adsabs/AstroCLIMB huggingface dataset:
Paper: Interplanetary Rotation of 2021 December 4 Coronal Mass Ejection on Its Journey to Mars
Authors: Mengxuan Ma, Liping Yang, Fang Shen, Chenglong Shen, Yutian Chi, Yuming Wang, Yufen Zhou, Man Zhang, Daniel Heyner, Uli Auster, Ingo Richter, Beatriz Sanchez-Cano
Figure caption: Panels (a) and (b) show the 3D magnetic flux-rope structure of the simulated CME in the interplanetary space at t = 31 (a) and t = 71 hr (b), respectively, where the slice is on the plane of z = −20 Rs with the radial range between 20 and 500 Rs. The colored rods represent magnetic field lines, and the colors denote the radial velocity (V  r ). The black lines denote orientation of the symmetric axis of the spheromak CME. Panels (c) and (d) show the magnetic flux ropes at t = 31 and t = 71 hr together at the lateral (c) and top (d) views, respectively. α, β, λ, and γ mark the top, bottom, left, and right parts of the flux rope, respectively. The red sphere represents the sphere with a radius of 20 Rs, and the black dashed lines are radial lines.
Paper: Interplanetary Rotation of 2021 December 4 Coronal Mass Ejection on Its Journey to Mars
Authors: Mengxuan Ma, Liping Yang, Fang Shen, Chenglong Shen, Yutian Chi, Yuming Wang, Yufen Zhou, Man Zhang, Daniel Heyner, Uli Auster, Ingo Richter, Beatriz Sanchez-Cano
Figure caption: Panels (a) and (b) show the 3D magnetic flux-rope structure of the simulated CME in the solar corona at t = 1 (a) and t = 3 hr (b), respectively, where the slice is on the plane of x = 0 Rs with the radial range between 1 and 20 Rs. The colored lines denote magnetic field lines, and the colors represent the radial velocity (V  r ). The black lines denote orientation of the symmetric axis of the spheromak CME. Panels (c) and (d) show the magnetic flux ropes at t = 1 and t = 3 hr together at the lateral (c) and top (d) views, respectively. α, β, λ, and γ mark the top, bottom, left, and right parts of the flux rope, respectively. The red sphere represents the Sun, and the black dashed lines are radial lines.
Paper: Interplanetary Rotation of 2021 December 4 Coronal Mass Ejection on Its Journey to Mars
Authors: Mengxuan Ma, Liping Yang, Fang Shen, Chenglong Shen, Yutian Chi, Yuming Wang, Yufen Zhou, Man Zhang, Daniel Heyner, Uli Auster, Ingo Richter, Beatriz Sanchez-Cano
Figure caption: Panel (a) shows the 3D magnetic flux-rope structure of the simulated CME at t = 31, t = 51, and t = 71 hr as well as the CIR in the radial range between 20 and 500 Rs. Here, the colors denote the radial velocity (V  r ). Panels (b), (c), (e), and (f) show distributions of the magnetic field strength B tot (b, c) and the radial velocity V  r  (e, f) on the surfaces at 275 (b, e) and 366 Rs (c, f), with the CME circled by the red lines and the CIR by the black lines. Panels (d) and (g) show distributions of the B tot (d) and V  r  (g) on the surface at 366 Rs for the simulation of the background solar wind, with the CIR circled by the black lines. The area circled by the red dashed lines shows where the CIR for the simulation of the CME is located.
Paper: Interplanetary Rotation of 2021 December 4 Coronal Mass Ejection on Its Journey to Mars
Authors: Mengxuan Ma, Liping Yang, Fang Shen, Chenglong Shen, Yutian Chi, Yuming Wang, Yufen Zhou, Man Zhang, Daniel Heyner, Uli Auster, Ingo Richter, Beatriz Sanchez-Cano
Figure caption: Panel (a) shows the 3D magnetic flux-rope structure of the simulated CME at t = 1 hr. The black eye shows the observation direction of SOHO/LASCO. Panels (b) and (c) show the synthetic white light images of STEREO-A/COR2 (b) and SOHO/LASCO C3 (c), which accord with real white light observations by STEREO-A/COR2 (d) and SOHO/LASCO C3 (e), respectively. Panels (d) and (e) show the comparison of GCS-fitted CME and real white light observations by STEREO-A/COR2 (d) and SOHO/LASCO C3 (e).
