adsabs/AstroCLIMB huggingface dataset:
Paper: Constraints on Compact Dark Matter from Gravitational Wave Microlensing
Authors: S. Basak, A. Ganguly, K. Haris, S. Kapadia, A. K. Mehta, and P. Ajith
Figure caption: Redshift distribution of binary black hole mergers assumed predicted by different models—uniform distribution in comoving volume, population synthesis models predicted by Belczynski et al. (2016a, 2016b) and Dominik et al. (2013). We also show, in thin gray lines, several models of primordial black hole mergers given in Mandic et al. (2016). Since most of them are “bracketed” by the three models that we consider, we do not use them explicitly in the computation of upper limits.
Paper: Constraints on Compact Dark Matter from Gravitational Wave Microlensing
Authors: S. Basak, A. Ganguly, K. Haris, S. Kapadia, A. K. Mehta, and P. Ajith
Figure caption: Distribution of the simulated binaries (light gray), detected binaries (dark gray) and lensed binaries (black). The binaries are assumed to be distributed uniformly in comoving four-volume. The detector PSDs are from O3a.
Paper: Constraints on Compact Dark Matter from Gravitational Wave Microlensing
Authors: S. Basak, A. Ganguly, K. Haris, S. Kapadia, A. K. Mehta, and P. Ajith
Figure caption: Microlensing optical depth (solid lines) and lensing probability (dashed lines) as a function of the source redshift zS assuming different values of fDM (shown in legend).
Paper: Constraints on Compact Dark Matter from Gravitational Wave Microlensing
Authors: S. Basak, A. Ganguly, K. Haris, S. Kapadia, A. K. Mehta, and P. Ajith
Figure caption: The color bar shows the lensing time delay ﹩{\mathrm{log}}_{10}({\rm{\Delta }}{T}_{{\ell }}/{\rm{s}})﹩ as a function of the redshifted lens mass ﹩{{M}_{{\ell }}}^{z}﹩ and dimensionless impact parameter y. The black dots show the merger events for which ΔTℓ is less than the signal duration τ.
Paper: Constraints on Compact Dark Matter from Gravitational Wave Microlensing
Authors: S. Basak, A. Ganguly, K. Haris, S. Kapadia, A. K. Mehta, and P. Ajith
Figure caption: Scatter plot of BBH events in the source frame lens mass Mℓ and impact parameter plane for fDM = 1. The color bar shows the value of the ﹩\mathrm{ln}{{ \mathcal B }}_{{\rm\small{U}}}^{{\ell }}﹩. The simulation corresponds to a redshift distribution that is uniform in comoving four-volume.
Paper: Constraints on Compact Dark Matter from Gravitational Wave Microlensing
Authors: S. Basak, A. Ganguly, K. Haris, S. Kapadia, A. K. Mehta, and P. Ajith
Figure caption: The left panel shows the posterior distributions of redshifted lens mass ﹩{{M}_{{\ell }}}^{z}﹩ (violin plots) and the Bayesian likelihood ratio between lensed and unlensed hypotheses (top horizontal axis) obtained from the binary black hole signals observed during O1 and O2. None of the likelihood ratios are significant enough to favor the lensing hypothesis. The right panel shows the same estimated from a simulated lensed/unlensed binary black hole event with redshifted masses ﹩{m}_{1}^{z}=35.2{M}_{\odot },{m}_{2}^{z}=31.7{M}_{\odot }﹩ (broadly consistent with the GW150914 event) and S/N = 16.1. For the simulated lensed event, the lensing hypothesis is significantly preferred (﹩\mathrm{ln}{{ \mathcal B }}_{{\rm\small{U}}}^{{\ell }}=26.7﹩) and the posterior on lens mass is consistent with the injected value ﹩{{M}_{{\ell }}}^{z}={10}^{3.4}{M}_{\odot }﹩. For the simulated unlensed event, ﹩\mathrm{ln}{{ \mathcal B }}_{{\rm\small{U}}}^{{\ell }}=-0.2﹩ is consistent with the values derived from real events shown in the left panel (within noise induced fluctuations).
