adsabs/AstroCLIMB huggingface dataset:
Paper: First Detection of Ices in Intermediate-mass Young Stellar Objects beyond the Milky Way
Authors: Guido De Marchi, Nolan Habel, Margaret Meixner, Katia Biazzo, Giovanna Giardino, Elena Sabbi, Ciaran Rogers, Jeroen Jaspers, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Katja Fahrion, Alec S. Hirschauer, Charles D. Keyes, David R. Soderblom, Laura Lenkić, Omnarayani Nayak, Bernhard Brandl
Figure caption: (a) CO2 vs. H2O ice column densities for the stars in NGC 346 (black dots) compared with those measured for massive stars (>8 M⊙) in the SMC (blue squares), in the LMC (red circles), and in the MW (large green triangles) as well as for low-mass Galactic YSOs (small purple triangles). The solid line is the best fit to the NGC 346 column densities and corresponds to a proportionality ratio of 0.18  ±  0.06. The dashed line is the best fit to the ice column densities measured toward high-mass MW YSOs and corresponds to a proportionality ratio of 0.21  ±  0.08. (b) Histograms showing the distribution of N(CO2)/N(H2O) ice column density ratios in NGC 346 (black line, gray shading), compared to the same in LMC massive protostars (red), in MW massive protostars (green), and in low-mass Galactic protostars (purple). (c) and (d) The same as panel (a) but for N(CO) vs. N(H2O) and N(CO) vs. N(CO2), respectively. The corresponding ratios, indicated by the solid lines, are 0.08  ±  0.02 and 0.52  ±  0.16, respectively. The dotted–dashed lines show the mean ratios for the high-mass LMC stars alone. Downward arrows are upper limits from the literature.
Paper: First Detection of Ices in Intermediate-mass Young Stellar Objects beyond the Milky Way
Authors: Guido De Marchi, Nolan Habel, Margaret Meixner, Katia Biazzo, Giovanna Giardino, Elena Sabbi, Ciaran Rogers, Jeroen Jaspers, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Katja Fahrion, Alec S. Hirschauer, Charles D. Keyes, David R. Soderblom, Laura Lenkić, Omnarayani Nayak, Bernhard Brandl
Figure caption: Optical depth spectra of the YSOs in our sample, shifted vertically for clarity. For illustration purposes, the red lines correspond to a linear combination of four ice mixtures selected from LIDA (3000 monolayers of pure H2O at a temperature of 15 K, H2O:CO2 in the ratio 10:1 at 10 K, CO:CO2 in the ratio 2:1 at 15 K, and pure OCS at 17 K) and provide a reasonable fit to the observations. The corresponding column densities are listed in Table 4. The legend at the top of each panel indicates the ice features discussed in the text and the corresponding wavelengths, to guide the eye.
Paper: First Detection of Ices in Intermediate-mass Young Stellar Objects beyond the Milky Way
Authors: Guido De Marchi, Nolan Habel, Margaret Meixner, Katia Biazzo, Giovanna Giardino, Elena Sabbi, Ciaran Rogers, Jeroen Jaspers, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Katja Fahrion, Alec S. Hirschauer, Charles D. Keyes, David R. Soderblom, Laura Lenkić, Omnarayani Nayak, Bernhard Brandl
Figure caption: Best fit to the SEDs of the observed source, obtained using the models by T. P. Robitaille et al. (2006) and T. P. Robitaille (2017). Black lines correspond to the best-fit YSO model, while gray lines indicate fits with slightly larger χ2 but still within 10% of the best fit (see T. P. Robitaille 2017 for more details). The best-fitting parameters are shown in Tables 1 and 2.
Paper: First Detection of Ices in Intermediate-mass Young Stellar Objects beyond the Milky Way
Authors: Guido De Marchi, Nolan Habel, Margaret Meixner, Katia Biazzo, Giovanna Giardino, Elena Sabbi, Ciaran Rogers, Jeroen Jaspers, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Katja Fahrion, Alec S. Hirschauer, Charles D. Keyes, David R. Soderblom, Laura Lenkić, Omnarayani Nayak, Bernhard Brandl
Figure caption: Optical depth spectrum of source 90108 before (dashed line) and after (solid line) subtraction of the Hu 11–6 recombination line. Vertical thin dashed lines mark the location of other hydrogen recombination lines and molecular hydrogen excitation lines, as indicated. Dotted lines show the column density integration range.