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: Corner plot of a selection of best-fitting parameters of the RELXILL+BBODY+XILLVER model. The contours in the 2D histograms show 68%, 90%, and 95% confidence levels. All the values of the best-fitted parameters are listed in Table 3, Model 4.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: Structures of the jet-induced flows in the r10 models, Q42-η5-r10, Q43-η5-r10, Q44-η5-r10, Q42-η5-r10-M, and Q42-η5-r10-P, at the end of simulations. See Table 1 for the model parameters. (a)–(e) 2D slice images of ﹩\mathrm{log}(\rho /{\rho }_{c})﹩ in the x–z plane through y = 0. (f)–(j) 2D slice images of the vertical velocity, v  z /c, in the same plane. (k)–(o) The vertical velocity averaged over the azimuthal angle ϕ, 〈v  z (R, z)/c〉 ϕ , at three different z's: z = 0 (red), z 1 ≡ l jet/3 (blue), and z 2 ≡ 2l jet/3 (black). Here ﹩R={\left({x}^{2}+{y}^{2}\right)}^{1/2}﹩ is the transverse distance from the z-axis, and l jet is the jet propagation length. The inset of each panel of (k)–(o) shows the vertical velocity along the jet axis, v  z (R = 0)/c, across the z-distance.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: (a)–(b) 2D slice images of the magnetic field strength in the local fluid frame, ﹩B^{\prime} (x,z)﹩, and in the computational frame, B(x, z), at t end for the Q42-η5-r10 model. (c)−(d) 2D slice images of the synchrotron volume emissivity in the local fluid frame, ﹩j{{\prime} }_{\nu ^{\prime} }(x,z)﹩ at ﹩\nu ^{\prime} =150\,\mathrm{MHz}﹩, and in the computational frame, j  ν (x, z) at ν = 150 MHz, for the same model. The images in (a)−(d) are in the x–z plane through y = 0. (e) A schematic diagram of a pair of approaching and receding jets, tilted with the observation angle, θ obs. The projected distances to the brightest spot, d  b , and to the faintest edge, d  f , from the injection point are illustrated. (f) Synchrotron surface brightness map, the log of the intensity calculated by integrating the synchrotron emissivity along the LOS, at ν = 150 MHz for a pair of approaching and receding jets displayed with θ obs = 60° for the Q42-η5-r10-P model. The unit is arbitrary. For illustrative purposes, a circle is inserted in the middle to represent the core region that contains the central black hole.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: 2D slice distributions of the Mach number (M  s ) of shocks (a), (d), the magnitude of the velocity shear Ωshear (the left side with x < 0 on panels (b) and (e)), the relativistic shear coefficient ﹩{{ \mathcal S }}_{r}﹩ (the right side with x > 0 on panels (b) and (e)), the magnitudes of the total vorticity Ω t  (the left side with x < 0 on panels (c) and (f)), and the vorticity excluding the shear Ω− (the right side with x > 0 on panels (c) and (f)) for the Q42-η5-r10 and Q42-η5-r10-M models. (g)–(i) PDFs of the shock Mach number, M  s , for the six models listed in Table 1. (j)–(l) PDFs of the shock speed, β  s  = v  s /c, for the same six models. Different line types are used for the shock zones in the jet-spine flow (red dashed lines), backflow (blue dotted–dashed lines), and shocked ISM (green dotted lines), and for the bow shock surface (cyan solid lines). The black solid lines plot the PDFs for all the shocks identified in the simulation domain. The shock zones with M  s  ≥ 1.01 are included, and the quantities shown are at t end. Here, N  t  is the total number of grid zones in the volume encompassed by the bow shock surface, and N  j  is the number of zones occupied by the initial jet radius.