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Overview of the OMNI data and MMS2 measurements during 06:15:00–07:10:00 UT. (a) Three components of the interplanetary magnetic fields approximately shifted to the bow shock. (b)–(e) MMS2 observations in the magnetosheath: (b) three components of the magnetic field, (c) total magnetic field, and (d) ion and (e) electron differential energy fluxes. The GSE coordinate is employed.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: MMS2 observations between 06:34:00 and 06:37:00 UT. (a) Three components of the magnetic field, (b) total magnetic field, (c) electron density, (d) ion bulk velocities, (e) ion temperatures, (f) the parameter ﹩k=\tfrac{{T}_{i\perp }}{{{Ti}}_{\parallel }}-\left(1+\tfrac{1}{{\beta }_{\perp }}\right)﹩, which is critical to the ion-mirror instability, (g) current density estimated by the curlometer method (the quality factor for the MMS tetrahedron is 0.77), Jc = ∇ × B. (h) Sketch of the mirror-modulated reconnecting current sheet; the blue dashed lines are the unperturbed magnetic field, the magenta dashed line indicates the center of the current sheet, and the black solid lines represent the mirror-modulated magnetic field. (j) Sketch of two EDRs and electron flow vortices (red rings) within the IDR.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Two EDRs observed in an IDR by MMS2. (a) Three components of the magnetic field; (b) total magnetic field and electron density; (c) ion bulk velocities; (d) electron bulk velocities; (e) current densities calculated from plasma moments, Jp = en(vi − ve); (f)–(h) three components of the measured electric field (black), −vi × B (blue), −ve × B (red); (i) energy dissipation J · (E + ve × B); (j) electron nongyrotropy Q0.5. The two yellow dashed lines mark the two separatrices.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Oblique tearing instability and electron K-H instability in the current sheet. Left column: time-shifted observations of all four spacecraft (see Figure A5 in the Appendix for the original observations). (a) Total magnetic field, (b) electron number density, (c) electron perpendicular temperature, (d)–(f) three components of the current density, (g) total current density, and (h) L component of the electron bulk velocity and the half local electron Alfvén speed. Right column: measurements during 06:36:19.00–06:36:21.00 UT. (i) The current density in the L–M plane JLM (color dots); the magnetic field in the L–M plane BLM (blue and red arrows) on the two sides of the current sheet defines the unstable range of the tearing instability predicted by the theory (marked by the gray shaded area). (j) Electron flow vectors (with uniform background flow, VL = 50 km s−1, VN = −60 km s−1 removed) in the L–N plane. The location of MMS in the N direction is estimated according to the normal velocity of the current sheet (calculated by the timing method), with N = 0 corresponding to the normal position at the time when BL = 0.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Two EDRs in an IDR observed by MMS1. (a) Three components of the magnetic field; (b) total magnetic field and electron density; (c) ion bulk velocities; (d) electron bulk velocities; (e) current densities calculated from plasma moments, Jp = en(vi − ve); (f)–(h) three components of the measured electric field (black), −vi × B (blue), −ve × B (red); (i) energy dissipation J · (E + ve × B); and (j) electron nongyrotropy Q0.5. The two yellow dashed lines mark the two separatrices.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Two EDRs in an IDR observed by MMS3. (a) Three components of the magnetic field; (b) total magnetic field and electron density; (c) ion bulk velocities; (d) electron bulk velocities; (e) current densities calculated from plasma moments, Jp = en(vi − ve); (f)–(h) three components of the measured electric field (black), −vi × B (blue), −ve × B (red); (i) energy dissipation J · (E + ve × B); and (j) electron nongyrotropy Q0.5. The two yellow dashed lines mark the two separatrices.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Two EDRs in an IDR observed by MMS4. (a) Three components of the magnetic field; (b) total magnetic field and electron density; (c) ion bulk velocities; (d) electron bulk velocities; (e) current densities calculated from plasma moments, Jp = en(vi − ve); (f)–(h) three components of the measured electric field (black), −vi × B (blue), −ve × B (red); (i) energy dissipation J · (E + ve × B); and (j) electron nongyrotropy Q0.5. The two yellow dashed lines mark the two separatrices.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Schematic view of a deformed EDR. We consider two cases: (a) and (b) are for the EDR deformed in the L–N plane, while (c) and (d) are for the EDR deformed in the M–N plane. Panels (a) and (c) show the cartoon for a deformed EDR and the spacecraft trajectory across the EDR. Panels (b) and (d) display the profiles of BL and ﹩J\cdot {E}^{{\prime} }﹩ along the trajectory of the spacecraft as it crosses the EDR shown in (a) and (c), respectively. If the spacecraft crosses this deformed EDR oblique to N due to the background flow in L or M, it might cross the deformed EDR twice. In these cases, the spacecraft may record two peaks in ﹩J\cdot {E}^{{\prime} }﹩ similar to the MMS observation. However, the second crossing of the EDR must be manifested as a decrease of BL to zero, which is inconsistent with the nearly monotonic variation of BL as MMS crossed the current sheet. Therefore, we believe it is unlikely that the observation of the two EDRs is caused by a single deformed EDR.
Paper: Stacked Electron Diffusion Regions and Electron Kelvin–Helmholtz Vortices within the Ion Diffusion Region of Collisionless Magnetic Reconnection
Authors: Z. H. Zhong, M. Zhou, Yi-Hsin Liu, X. H. Deng, R. X. Tang, D. B. Graham, L. J. Song, H. Y. Man, Y. Pang, and Yu. V. Khotyaintsev
Figure caption: Four MMS spacecraft observations of the reconnecting current sheet without time shift. (a) Total magnetic field; (b) electron number density; (c) electron perpendicular temperature; (d)–(f) three components of the current density; (g) total current density; and (h) L component of the electron bulk velocity and the half local electron Alfvén speed.
