper: Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
Authors: K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, 一泽 董, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, Samuel Wyatt
Figure caption: The day 1.36 spectrum (black) compared with three different surface abundance models from Boian & Groh (2019) with L = 1.5 × 109 L ⊙, and ﹩\dot{M}=3\times {10}^{-3}﹩                      M ⊙ yr−1. The solar abundance represents a low-mass RSG (yellow), CNO-processed abundance represents a high-mass star (RSG, BSG, or YSG; blue), and He-rich abundance represents an LBV, WN, or other stripped star (pink). Vertical dashed lines represent the ions that are identified in the observed spectra that are labeled at the top of the plot. Vertical dotted lines in light gray show ions that are not detected but are part of the progenitor diagnostics detailed in Boian & Groh (2019). We convolve the model spectra with a Gaussian kernel to mimic the resolution of the observed spectra. While some individual features in each model are matched by the observed spectrum, there are differences between the model and observed spectrum that indicate that the conditions of the model are not the same as the observations.
Paper: Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
Authors: K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, 一泽 董, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, Samuel Wyatt
Figure caption: A comparison of the spectral evolution of SN 2023ixf (black) to the r1w4 model of Dessart et al. (2017; pink). Phases are shown to the right of the figure in pink for the model and black from the observed spectra. While the first observation at 1.2 days matches fairly well, the model spectra evolve much more rapidly, with P Cygni profiles developing at day 2 and all emission disappearing by day 4, while the observations show emission through days 6–7. The model spectrum at 0.5 day shows a number of lines that have faded by 1 day (e.g., N V).
Paper: Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf
Authors: K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, 一泽 董, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, Samuel Wyatt
Figure caption: The evolution of SN 2023ixf from day 1.18 through day 3, colored by phase. Ions are labeled in each panel, and the phase is given in the middle panel. Emission lines from the low-ionization levels, He I, N III, C III, O III, and N IV (λ 5074 Å), disappear over the first 0.5 day of evolution while emission from high-ionization levels, N IV (λ λ7103, 7109, λ7122), He II (λ4685.5), and C IV (λ λ 5801.3, 5811.98 Å), increase in strength. Spectra are fit with a blackbody function and normalized, corrected for redshift, and offset for readability. In the bottom panel, the B-band telluric feature is marked with a gray shaded region.
Paper: Minor Merger Growth in Action: JWST Detects Faint Blue Companions around Massive Quiescent Galaxies at 0.5 ≤ z ≤ 3.0
Authors: Katherine A. Suess, Christina C. Williams, Brant Robertson, Zhiyuan Ji, Benjamin D. Johnson, Erica Nelson, Stacey Alberts, Kevin Hainline, Francesco D'Eugenio, Hannah Übler, Marcia Rieke, George Rieke, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Daniel J. Eisenstein, Roberto Maiolino, Daniel P. Stark, Sandro Tacchella, Chris Willott
Figure caption: Top: stellar mass vs. redshift for all companions (“buddies”) and primary hosts; typical error bars shown in legend. The Tal et al. (2014) CANDELS-wide mass completeness limit is shown in red; most of our detected companions are below this limit. Bottom: number of companions per host as a function of redshift, in bins of companion mass. Points are excluded if the companion mass is less than 1.5 dex below the HST mass completeness. Massive companions are rare across redshift, existing around only ∼10% of hosts (consistent with Newman et al. 2012). Low-mass companions are increasingly more common, with most massive quiescent galaxies hosting at least 1–2 companions with ﹩8\lt \mathrm{log}{M}_{* }/{M}_{\odot }\lt 9﹩.
Paper: Minor Merger Growth in Action: JWST Detects Faint Blue Companions around Massive Quiescent Galaxies at 0.5 ≤ z ≤ 3.0
Authors: Katherine A. Suess, Christina C. Williams, Brant Robertson, Zhiyuan Ji, Benjamin D. Johnson, Erica Nelson, Stacey Alberts, Kevin Hainline, Francesco D'Eugenio, Hannah Übler, Marcia Rieke, George Rieke, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Daniel J. Eisenstein, Roberto Maiolino, Daniel P. Stark, Sandro Tacchella, Chris Willott
Figure caption: Spatially resolved M/L and UVJ diagrams. Left: M/L profiles for each individual primary quiescent galaxy (gray curves), a median stack of all quiescent galaxies (black diamonds), and a median stack of all identified companions (purple points split by mass ratio), binned by their separation from their host. Right: shaded hexagons show the spatially resolved rest-frame UVJ colors of all quiescent primaries; purple contours indicate the UVJ colors of all companions (split by mass ratio). While individual quiescent primaries show a range of behaviors, on average most quiescent galaxies in our sample show radially decreasing M/L profiles and have outskirts which lie outside the quiescent UVJ box. Massive companions have relatively high M/L and quiescent UVJ colors, while low-mass companions have lower M/L values and lie in the low-mass star-forming region of UVJ space.