Paper: First Detection of Ices in Intermediate-mass Young Stellar Objects beyond the Milky Way
Authors: Guido De Marchi, Nolan Habel, Margaret Meixner, Katia Biazzo, Giovanna Giardino, Elena Sabbi, Ciaran Rogers, Jeroen Jaspers, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Katja Fahrion, Alec S. Hirschauer, Charles D. Keyes, David R. Soderblom, Laura Lenkić, Omnarayani Nayak, Bernhard Brandl
Figure caption: Observed spectra and fitted continua.
Paper: Mitigating Eddington and Malmquist Biases in Latent-inclination Inference of the Tully–Fisher Relation
Authors: Hai Fu
Figure caption: MCMC-sampled posterior PDFs from the dual-scatter model (green) compared to those from the forward model (blue) and the inverse model (red). The data are from sample C, whose input parameters are indicated by black dashed lines and black crosses. The dual-scatter model produces relatively unbiased inferences for all parameters, gives more realistic statistical uncertainties, and reveals parameter degeneracies. For example, the two σ’s are tightly correlated on an ellipse: ﹩{\sigma }_{m}^{2}+{\beta }^{2}{\sigma }_{w}^{2}={\sigma }_{t}^{2}﹩, as indicated by the dotted curve in the panel.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) The rms amplitude as a function of the spherical harmonic degree. The formal uncertainties of MTW120 model are denoted as an orange dashed line, and the coefficient differences between MRO120D and MTW120 models are denoted as a blue dashed line. (b) The relative errors of the coefficient differences to the MTW120 model coefficients as a function of the spherical harmonic degree.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The rms amplitude as a function of the spherical harmonic degree of two gravity field models. The gravity field coefficients are denoted by a green (MRO120D model), red (MRO120F model), and orange (MTW120 model) solid line, and the formal uncertainties of the gravity field coefficients are denoted by dashed line.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) Gravity anomalies of the MTW120 gravity field model defined in accordance with A. S. Konopliv et al. (2016). (b) Differences between MTW120 and MRO120D gravity field models. The minimum, maximum, and rms value of the differences were −4.36, 4.53, and 0.5 mGal. The gravity anomalies were generated using shtools (M. A. Wieczorek & M. Meschede 2018). Maps are plotted in Hammer projection.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The periapsis ground track distribution of Tianwen-1 in Hammer projection over the period from 2021 June to 2024 October. The periapsis altitude is around 265 km.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: (a) Gravity anomaly errors from the full covariance matrix for the MTW120 model. The minimum, maximum, and rms value of the differences were 7.457, 32.886, and 25.08 mGal, respectively. (b) The differences in gravity anomaly errors between MRO120D and MTW120 gravity field models. Maps are plotted in Hammer projection.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The rms of Tianwen-1 Doppler tracking data postfit residual for 1-data arcs of the Tianwen-1 orbiter data using two gravity field models. The red “diamond” line denotes the MRO120D model, and the blue “circle” line denotes the MTW120 model.