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: 2D maps of the synchrotron intensity, ﹩\mathrm{log}[{I}_{\nu }(x,z)/{I}_{\nu }^{\max }({\theta }_{\mathrm{obs}}=90^\circ )]﹩, at ν obs = 150 MHz for the approaching jet (top) and receding counterjet (bottom) at t end for the Q42-η5-r10, Q42-η5-r10-P, and Q44-η5-r100 models. The intensity is calculated with σ = 2.2. For each model, two cases with θ obs = 60° and 30◦ are presented. Each panel shows a pair of jet and counterjet, with intensities normalized by the peak value for each model as viewed at θ obs = 90°, ﹩{I}_{\nu }^{\max }({\theta }_{\mathrm{obs}}=90^\circ )﹩. For both the jet and counterjet maps in each panel, the relative intensity ratios, ﹩{ \mathcal F }={I}_{\nu }^{\max }/{I}_{\nu ,N}^{{\rm{Q}}42{\rm{r}}10}﹩, are provided, where ﹩{I}_{\nu }^{\max }﹩ is the peak intensity of each jet (or counterjet), and ﹩{I}_{\nu ,N}^{{\rm{Q}}42{\rm{r}}10}﹩ is the peak value of the face-on map (θ obs = 90°) for the Q42-η5-r10 model. Here, 〈Γ〉spine ≈ 2.1, 2.1, and 2.8 for Q42-η5-r10, Q42-η5-r10-P, and Q44-η5-r100, respectively. For illustrative purposes, a circle is inserted in the middle to represent the core region that contains the central black hole.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: 2D maps of the synchrotron intensity integrated along the LOS, ﹩\mathrm{log}[{I}_{\nu }(x,z)/{I}_{\nu }^{\max }]﹩, at ν obs = 150 MHz, where the intensity is normalized by its peak value, ﹩{I}_{\nu }^{\max }﹩. Each panel is labeled with the model name, σ, θ obs, and the relative intensity ratio, ﹩{ \mathcal F }\equiv {I}_{\nu }^{\max }/{I}_{\nu ,N}^{{\rm{Q}}42{\rm{r}}10}﹩, where ﹩{I}_{\nu ,N}^{{\rm{Q}}42{\rm{r}}10}﹩ is the peak value of the face-on map (θ obs = 90°) for the Q42-η5-r10 model with σ = 2.2. All maps are displayed at t end. The mean Lorentz factor of the jet-spine flow, 〈Γ〉spine, is 2.1, 2.1, 1.7, 8.7, and 2.8 for Q42-η5-r10, Q42-η5-r10-P, Q42-η5-r10-M, Q44-η5-r10, and Q44-η5-r100, respectively (see Table 1). Note that with relativistic beaming, the Doppler factor is ﹩{ \mathcal D }=1/({\rm{\Gamma }}[1-(v/c)\cos \theta ])﹩. So the emission is boosted most for mildly relativistic sources viewed at a small LOS angle, θ ≲ 30°.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: Same as Figure 1, except for the r100 models, Q44-η5-r100, Q45-η5-r100, and Q45-η3-r100, shown. See Table 1 for the model parameters.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: 2D slice images of the adiabatic index, γ, for Q42-η5-r10, Q42-η5-r10-P, and Q44-η5-r100. In these models, the jet inflow is hotter than the background, with T  j  ≈ T  b /η and γ  j  ≈ 1.6 at injection. After passing through shocks, the jet fluid becomes thermally relativistic, with γ ≈ 1.47 (dark blue), while the background gas remains nonrelativistic with γ = 5/3 (dark red). In the backflow region, shown primarily in a whitish peach hue, the jet material mixes with the ambient gas, mainly through the Kelvin–Helmholtz instability.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: (a) Deceleration factor, ﹩{{ \mathcal R }}_{\mathrm{dec}}\equiv {v}_{\mathrm{head}}/{v}_{j}﹩, vs. the initial Lorentz factor of the jet, Γ j . (b) ﹩{{ \mathcal R }}_{\mathrm{dec}}﹩ vs. the mean Lorentz factor of the jet-spine flow, 〈Γ〉spine. (c) Jet-spine spreading angle at z 2, θ  j (z 2), vs. the initial jet-head speed, v head*. All eight jet models listed in Table 1 are shown with different symbols.
