adsabs/AstroCLIMB huggingface dataset:
Paper: MUSSES2020J: The Earliest Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063
Authors: Ji-an Jiang, Naoki Yasuda, Keiichi Maeda, Nozomu Tominaga, Mamoru Doi, Željko Ivezić, Peter Yoachim, Kohki Uno, Takashi J. Moriya, Brajesh Kumar, Yen-Chen Pan, Masayuki Tanaka, Masaomi Tanaka, Ken'ichi Nomoto, Saurabh W. Jha, Pilar Ruiz-Lapuente, David Jones, Toshikazu Shigeyama, Nao Suzuki, Mitsuru Kokubo, Hisanori Furusawa, Satoshi Miyazaki, Andrew J. Connolly, D. K. Sahu, G. C. Anupama
Figure caption: Light curves of MUSSES2020J, FBUTs (Vinkó et al. 2015; Perley et al. 2019; Ho et al. 2020; Perley et al. 2021; here we classify Dougie as an FBUT due to the extremely high luminosity and fast light-curve decline in UV), SN 2018gep (Ho et al. 2019a), and normal FBOTs discovered by previous HSC and PS1 observations (broken lines; 3σ g-band nondetection limits are given as open triangles; Tanaka et al. 2016; Tampo et al. 2020; Drout et al. 2014). Light curves of some optically selected TDEs and candidates (Gezari et al. 2012; Arcavi et al. 2014; Blagorodnova et al. 2017) are plotted with transparent symbols for comparisons. Galactic extinction of MUSSES2020J has been corrected, assuming an extinction to reddening ratio R  V  of 3.1 (Schlafly & Finkbeiner 2011). The gray stripe indicates the period of the MUSSES2020 Subaru/HSC observation. The 3σ nondetection limits of 27.4 mag (g) and 26.2 mag (r) of Subaru/HSC observations at about 160 days (rest frame) after the discovery are not shown on the plot. Transients with comparable rest-frame central-wavelength light curves are given by similar colors, and redder colors represent observations in redder rest-frame wavelengths.
Paper: MUSSES2020J: The Earliest Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063
Authors: Ji-an Jiang, Naoki Yasuda, Keiichi Maeda, Nozomu Tominaga, Mamoru Doi, Željko Ivezić, Peter Yoachim, Kohki Uno, Takashi J. Moriya, Brajesh Kumar, Yen-Chen Pan, Masayuki Tanaka, Masaomi Tanaka, Ken'ichi Nomoto, Saurabh W. Jha, Pilar Ruiz-Lapuente, David Jones, Toshikazu Shigeyama, Nao Suzuki, Mitsuru Kokubo, Hisanori Furusawa, Satoshi Miyazaki, Andrew J. Connolly, D. K. Sahu, G. C. Anupama
Figure caption: Physical properties based on the blackbody fits of multiband observations of MUSSES2020J. In the top panel, data points show the luminosity inferred from the sum of the total Stefan–Boltzmann luminosity of the thermal component. Data points in the middle and bottom panels show the evolution of the best-fit photospheric radius and blackbody temperature, respectively. Error bars of the panels are provided at the 1σ confidence level. Around the g-band maximum when the temperature is high (as inferred from the color evolution in Figure 3), the peak of the blackbody radiation curve is at a very short wavelength. Only the lower limits for the blackbody temperature and luminosity, and thus the upper limit for the radius, can be placed by the blackbody fit in the observed wavelength regime. The triangle in each panel corresponds to the 4σ upper/lower limit of each parameter.
Paper: MUSSES2020J: The Earliest Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063
Authors: Ji-an Jiang, Naoki Yasuda, Keiichi Maeda, Nozomu Tominaga, Mamoru Doi, Željko Ivezić, Peter Yoachim, Kohki Uno, Takashi J. Moriya, Brajesh Kumar, Yen-Chen Pan, Masayuki Tanaka, Masaomi Tanaka, Ken'ichi Nomoto, Saurabh W. Jha, Pilar Ruiz-Lapuente, David Jones, Toshikazu Shigeyama, Nao Suzuki, Mitsuru Kokubo, Hisanori Furusawa, Satoshi Miyazaki, Andrew J. Connolly, D. K. Sahu, G. C. Anupama
Figure caption: Upper panel: a host spectrum modeled by HSC SSP multiband photometries (blue points; Tanaka 2015). Red pointings are synthesized photometries with the model spectrum. Lower panel: A combined 1200 s × 5 host spectrum taken by Gemini North/GMOS on 2021 July 18 (UTC). A bimodal emission feature around observed wavelength 7690 Å (right zoom-in inset) was detected in all 1200 s exposures (left zoom-in inset). The central wavelengths of 7686.3 Å and 7691.6 Å of the gray stripes correspond to the [O II] λ3726.1 and λ3728.8 lines at a redshift of 1.0628, respectively.