Paper: Evaluating the Contributions of Tianwen-1 Orbiter Tracking Data to the Mars Gravity Field Modeling
Authors: Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Wanling Yang, Jianfeng Cao, Denggao Qiu, Xie Li, Jean-Pierre Barriot
Figure caption: The rms of orbit overlap differences in the radial (a), along-track (b), and cross-track (c) directions and in total position (d) for the 12 hr orbit prediction from 1 day data arcs using two gravity field models.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: Savage–Dickey BFs in support for a CGW at each GW frequency. The orange curve indicates results for the case where common red noise (CRN) is not included in the analysis, while the black curve is for the case where it is included. We found that no CGWs are detected in the PPTA DR3 if a CRN is accounted for. The black and gray vertical dashed lines mark, respectively, the frequency of 1 yr−1 and of 1/Tobs. These two vertical lines retain the same meaning in all subsequent figures of this paper.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: All-sky 95% credibility upper limits on the CGW strain amplitude h0. The PPTA DR3 (black) is more sensitive than the DR1 (blue) by at least a factor of 4 over a wide frequency range. For comparison, the most recent strain upper limits from the EPTA, NANOGrav, and IPTA are also included in the figure.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: BF for comparison between different models, where numerical values represent the extent to which the data favors the model to which the arrow points. CGW here refers to a continuous wave signal with frequencies between 1 and 2.5 nHz, the frequency range where the BF peaks in Figure 1.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: The values of the all-sky CGW frequentist detection statistic ﹩{{ \mathcal F }}_{\,\rm{p}\,}﹩ and the respective FAP are shown against GW frequency.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: The values of the CGW detection statistic ﹩{{ \mathcal F }}_{\,\rm{e}\,}﹩, maximized over a range of 192 uniformly distributed sky positions for every GW frequency.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: Sky map of 95% credibility upper limits on the CGW signal amplitude h0 at 6 nHz for the PPTA DR3. Pulsars are marked as white stars, while the black plus sign indicates the most sensitive sky location.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: Horizon luminosity distance, dL, obtained from the sky-averaged 95% upper limit on strain amplitude h0 shown in Figure 5. The luminosity distance limit is calculated with Equation (11) for three chirp masses: 108M⊙, 109M⊙, and 1010M⊙.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: Sky map of the 95% lower limit on the luminosity distance to individual SMBBHs with ﹩{ \mathcal M }=1{0}^{9}{M}_{\odot }﹩ and fGW = 22 nHz. White diamonds indicate the positions of known SMBBH candidates or galaxy clusters that could host an SMBBH.
Paper: Searching for Continuous Gravitational Waves in the Parkes Pulsar Timing Array Data Release 3
Authors: Shi-Yi Zhao, Zu-Cheng Chen, Jacob Cardinal Tremblay, Boris Goncharov, Xing-Jiang Zhu, N. D. Ramesh Bhat, Małgorzata Curyło, Shi Dai, Valentina Di Marco, Hao Ding, George Hobbs, Agastya Kapur, Wenhua Ling, Tao Liu, Rami Mandow, Saurav Mishra, Daniel J. Reardon, Christopher J Russell, Ryan M. Shannon, Shuangqiang Wang, Lei Zhang, Andrew Zic
Figure caption: Upper limit on the number density (nUL) of SMBBHs in the local Universe as a function of GW frequency. Different curves correspond to binaries with different chirp masses. The density is measured in terms of comoving volume.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: 2D dynamical structures of the inner region at t = 365 yr, in the FidNoH run. (a) Gas density normalized by the initial midplane density with the surfaces of τr,xuv = 1 (purple dotted line), τr,irr = 1 (blue dotted−dashed line), τθ,disk = 1 (red dashed line), and the disk region z = 5Hmid (white dashed line). Thin lines threading to the disk show the poloidal magnetic field. (b) Mach number of the radial gas velocity, with the poloidal field line. The white solid line represents the location where the poloidal speed ∣vpol∣ reaches the poloidal Alfvén velocity (Alfvén surface). The arrows show the poloidal velocity direction (black: subsonic; white: supersonic). (c) Toroidal magnetic field normalized by the initial magnetic field strength at the midplane, with the poloidal field line. Green contour lines correspond to the plasma beta β = 1 (thin) and 10 (thick). (d) Ambipolar Elsässer number Am, with the poloidal field line. The white contours show the level of 0.1 (dashed), 1 (solid), and 10 (dotted). (e) Gas temperature, with the same optical depth and height lines as in panel (a). The snow surface (T = 170 K) is shown with the cyan line. (f) Joule heating rate, with the poloidal field lines.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Vertical profiles of the temperature (left), heating rate per unit volume (middle), and current density (right) at r = 1 au and t = 365 yr, for FidNoH (top panels) and FidH+ (bottom panels). Left: simulation gas temperature (black solid line; among which the contribution from reemission is shown by the blue dashed–dotted line), and expected temperatures due to Joule heating only (purple dashed line), due to irradiation only under the Static model (gray solid line), and under the simulation density and heating rate profiles (red dashed line). Middle: Joule heating rate (qJoule; blue line) and irradiation heating rate (qirr; orange line) are shown. The gray shaded region is optically thick for disk radiation. Vertical yellow lines indicate the location of τr,irr = 1. Right: magnitude of the current density (black line) and the components due to global field structure (colored lines; see Section 2.4.3), where negative values are shown by dotted lines.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Radial distributions of the time-averaged mass accretion rate (﹩\left\langle {\dot{M}}_{{\rm{acc}}}\right\rangle ﹩; black thick line) and cumulative mass-loss rate (﹩{\dot{M}}_{{\rm{loss}}}﹩; gray thin line) for the runs of FidNoH (left), FidH+ (middle), and FidH− (right). The accretion rates predicted from the wind stress Tϕθ only (orange dashed–dotted line) and from both Trϕ and Tϕθ (red dashed line; see Equation (29)) are shown. The local mass-loss rates (﹩{d}{\dot{M}}_{{\rm{loss}}}/{d}\mathrm{ln}r﹩; Equation (35)) of the top and bottom surfaces are, respectively, shown with blue and yellow lines, with negative values indicated by dotted lines. The accretion rate and local mass-loss rate are smoothed. The shaded region represents the buffer zone (see Section 2.3).