Paper: A Simulation Study of Low-power Relativistic Jets: Flow Dynamics and Radio Morphology of FR-I Jets
Authors: Ayan Bhattacharjee, Jeongbhin Seo, Dongsu Ryu, Hyesung Kang
Figure caption: Time variations of (a) the jet-head advance speed, v head, (b) the axial ratio, ﹩{ \mathcal A }={l}_{\mathrm{jet}}/{ \mathcal W }﹩, and (c) the lateral width, ﹩{ \mathcal W }﹩, of the lobe for all the models listed in Table 1. The r100 models that generate the jet flows propagating beyond the galactic core (∼kiloparsec) are denoted with bold lines.
Paper: Synthesis and Spectroscopic Characterization of Interstellar Candidate Ethynyl Thiocyanate: HCCSCN
Authors: Elena R. Alonso, Aran Insausti, Lucie Kolesniková, Iker León, Brett A. McGuire, Christopher N. Shingledecker, Marcelino Agúndez, José Cernicharo, Víctor M. Rivilla, Carlos Cabezas, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Jean-Claude Guillemin
Figure caption: Transitions used to constrain the 3σ upper limit for HCCSCN in the GBT PRIMOS observations of Sgr B2(N) in the case of a cold, extended component in absorption (left) and a warm, compact component (right). Hyperfine splitting is not resolved at these line widths (see text), so the unresolved quantum numbers are provided.
Paper: Synthesis and Spectroscopic Characterization of Interstellar Candidate Ethynyl Thiocyanate: HCCSCN
Authors: Elena R. Alonso, Aran Insausti, Lucie Kolesniková, Iker León, Brett A. McGuire, Christopher N. Shingledecker, Marcelino Agúndez, José Cernicharo, Víctor M. Rivilla, Carlos Cabezas, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Jean-Claude Guillemin
Figure caption: Broadband CP-FTMW spectrum of HCCSCN. The red rhombus indicates measured transition. The inset shows the nuclear quadrupole hyperfine structure for 20,2 ← 10,1 rotational transition.
Paper: Synthesis and Spectroscopic Characterization of Interstellar Candidate Ethynyl Thiocyanate: HCCSCN
Authors: Elena R. Alonso, Aran Insausti, Lucie Kolesniková, Iker León, Brett A. McGuire, Christopher N. Shingledecker, Marcelino Agúndez, José Cernicharo, Víctor M. Rivilla, Carlos Cabezas, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Jean-Claude Guillemin
Figure caption: Transitions used to constrain the upper limit for HCCSCN toward the G+0.693 molecular cloud. The gray histogram shows the observed spectra, the red curve indicates the LTE model using the upper limit derived for the column density (see the text), and the purple line shows the line emission from all the molecules identified in the region (including the contribution of HCCSCN). As in Figure 4 hyperfine splitting is not resolved, so the unresolved quantum numbers are provided.
Paper: Synthesis and Spectroscopic Characterization of Interstellar Candidate Ethynyl Thiocyanate: HCCSCN
Authors: Elena R. Alonso, Aran Insausti, Lucie Kolesniková, Iker León, Brett A. McGuire, Christopher N. Shingledecker, Marcelino Agúndez, José Cernicharo, Víctor M. Rivilla, Carlos Cabezas, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Jean-Claude Guillemin
Figure caption: Section of the room-temperature millimeter-wave spectrum of HCCSCN. The upper panel shows the experimental spectrum, while the lower panel illustrates a stick reproduction of the ground state (G.S.) and v 9 = 1, 2 excited vibrational states using the spectroscopic constants from Table 1. The trend of the relative intensities is not always consistent in theory and experiment due to the performance of the experimental setup (multiplication chain, cell transmission, and detector sensitivity).