Paper: MUSSES2020J: The Earliest Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063
Authors: Ji-an Jiang, Naoki Yasuda, Keiichi Maeda, Nozomu Tominaga, Mamoru Doi, Željko Ivezić, Peter Yoachim, Kohki Uno, Takashi J. Moriya, Brajesh Kumar, Yen-Chen Pan, Masayuki Tanaka, Masaomi Tanaka, Ken'ichi Nomoto, Saurabh W. Jha, Pilar Ruiz-Lapuente, David Jones, Toshikazu Shigeyama, Nao Suzuki, Mitsuru Kokubo, Hisanori Furusawa, Satoshi Miyazaki, Andrew J. Connolly, D. K. Sahu, G. C. Anupama
Figure caption: Color evolution of MUSSES2020J and other FBUTs. The color evolution of MUSSES2020J shows that the UV color is relatively red in the early time and gets bluer slowly in the light-curve rising phase. Considering the redshift effect, the observed g − r color evolution of MUSSES2020J is consistent with the UVW2 − UVW1 color of AT 2018cow in the postmaximum phase. In addition to a peculiar plateau feature in the optical light curve of Dougie (Figure 1), its postmaximum UV color evolution is redder and slower than those of MUSSES2020J and AT 2018cow, suggesting a lower temperature and possibly a different origin from other FBUTs.
Paper: MUSSES2020J: The Earliest Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063
Authors: Ji-an Jiang, Naoki Yasuda, Keiichi Maeda, Nozomu Tominaga, Mamoru Doi, Željko Ivezić, Peter Yoachim, Kohki Uno, Takashi J. Moriya, Brajesh Kumar, Yen-Chen Pan, Masayuki Tanaka, Masaomi Tanaka, Ken'ichi Nomoto, Saurabh W. Jha, Pilar Ruiz-Lapuente, David Jones, Toshikazu Shigeyama, Nao Suzuki, Mitsuru Kokubo, Hisanori Furusawa, Satoshi Miyazaki, Andrew J. Connolly, D. K. Sahu, G. C. Anupama
Figure caption: Locations of MUSSES2020J and the nucleus of the host galaxy. Red spots are centers of the host galaxy measured from HSC SSP broadband images (griz). The coordinates of MUSSES2020J in g and r bands are shown by blue and green spots, respectively. Due to the faintness of MUSSES2020J in the first two nights, here we only present coordinates measured from observations from the third night. The 1σ astrometric uncertainty regions of each measurement are denoted by transparent colors. The entire selected area is denoted by a white box at the center of the HSC g, r, and i composite multicolor thumbnail image of the host galaxy shown in the bottom-right corner. Blue and red crosses in the box indicate the locations of MUSSES2020J (g band) and the host nucleus (i band), respectively.
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: (A) synchrones computed for ejection 20, 40, 60, 80, and 100 days prior to the date of observation and (B) syndynes, showing the paths of particles with β = 0.1, 0.03, 0.01, 0.003, and 0.001. Celestial north points up and east points to the left.
Paper: Multiplicity Statistics of Stars in the Sagittarius Dwarf Spheroidal Galaxy: Comparison to the Milky Way
Authors: Victoria Bonidie, Travis Court, Christine Mazzola Daher, Catherine E. Fielder, Carles Badenes, Jeffrey Newman, Maxwell Moe, Kaitlin M. Kratter, Matthew G. Walker, Steven R. Majewski, Christian R. Hayes, Sten Hasselquist, Keivan Stassun, Marina Kounkel, Don Dixon, Guy S. Stringfellow, Joleen K. Carlberg, Borja Anguiano, Nathan De Lee, Nicholas W. Troup
Figure caption: Upper panel: number of Sgr dSph stars with ﹩{\rm{\Delta }}{\mathrm{RV}}_{\max }﹩ above the given threshold (red squares), together with the 50th rank (black line), 16th–84th ranks (dark blue region), and 2nd–98th ranks (light blue region) of values seen in the MW analog samples. Lower panel: difference between the number of RV variable stars measured in the Sgr and MW analog samples (orange triangles), alongside our estimate for the difference that would arise from the offset of [α/H] values between the samples (blue squares).