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Radial distributions of the time-averaged energy change rates normalized by the energy gain in the total energy equation (Γacc + Γrad; Equation (36)) with smoothing: the loss of the total energy (Λwind + Λrad; gray thick line; Equation (36)), loss of mechanical energy (Λwind,mech + ΓJoule; dashed light-blue line; Equation (49)), gain of mechanical energy (Γacc − Qcomp; red line; Equation (49)), release by the disk accretion (Γacc; yellow line; Equation (39)), loss by the disk wind (Λwind; dashed dark-blue line; Equation (37)), dissipation by Joule heating (ΓJoule; black line; Equation (47)), and net radiative cooling (Λrad − Γrad; gray thin line; Equation (40)).
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Radial distributions of the time-averaged midplane temperature: the simulation temperature (black line), expected temperature solely due to the Joule heating rate that is calculated from the simulation (TJoule; purple dashed line), the viscous disk model (Tvis; Equation (60); orange dashed line), and the Static model (gray solid line; see Section 2.4.5).
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Snapshots of the physical structures on the southern disk surface at t = 306, 313, 318, and 328 yr (top to bottom rows) in the FidH+ run. Left maps: density with velocity vectors (color: vertical mass flux) and poloidal magnetic fields (thin lines). Orange lines indicate the current layer where the toroidal field flips. Crosses mark the locations of magnetic islands, which are the centers of looped poloidal fields. Middle maps: temperature scaled by r1/2, with lines of τr,xuv = 1 (dotted) and τr,irr = 1 (dashed–dotted). Right maps: toroidal magnetic fields with Am contours (Am = 0.1 [red dotted], 1 [red solid], 10 [red dashed]), and the same lines as in the middle panels. Rightmost panels: forces along the poloidal fields (i.e., a positive force helps launch the outflow) originating from 5 au (indicated in all other panels). The forces present the sum of gravitational and centrifugal forces (gray), the pressure gradient force (blue), and the Lorentz force (red), each normalized by the gravitational force.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Schematic illustration of the mechanism for forming a low-density wind when the Hall effect is active, especially for the positive polarity. Left: without the Hall effect, the current layer, where Bϕ reverses, is located in the gas-pressure-dominated region, and the wind is typically launched above this layer near where β ∼ 1. Right: with the Hall effect, the current layer is pushed to a higher altitude than the β ∼ 1 surface. The Lorentz force dominates over the pressure gradient force and draws the gas into the current layer, creating a downward flow in the surface. As a result, the wind base is shifted to even higher altitudes and thus has much lower density.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Ratio of the total irradiation heating rate in the simulation to that in the Static model, firr, after the time average. All the runs in this paper are shown: FidNoH (top left), FidH+ (top middle), FidH− (top right), OpNoH (bottom left), OpH+ (bottom middle), and OpH− (bottom right). Dashed lines represent the energy rate ratio based on the two-layer model with the absorption surface of τr,irr = 1 (see Section 4.1 and Appendix E).
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Time-averaged midplane temperature profiles with κirr = 10 cm2 g−1: OpNoH (left), OpH+ (middle), and OpH− (right). For comparison, the models with κirr = 1 cm2 g−1 are shown as colored dashed lines and the Static model as thin gray lines.