Paper: Synthesis and Spectroscopic Characterization of Interstellar Candidate Ethynyl Thiocyanate: HCCSCN
Authors: Elena R. Alonso, Aran Insausti, Lucie Kolesniková, Iker León, Brett A. McGuire, Christopher N. Shingledecker, Marcelino Agúndez, José Cernicharo, Víctor M. Rivilla, Carlos Cabezas, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Jean-Claude Guillemin
Figure caption: Observed lines of HCCSCN with the QUIJOTE line survey. The abscissa corresponds to the rest frequency in MHz. The ordinate is the antenna temperature corrected for atmospheric and telescope losses in mK. Blanked channels correspond to negative features produced in the folding of the frequency-switching data. The synthetic spectrum for each transition is shown in red. The physical parameters used to generate them are given in the text.
Paper: Synthesis and Spectroscopic Characterization of Interstellar Candidate Ethynyl Thiocyanate: HCCSCN
Authors: Elena R. Alonso, Aran Insausti, Lucie Kolesniková, Iker León, Brett A. McGuire, Christopher N. Shingledecker, Marcelino Agúndez, José Cernicharo, Víctor M. Rivilla, Carlos Cabezas, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Jean-Claude Guillemin
Figure caption: Optimized structure of the HCCSCN molecule depicted in the ab inertial plane.
Paper: The Effect of Anisotropic Energy Injection on the Ejecta Emission
Authors: Yu-Fei Li, Da-Bin Lin, Li Zhou, Jia Ren, Zhi-Lin Chen, En-Wei Liang
Figure caption: The multband light curve of the emission from the ejecta with anisotropic energy injection, including 1 keV (X-ray band), 30 eV (U-band), and 1 eV (optical band). The left-hand panel shows the light curves of the ejecta, which are represented by solid lines of different colors (along the jet’s axis direction, θ v = 0°), each corresponding to a different jet breakout time from the ejecta (the magenta lines for t b = 1.7 s, the red lines for t b = 6 s, and the black lines for t b = 18 s). The blue (X-ray band) and green (U-band) dashed lines represent the emission of from the Poynting-flux-dominated jet (D. Xiao & Z.-G. Dai 2017; D. Xiao et al. 2019), the blue (X-ray band) and green (U-band) dotted lines represent the light curve of the emission of afterglows in GRB 170817A (J. Ren et al. 2020). The right-hand panel shows the multband light curve of the emission from the ejecta with anisotropic (the black dashed lines) and isotropic (the red solid lines) energy injection (along the equatorial direction, viewing angles θ v = 90°). The blue dotted line represents the emission light curve of the ejecta at breakout time t b = 18 s.
Paper: The Effect of Anisotropic Energy Injection on the Ejecta Emission
Authors: Yu-Fei Li, Da-Bin Lin, Li Zhou, Jia Ren, Zhi-Lin Chen, En-Wei Liang
Figure caption: The evolution of the jet energy injecting efficiency ξ jet (left-hand panel) and magnetar wind energy efficiency ξ pw (right-hand panel). In the left-hand panel the solid lines represent the breakout time of the jet at t b = 0.2 s,  1.7 s,  6.0 s, and  18 s corresponding to the red, blue, green, and black solid lines, respectively. In the right-hand panel the solid line represents the magnetar wind energy efficiency at different opacities (lanthanide-free dynamical ejecta) κ = 0.2 cm2 g−1 (red line), 1.0 cm2 g−1 (blue line), and the black dashed line opacity is κ = 10 cm2 g−1 (lanthanide-rich dynamical ejecta, H. Gao et al. 2015).