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: FWHM of the dust tail as a function of the angular distance from the nucleus, observed at plane crossing on UT 2020 September 17. Best-fit lines (Equation (3)) to the east of the nucleus indicate ejection velocities 4 ± 1 m s−1 (for β = 1 particles).
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: Composite HST images of active asteroid P/2020 O1 marked with the UT dates of the observations. A color bar (logarithmic scale), the projected antisolar direction (−S), and the negative heliocentric velocity vector (−V) are indicated. Each panel shows a region 18.″0 × 2.″5 in the standard orientation: celestial north points up and east points to the left.
Paper: Multiplicity Statistics of Stars in the Sagittarius Dwarf Spheroidal Galaxy: Comparison to the Milky Way
Authors: Victoria Bonidie, Travis Court, Christine Mazzola Daher, Catherine E. Fielder, Carles Badenes, Jeffrey Newman, Maxwell Moe, Kaitlin M. Kratter, Matthew G. Walker, Steven R. Majewski, Christian R. Hayes, Sten Hasselquist, Keivan Stassun, Marina Kounkel, Don Dixon, Guy S. Stringfellow, Joleen K. Carlberg, Borja Anguiano, Nathan De Lee, Nicholas W. Troup
Figure caption: The visit spectra for the Sgr dSph member, 2M09133453+2314547, shown around the Fe II line at 15,773.5860 Å and the Fe I line at 15,776.733 Å (Kramida et al. 2021). The ﹩{\rm{\Delta }}{\mathrm{RV}}_{\max }\,﹩ for this star is 5.42 km s−1, corresponding to the difference between the visit spectra highlighted in red (MJD 57680) and blue (MJD 57378).
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: Lightcurve of O1 in data from UT 2020 November 25 and UT 2020 December 25. The December data have been shifted assuming a double-peaked period of 1.67 hr. A sine curve with a period of 0.83 hr was plotted with the dashed line.
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: Comparison between HST images (upper) and Monte Carlo models (lower) at three epochs of observation. Adopted model parameters are described in Section 4.1. Celestial north points up and east points to the left.
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: Scattering cross section as a function of time, expressed as Day of Year (DOY = 1 on UT 2020 January 1). The radii of the apertures (in units of 102 km) are indicated.
Paper: Searching for a Hypervelocity White Dwarf SN Ia Companion: A Proper-motion Survey of SN 1006
Authors: Joshua V. Shields, Wolfgang Kerzendorf, Matthew W. Hosek, Ken J. Shen, Armin Rest, Tuan Do, Jessica R. Lu, Andrew G. Fullard, Giovanni Strampelli, Alfredo Zenteno
Figure caption: Position (left) and proper-motion (right) residuals of DECam vs. Gaia measurements for cross-matched sources in R.A. and decl. over uncertainty in each dimension. We expect 68% of sources to be smaller than 1σ. We find ∼92% of sources in position space and ∼85% of sources in proper-motion space lie within this region, suggesting that our errors may be overestimated.
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: The blue curve shows the empirical dust grain ejection velocity from O1 as a function of particle radius. Black curves show the velocity–radius relation from the SSA and the Whipple model, respectively, as described in the text.
Paper: Hubble Space Telescope Observations of Active Asteroid P/2020 O1 (Lemmon-PANSTARRS)
Authors: Yoonyoung Kim, David Jewitt, Jessica Agarwal, Max Mutchler, Jing Li, Harold Weaver
Figure caption: Measured surface brightness along the tail (black line), with sample models showing the effect of maximum particle size (β min). The size distribution index (q) does not significantly affect the surface brightness gradient of the west tail.