Paper: Minor Merger Growth in Action: JWST Detects Faint Blue Companions around Massive Quiescent Galaxies at 0.5 ≤ z ≤ 3.0
Authors: Katherine A. Suess, Christina C. Williams, Brant Robertson, Zhiyuan Ji, Benjamin D. Johnson, Erica Nelson, Stacey Alberts, Kevin Hainline, Francesco D'Eugenio, Hannah Übler, Marcia Rieke, George Rieke, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Daniel J. Eisenstein, Roberto Maiolino, Daniel P. Stark, Sandro Tacchella, Chris Willott
Figure caption: Left: difference in F150W magnitude between primary quiescent galaxy and all companions as a function of separation, colored by primary redshift. It is more difficult to detect faint companions that are close to their hosts, especially at high redshift. Right: inferred mass ratio between primary quiescent galaxy and companions as a function of separation. The gray shaded region indicates mass ratios >1:10, where previous studies such as Newman et al. (2012) using HST CANDELS-wide imaging were complete. Just 6% of companions in this study were in the regime probed by HST.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: Time evolution of the Lorentz factor of two representative positrons from the 3D σ = 10 simulation in Figure 2. Solid lines indicate when the positron is free, dotted when trapped; see the text. The spatial track of positron A is in Figure 2.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: Isosurfaces of reconnected plasma density from the 3D σ = 10 simulation at ct/L ≃ 10. The trajectory of a representative high-energy positron is overlaid, starting at the filled red circle and ending at the tip of the red arrow, after looping once through the periodic z boundary. It is colored in solid red if the positron is in the upstream (inflow) region above the midplane (on the same side as the observer), otherwise it is dotted black. The red open circle indicates the particle position at the time ct/L ≃ 10 of the density isosurfaces. We only show a subset of the domain along y, zooming into the vicinity of the layer (at time t, the y-extent of the domain is 2ct). The domain is replicated three times in z for easier visualization of the positron track.
Paper: Minor Merger Growth in Action: JWST Detects Faint Blue Companions around Massive Quiescent Galaxies at 0.5 ≤ z ≤ 3.0
Authors: Katherine A. Suess, Christina C. Williams, Brant Robertson, Zhiyuan Ji, Benjamin D. Johnson, Erica Nelson, Stacey Alberts, Kevin Hainline, Francesco D'Eugenio, Hannah Übler, Marcia Rieke, George Rieke, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Daniel J. Eisenstein, Roberto Maiolino, Daniel P. Stark, Sandro Tacchella, Chris Willott
Figure caption: HST F160W, JWST F150W, JWST F444W, a primary-subtracted short-wavelength (SW) stacked JWST image, and a color JWST image. Rows are ordered by redshift. In the SW stack, potential companions with photometric redshifts consistent within 1σ are indicated with 0.″2 green circles; 2σ with dashed 0.″2 yellow circles; and inconsistent with dashed 0.″2 red circles. The black circle indicates our companion search radius (35 kpc).
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: Time evolution of the reconnection rate v in/c, where v in is the inflow speed averaged over 0.2L < y < 0.6L. Solid lines refer to 3D, dashed to 2D. The reconnection rate attains a quasi-steady value at t ≳ 3 L/c.
Paper: Minor Merger Growth in Action: JWST Detects Faint Blue Companions around Massive Quiescent Galaxies at 0.5 ≤ z ≤ 3.0
Authors: Katherine A. Suess, Christina C. Williams, Brant Robertson, Zhiyuan Ji, Benjamin D. Johnson, Erica Nelson, Stacey Alberts, Kevin Hainline, Francesco D'Eugenio, Hannah Übler, Marcia Rieke, George Rieke, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Daniel J. Eisenstein, Roberto Maiolino, Daniel P. Stark, Sandro Tacchella, Chris Willott
Figure caption: Difference in observed (left) and inferred rest-frame (right) color between each primary quiescent galaxy and its possible companions. Most companions are bluer than their primary galaxy in both observed and inferred rest-frame color: 83% (13%) of companions have observed colors bluer (redder) than their primary, and 85% (5%) of companions have rest-frame colors bluer (redder) than their primary.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: Top: particle energy spectra in 3D (solid) and 2D (dashed) for different magnetizations (legend in the bottom panel). Middle: spectra of free (dashed) and trapped (solid) particles. Free spectra are only shown for γ ≳ 3σ (beyond injection). Black dotted lines show the predicted spectra of trapped particles based on Equation (3). Bottom: particle spectra measured at the injection time. We only consider particles whose maximum Lorentz factor is >3σ, and we define injection as the time when a particle starts the free phase (each particle is counted more than once if it experiences more than one free phases). Spectra in the bottom panel are normalized such that their integral is unity. Spectra in all panels are time-averaged between 3 L/c and 7.5 L/c.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: 2D histograms of Δt exit. In the left column, we consider particles that exit the box as free, and define Δt exit as the difference between the exit time t exit and the time when their last (i.e., current) free phase started. In the right column, we consider particles that exit the box as trapped, and define Δt exit as the difference between the exit time t exit and the time when their last free phase ended (i.e., the last time the particle got captured). Particles that never experienced a free phase are not included. Dashed red lines on the left are the same as in the right panel of Figure 5 in the main text. Dashed red lines on the right indicate L/c. The Lorentz factor γ on the horizontal axis is measured at t exit. The histograms are normalized to their respective maxima, and colors span the range [10−3, 1] in logarithmic increments.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: 2D histograms of acceleration time t acc (left) and escape time t esc (right) of free particles. Dashed red lines are predictions based on the measured reconnection rate (left) and on the power-law slope of free particles (right), as described in the text. The Lorentz factor γ on the horizontal axis is the instantaneous value on the left, while it is the value at the end of the free phase on the right. The histograms are normalized to their respective maxima, and colors span the range [10−3, 1] in logarithmic increments.