Paper: The Effect of Anisotropic Energy Injection on the Ejecta Emission
Authors: Yu-Fei Li, Da-Bin Lin, Li Zhou, Jia Ren, Zhi-Lin Chen, En-Wei Liang
Figure caption: The left-hand panel shows the effect of the characteristic angle θ c of the structured jet on the emission light curves of the ejecta. The distributions of the blue solid line, green solid line, and red solid line correspond to the characteristic angle θ c = 5°, 3°, 1° of the structured jet. The right-hand panel shows the effect of the energy distribution ratio of magnetar f iso on the emission light curves of the ejecta. The distributions of the blue solid line, green solid line, and red solid line correspond to the EM spin energy fraction is f iso = 0.2,  0.5,  0.8.
Paper: The Effect of Anisotropic Energy Injection on the Ejecta Emission
Authors: Yu-Fei Li, Da-Bin Lin, Li Zhou, Jia Ren, Zhi-Lin Chen, En-Wei Liang
Figure caption: Panel (a): the distribution of mass of ejecta with angle θ. Panel (b): the multband light curve of the emission from the ejecta with anisotropic (the red line) and isotropic (the blue line) merger ejecta, including 1 keV (X-ray band), 30 eV (U-band), and 1 eV (optical band).
Paper: High Spectral Resolution Observations of Propynal (HCCCHO) toward TMC-1 from the GOTHAM Large Program on the GBT
Authors: Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Model spectrum (red trace) of C6H based on transition rest frequencies taken from the CDMS online catalog (ID#:c073501 before the 2023 December update) compared to the astronomical spectrum (black trace) of TMC-1 around 15247.98 MHz. New fits to the C6H rest frequencies were reported in Remijan et al. (2023) and are available at https://cdms.astro.uni-koeln.de/ species ID#:c073501.
Paper: High Spectral Resolution Observations of Propynal (HCCCHO) toward TMC-1 from the GOTHAM Large Program on the GBT
Authors: Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Astronomical data taken as part of the GOTHAM program and the subsequent fits for four velocity components of HCCCHO, illustrating the mismatch in the rest frequencies taken from the CDMS catalog (red trace) and the measured frequencies from the GBT (black trace). HCCCHO transition quantum numbers and upper state energy levels (K) are given in the top-right corner of each panel.
Paper: High Spectral Resolution Observations of Propynal (HCCCHO) toward TMC-1 from the GOTHAM Large Program on the GBT
Authors: Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Astronomical data taken as part of the GOTHAM large program on the GBT and the subsequent fits for four velocity components of HCCCHO based on the new spectral line fitting (orange trace) and the measured frequencies from the GBT (black trace). The panel description is the same as in Figure 2.
Paper: Light Echoes of Protoplanetary Disks
Authors: Austin J. King, Benjamin C. Bromley
Figure caption: Model light echoes: each of the panels above show the shape of a modeled echo light curve from an optically thick, circumstellar structure. The top two panels show a more extended disk, modeled with inner radius r in = 2 au and outer radius r out = 2r in. The bottom panels show the same information for a ring-like structure, with r in = 2 au and r out = 1.1r in. The two left panels represent a near face-on disk (i = 5°) and the two right panels represent a disk inclination of i = 45°. All curves are modeled with an albedo of 0.5.
Paper: Light Echoes of Protoplanetary Disks
Authors: Austin J. King, Benjamin C. Bromley
Figure caption: Geometric disk model: (a) a cross sectional side view along the x-axis of the protoplanetary disk. The flash at the origin depicts a solar flare. The yellow squiggles show the path of a photon as it strikes at a distance r on the disk and reflects toward the observer at a scattering angle of θ  s . i denotes the inclination of the disk relative to the observer (i = 0° = face-on, i = 90° = edge-on), H is the physical height of the disk at its inner radius, r in and r out is the outer radius. (b) A top-down view of the disk along the z-axis. r in and r out once again denote inner and outer radii, respectively. The yellow ring shows all angles, phi, that a photon traveling to distance r will interact with before scattering to the observer. Note: in this orientation, the portion of the disk aligned with the negative y-axis would be defined as the “nearside,” as it is inclined toward the observer.