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: Quantities relevant to the nonlinear phase, all for a simulation with ξ = 2.8 × 106: (a) The early evolution of ﹩{\hat{\omega }}^{2}﹩ and ﹩\hat{E}﹩. The peaks in ﹩{\hat{\omega }}^{2}﹩ occur later than the zeros of ﹩\hat{E}﹩. (b) Comparison of ﹩{\hat{f}}_{-}﹩ at the second zero-crossing with the analytic model for ﹩{\hat{f}}_{-,\mathrm{new}}﹩ in Equation (37). The value of ﹩{\hat{f}}_{-}﹩ at negative u is larger than that of ﹩{\hat{f}}_{-,\mathrm{new}}﹩ in part because ﹩{\hat{f}}_{-}﹩ includes electrons already present at the time of screening, which are part of ﹩{\hat{f}}_{-,\mathrm{old}}﹩, that have backwashed to negative u. (c) Phase space at the second zero-crossing, with every 500th particle marked. (d) An exponential decay fit, ﹩\overline{\hat{E}\left(\hat{t}\right)}={e}^{-0.0016\hat{t}}﹩. The simulated ﹩\hat{E}﹩ diverges from the fit near the transition to linearity, discussed in Section 7. (e) The value of ﹩{\hat{f}}_{+}﹩ near the end of the nonlinear period, ﹩\hat{t}=5130﹩, showing several bounces stacked on top of each other. (f) Fit of the decay constant in ﹩\overline{\hat{E}}\left(\hat{t}\right)={e}^{-a\left(\hat{t}-{\hat{t}}_{\mathrm{screen}}\right)}﹩ as found in the simulation and predicted by the fit presented in Equation (49).
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: Evolution of parameters important to the transition to linearity in simulations with (left) ξ = 2.8 × 106 and (right) ξ = 2.3 × 107, shown in blue. Displayed are (from top to bottom) the squared frequency of the oscillation, the ratio of the rms amplitude of the electric field in the simulation box to the frequency (which characterizes the change in particle u caused by the wave), and the normalized rate of change of the oscillation frequency. The dashed orange lines show the same quantities in a simulation run starting from an electric field with a finite k, as discussed at the end of Section 7. The plotted frequency is the value of Equation (24) evaluated across the box, equivalent to the quantity plotted for the k = 0 simulation, even though this simulation has spatial variation.
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: Depiction of the fragmentation of the ξ = 2.8 × 106 simulation into higher-k modes. The first plot shows the electric field in the simulation box before the k = 0 breakup; the second shows the electric field after the fragmentation. Both of these plots show the full simulation domain, but the skin depth shrinks as time progresses, such that the axis labels of the two plots are different. The final plot zooms in on a small section of the box at three close times; the black lines move at the speed of light between the times and are overrun by the peak of one oscillation, indicating that the modes are superluminal.
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: Comparisons of important quantities for different temperatures: 0.1 mc 2 (blue), 1 mc 2 (orange), and 10 mc 2 (red). Note that, in the right plot, the x-axis extends to different values of x in units of skin depth, even though the simulation box size is the same because higher-temperature simulations have a larger skin depth.
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: The electric field in a simulation with ξ = 2.8 × 106 compared to an oscillation with amplitude given by Equation (55) and time-dependent frequency given by Equation (24). The comparison begins after the simulation has fragmented into finite-k modes, as discussed in Section 7.
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: Electron distribution function at ﹩{\hat{t}}_{\mathrm{screen}}﹩ for ξ = 2.8 × 106 from the analytic solution, Equation (36), and from the simulation.
Paper: Electric Field Screening in Pair Discharges and Generation of Pulsar Radio Emission
Authors: Elizabeth A. Tolman, A. A. Philippov, A. N. Timokhin
Figure caption: Comparison of electric field evolution in the first kinetic bounce shown in Figure 2 with its fluid analog.
Paper: On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath
Authors: Ore Gottlieb, Serena Moseley, Teresita Ramirez-Aguilar, Ariadna Murguia-Berthier, Matthew Liska, Alexander Tchekhovskoy
Figure caption: Time evolution of the jet and mass properties as measured at r = 10r  g  in different models. Panel (a): Accretion rate on the BH exhibits a continuous decrease over the first second before stabilizing. Panel (b): Gravitationally bound mass rapidly decays from ∼0.1  M ⊙ to ∼(10−3−10−4) M ⊙ as the torus is consumed by the BH. Panel (c): When the jet is launched successfully, its launching efficiency (﹩\eta ={L}_{j,0}/\dot{M}{c}^{2}﹩, where L  j,0 is the jet power upon launching, or the radial energy flux excluding the rest energy flux) builds over the first ∼0.5 s before reaching a MAD state. Panel (d): The decrease in the accretion rate leads to luminosity drop to typical sGRB luminosities. If ﹩\,{v}_{\min }\lt \,{v}_{\mathrm{esc}}﹩ and β  p  is not low enough, massive accretion on the jet axis inhibits a successful jet launching (model α3d1Mb).
