adsabs/AstroCLIMB huggingface dataset:
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Model uncertainty of the GRMHD score-based prior. We trained a prior on the full GRMHD training data set (“Full”) and two priors (“Subset 1” and “Subset 2”) on two disjoint subsets of the GRMHD training data set. We obtained posterior samples under these three realizations of a GRMHD prior given synthetic observations of the four ringlike test images. Panel (a) shows the posterior means and pixel-wise standard deviations. The visual statistics of the three priors are similar. However, as the GRMHD 2 posterior under Subset 2 demonstrates, due to randomness in training, the resulting score-based prior may not always impose certain features so strongly. In this case, the Subset 2 prior results in some off-center rings when reconstructing the GRMHD 2 image. Panel (b) shows extracted ring features, comparing to the ground truth as shown in Figure 11. Consistent with the results for the 64 × 64 GRMHD prior in Figure 11, these realizations of a 32 × 32 GRMHD prior tend to slightly overestimate the diameter. However, among the different realizations of the prior, the extracted ring features are fairly consistent. The feature most sensitive to model uncertainty of the prior is fractional central brightness.
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Ablation of data annealing and flux constraint. The simulated measurements are of the Crescent image in Figure 3. The posterior samples are shown with their original number of pixels (i.e., 32 × 32 or 64 × 64) and with their original pixel values (which should be between 0 and 1). “None” is vanilla optimization without data-weight annealing or a flux constraint objective. Without a flux constraint, the total flux V( x ) of samples varies widely; furthermore, a posterior that is unconstrained in the total flux may be too complicated to model with VI. Without data annealing, optimization may become unstable, as is the case for the GRMHD prior here. Optimization is generally more stable when both data annealing and a flux constraint are used.
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Visualization of extracted ring features of M87* images. Shown is a random sample (centered by REx) from each posterior for April 6. Parameter d is the ring diameter; w is the ring width. Parameters r left and r right delimit the radial FWHM used to estimate the orientation angle and asymmetry. Parameter η is the orientation angle measured east of north. The purple cross marks the location of peak brightness. Asymmetry A and fractional central brightness f  C  are not visualized. The green dashed circle demarcates the inner disk of radius 5 μas used to define f  C .
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Extracted ring features of M87* images. The means and error bars were computed the same way as for Figure 11. The different priors (CIFAR, GRMHD, RIAF, CelebA) all agree on the diameter, orientation, and asymmetry up to error bars. There is some disagreement in asymmetry for April 10, which is the day with fewest observations. We note a slight upward trend in diameter and orientation angle over the observation days. The width and fractional central brightness change with the prior, with the GRMHD prior providing the thinnest rings and most brightness contrast. Please see Figure 7 for image samples.
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Bimodal M87* image posteriors under the CelebA prior. A two-component Gaussian mixture model was fit to 128 posterior samples for April 5, 6, and 10. The mean, std. dev., and weight of each Gaussian mixture component are shown. The only single-mode posterior is for April 11, which is the day with the most (u,v) coverage.
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Mean and std. dev. of posterior samples. Like with the simulated data in Figure 4, uncertainty decreases as the prior becomes stronger. Note that under the CIFAR-10 prior the day with the most uncertainty is April 10, the day with the least data. The stronger priors (i.e., GRMHD and RIAF) do not exhibit more uncertainty for this day compared to other days.
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Effect of target flux ﹩\bar{V}﹩. The simulated measurements are of the Crescent image in Figure 3, and the prior is the CelebA score-based prior. ﹩\bar{V}=112﹩ is the default target total flux chosen based on samples from the prior. When ﹩\bar{V}﹩ is halved to 56, the estimated posterior images are sparser. When ﹩\bar{V}﹩ is doubled to 224, the estimated posterior images have less compactness. ﹩\bar{V}=112﹩ is essentially the preferred total flux under the score-based prior.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: SED of HAWC J2031+415. The other observations are from F. Aharonian et al. (2005), J. Albert et al. (2008), and A. U. Abeysekara et al. (2018b, 2018a), respectively, and were selected as the most current independent observations available. Additionally, all uncertainties are statistical only.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: The longitudinal profiles for the excess count maps for HAWC J2031+415. The red fitted lines correspond to the fitted Gaussians of each band while the blue dashed lines are the simulated PS Gaussians discussed in Section 4. The location of PSR J2032+4127 is indicated by the vertical line. The distance between HAWC J2031+415's best-fit centroid location and the pulsar’s location is 0.°13 or about 3 pc.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: Left: the full multiwavelength fit results. The different SYN fit bands indicate the expected X-ray and radio fluxes for different magnetic fields from the IC fit using HAWC data. The 1.48 μG fit indicated by the thicker dashed line is the best-fit magnetic field using the Suzaku spectrum. Additionally, the IC HAWC data fit is broken into CMB, FIR, and NIR components. Right: zoomed-in TeV fit results. All three TeV models fit the data well, though it is clear that lower energy data are needed to properly constrain the PD model index.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: Left: a significance map of the ROI (green contour) with the source associations found in Section 3. A mask is placed on 3HWC J2019+367 to avoid contamination from its emission for this analysis. Right: HAWC J2031+415's emission is shown after contributions from HAWC J2030+409 and 3HWC J2020+403 were subtracted from the data map.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: 172 days of HAWC data from 2017 May 26 to November 14. The maximum significance is located near HAWC J2031+415 and is 6.10σ for this interval.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: The significance map used for the energy morphology study. The rectangle highlights the longitudinal profile region used for the energy-dependent morphology study.