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Top row: gas density profile at the midplane, normalized to the initial midplane gas pressure, across the simulation domain for high-res, A = 0.5. Second row: dust-to-gas ratio for three snapshots in the vicinity of t = 180Ω−1. Wide particle filaments form everywhere, and a steady-state particle pileup occurs in the region of minimum headwind η. The dust-to-gas ratio peaks at Z ≳ 0.03 with a local headwind of Π ≈ 0.0283. Third row: headwind parameter Π. Bottom row: normalized dust-to-gas ratio Z/Π, along with the SI criteria (dotted lines). These criteria are also shown in Figure 6.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Snapshot of high-res ,A=0.5 at t = 180Ω−1, when the maximum particle density is reached (Figure 3). The third row shows the mean particle density; ρ 0 is the initial midplane gas density at x = ±∞ . The bottom rows zoom in farther to two regions that show interesting structure. They show a slice of the simulation at y = 0. The left region shows features of Kelvin–Helmholtz turbulence. The peak density at the midplane is a temporary aberration; as turbulence develops the density drops (Figure 7). The right region shows a small density peak, but little structure. The local pressure gradient is Π ≈ 0.028.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Snapshot of high-res ,A=0.5 at t = 264.7Ω−1, which is our final snapshot and it is later than the time when Run Z2T1 of Li & Youdin (2021) formed filaments. The third row shows the mean particle density; ρ 0 is the initial midplane gas density. The bottom row zooms in farther to the regions with the highest Z. They show a slice of the simulation at y = 0. Neither region shows strong clumping. For the region on the right, Z ≈ 0.027 and Π ≈ 0.226, so the lack of strong clumping is expected. But on the left, Z ≈ 0.025 and Π ≈ 0.029 is well inside the region where strong clumping would occur if the conditions present in the pressure bump were met over a wider radial region of the disk.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Solid abundance criterion for strong clumping in terms of Z/Π vs. τ as reported in Carrera et al. (2015, blue), Yang et al. (2017, red), and Li & Youdin (2021, green), but for the case without a pressure bump. The orange star marks the (τ, Z/Π) for the high-res ,A=0.5 snapshots in Figure 4 (τ ≈ 0.0123, Z/Π ≈ 1.06). If the conditions in the density peak in our high-res run were applied over an extended radial region of the disk, previous works show that the SI would produce strong clumping.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Maximum particle density, normalized to the initial midplane gas density, for all runs. Blue: A = 0.5 cannot form planetesimals despite having enough resolution to resolve the fastest-growing modes of the SI. Green and orange: A = 0.6 forms planetesimals, even at low resolution, but A = 0.5 does not. The vertical line marks the time of the snapshot shown in Figure 5.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Number of grid cells per λ for our two resolutions, where λ is the wavelength of the fastest-growing mode of the SI (Equation (19)). The high-resolution run has just enough resolution to resolve the fastest-growing modes everywhere, despite the small particle size and low η inside the pressure bump. The low-resolution run does not adequately resolve the SI in the planetesimal formation region, as the number of cells per λ is < 1.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Gas pressure profile with and without a pressure bump. Our simulations have bump amplitudes of A = 0.5 (high-res and low-res, blue) and A = 0.6 (low-res, orange). For reference, we also show the pressure profile without a bump (gray) and with the smallest bump with a particle trap (﹩\max [{dP}/{dr}]\geqslant 0;﹩ green). Because the pressure bump is sitting on top of a background pressure gradient, the point of minimum headwind is offset from the center of the simulation box.
Paper: Tidal Disruption on Stellar-mass Black Holes in Active Galactic Nuclei
Authors: Y. Yang, I. Bartos, G. Fragione, Z. Haiman, M. Kowalski, S. Márka, R. Perna, H. Tagawa
Figure caption: Example evolution of orbital parameters. Evolution is shown as a function of time for the semimajor axis a (top), eccentricity e (middle), and inclination θ (angle between the semimajor axis and the AGN disk plane in degrees; bottom) for four sample orbits. Each example orbit begins with a = 0.02 pc and has the following initial parameters. Blue: e = 0.2, θ = 80°, ψ = 0°. Orange: e = 0.5, θ = 80°, ψ = 0°. Green: e = 0.2, θ = 70°, ψ = 0°. Red: e = 0.2, θ = 80°, ψ = 20°. Here, ψ is the initial angular rotation of the semiminor axis from the disk plane; see Yang et al. (2019b).