Paper: Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415
Authors: R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, A. Sandoval, D. Salazar-Gallegos, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, L. Villaseñor, X. Wang, Zhen Wang, I. J. Watson, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: The results from the energy morphology study as described in Section 4. HAWC J2031+415's true size is presented on the y-axis and the distance to the pulsar is on the x-axis.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Radial dependence of the mass accretion rate (solid lines) and the mass wind rate (dashed lines) for Models I–III, as obtained using Equations (20) and (21), respectively. Panels (a)–(d) show the results at t/τ 0 = 0.01, t/τ 0 = 0.1, t/τ 0 = 1.0, and t/τ 0 = 30, respectively. The mass accretion rate is represented by black solid lines and the mass wind rate by blue dashed lines, with both rates normalized by the Eddington accretion rate. Different line styles indicate different models. Note that there is no blue line for Model I, as there is no wind present for ϵ rad = 1.0.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Time evolution of the mass accretion rates estimated at the disk’s inner radius for all models, along with the corresponding slopes. In panel (a), the mass accretion rate is normalized by the Eddington accretion rate. Different line colors represent different models. In panel (b), the slope is represented by the power-law index of time. The gray solid and dashed lines correspond to −5/3 (mass fallback rate case; G. Lodato et al. 2009) and −19/16 (classical solution case; J. K. Cannizzo et al. 1990), respectively. The inset displays the slope at early times.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Time evolution of the disk luminosities of the three spectral bands and the bolometric luminosities for Models I–IV. Panels (a), (b), (c), and (d) show bolometric and three luminosities (X-ray, UV, and optical). Different colors indicate different models in all the panels.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: The same format as Figure 4, but for Models III and IV.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Radial profiles of C  w,0, obtained using Equation (15), for Models II–IV at different time epochs. Panels (a)–(d) show profiles at t/τ 0 = 0.01, t/τ 0 = 0.1, t/τ 0 = 1.0, and t/τ 0 = 30, respectively, displayed chronologically. In each panel, different colors represent different models. The black dashed line indicates the ﹩{C}_{w,\mathrm{sim}}=2\times {10}^{-5}﹩ line, obtained from simulations (T. K. Suzuki et al. 2016), which serves as the fiducial value.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Time evolution of the disk mass and angular momentum for Models I–IV. The different colors represent the different models. The disk mass is normalized by the mass of the bound debris, given by M 0 = M ⋆/2 ∼ 1.0 × 1033 g(M ⋆/M ⊙). The normalization of the disk angular momentum is determined by the angular momentum of the bound debris, ﹩{J}_{0}={M}_{0}\sqrt{2{{GMr}}_{t}}\sim 4.3\times {10}^{55}\,{\rm{g}}\,{\mathrm{cm}}^{2}\,{{\rm{s}}}^{-1}﹩.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption:  ϵ rad-dependent mass-loss rates at the three different times for ﹩{\bar{\alpha }}_{z\phi }=0﹩. Different colors indicate those different times. The mass-loss rates are normalized by the Eddington accretion rate, ﹩{\dot{M}}_{\mathrm{Edd}}﹩. The filled circle represents each data point in every ϵ rad = 0.1 step.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Frequency distributions of the spectral luminosities (see Equation (29)) for Models I–IV. Different models are represented in different colors. Panels (a), (b), and (c) display the t/τ 0 = 0.01 case, the t/τ 0 = 0.1 case, and the t/τ 0 = 1.0 case, respectively.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Same format as Figure 7, but for the mass-loss rates for Models II–IV. Note that there is no mass loss in Model I.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption:  ϵ rad dependence of the slopes of mass accretion and mass-loss rates for ﹩{\bar{\alpha }}_{z\phi }=0﹩. For all the cases, n, n  w , and n  l  are evaluated at t/τ 0 = 30 and are denoted by blue, red, and black solid lines, respectively. Each data point in every ϵ rad = 0.1 step is indicated by the filled square. The horizontal black dashed line indicates the no-wind case (n = −19/16) as a fiducial value (J. K. Cannizzo et al. 1990).
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Time evolution of the mass accretion rate estimated at the ISCO radius and the mass-loss rate for the case of M  i  = 0.005 M ⊙. Panels (a) and (b) represent the mass accretion rate curve and the mass-loss rate curve for all four models, respectively. The different colored lines indicate different models. The Eddington accretion rate normalizes both the mass accretion and mass-loss rates. The insets of panels (a) and (b) display the mass accretion and mass-loss rates for the M  i  = 0.5 M ⊙ case, respectively.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Radial profiles of the mass accretion rates, which are obtained by Equation (20), at a near initial time t/τ 0 = 0.001. Panels (a)–(d) represent those of Models I–IV. For all panels, the blue and red solid lines correspond to an initial disk mass of M  i  = 0.5 and 0.005 M ⊙, respectively. The mass accretion and mass-loss rates are normalized by the Eddington accretion rate.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Radial profile of the ratio of radiation to gas pressure for Models I–IV at a near-initial time t/τ 0 =  0.001. Panels (a) and (b) correspond to an initial disk mass of M  i  = 0.5 and 0.005 M ⊙, respectively. In both panels, the different colored lines indicate different models.