Paper: The Stability of the Electron Strahl against the Oblique Fast-magnetosonic/Whistler Instability in the Inner Heliosphere
Authors: Seong-Yeop Jeong, Joel B. Abraham, Daniel Verscharen, Laura Berčič, David Stansby, Georgios Nicolaou, Christopher J. Owen, Robert T. Wicks, Andrew N. Fazakerley, Jeffersson A. Agudelo Rueda, and Mayur Bakrania
Figure caption: Radial profiles of T∥c, T∥s, B0, nc/ne, ns/ne, and vAe in our PSP and Helios data sets, separated between the low-β∥c and the high-β∥c regimes according to Equation (1).
Paper: The Stability of the Electron Strahl against the Oblique Fast-magnetosonic/Whistler Instability in the Inner Heliosphere
Authors: Seong-Yeop Jeong, Joel B. Abraham, Daniel Verscharen, Laura Berčič, David Stansby, Georgios Nicolaou, Christopher J. Owen, Robert T. Wicks, Andrew N. Fazakerley, Jeffersson A. Agudelo Rueda, and Mayur Bakrania
Figure caption: Profiles of the low-β∥c threshold of the oblique FM/W instability from Equation (2) and Us as functions of heliocentric distance. All PSP and Helios data underlying this figure have β∥c < 0.25.
Paper: The Stability of the Electron Strahl against the Oblique Fast-magnetosonic/Whistler Instability in the Inner Heliosphere
Authors: Seong-Yeop Jeong, Joel B. Abraham, Daniel Verscharen, Laura Berčič, David Stansby, Georgios Nicolaou, Christopher J. Owen, Robert T. Wicks, Andrew N. Fazakerley, Jeffersson A. Agudelo Rueda, and Mayur Bakrania
Figure caption: Profiles of the high-β∥c threshold of the oblique FM/W instability from Equation (3) and Us as functions of heliocentric distance. All PSP and Helios data underlying this figure have β∥c > 0.25.
Paper: A Rapid Ionization Change in the Nebular-phase Spectra of the Type Ia SN 2011fe
Authors: M. A. Tucker, C. Ashall, B. J. Shappee, C. S. Kochanek, K. Z. Stanek, and P. Garnavich
Figure caption: Flux-calibrated spectroscopic evolution of SN 2011fe at >200 days after maximum light. Error bars along the right axis represent typical flux-calibration uncertainties after the BVR spline fits (see Section 2). The gray hatched region marks the O2 A-band telluric feature. The new LBT MODS spectra are provided as data behind the figure.(The data used to create this figure are available.)
Paper: A Rapid Ionization Change in the Nebular-phase Spectra of the Type Ia SN 2011fe
Authors: M. A. Tucker, C. Ashall, B. J. Shappee, C. S. Kochanek, K. Z. Stanek, and P. Garnavich
Figure caption: Spectroscopic comparison at various epochs using the same color scheme as Figure 1 but normalized by the mean flux near 5300 Å. Dominant line identifications before and after the distinct ionization transition at ∼500 days are given in black and gray, respectively. Lines with a “?” indicate that the line’s contribution to the observed spectral feature is unclear. Fe emission lines after the ionization transition are likely blends of forbidden and permitted transitions (Fransson & Jerkstrand 2015), but we omit the bracket notation for visual clarity.
Paper: A Rapid Ionization Change in the Nebular-phase Spectra of the Type Ia SN 2011fe
Authors: M. A. Tucker, C. Ashall, B. J. Shappee, C. S. Kochanek, K. Z. Stanek, and P. Garnavich
Figure caption: Temporal evolution of the 7300 Å feature, transitioning from [Fe II]+[Ni II] to [Ca II] around ∼480 days after ﹩{t}_{\max }﹩ (see Section 3.2).
Paper: A Rapid Ionization Change in the Nebular-phase Spectra of the Type Ia SN 2011fe
Authors: M. A. Tucker, C. Ashall, B. J. Shappee, C. S. Kochanek, K. Z. Stanek, and P. Garnavich
Figure caption: Velocity evolution of the continuum-subtracted [Ca II] profile at >450 days (black) compared to the theoretical 1000 day nebular spectra computed by Fransson & Jerkstrand (2015) using density profiles from the W7 deflagration model (green; Iwamoto et al. 1999) and the N100 delayed-detonation model (blue; Seitenzahl et al. 2013a). The thin red lines are the line profile reflected across the line center to highlight the profile symmetry.
Paper: A Rapid Ionization Change in the Nebular-phase Spectra of the Type Ia SN 2011fe
Authors: M. A. Tucker, C. Ashall, B. J. Shappee, C. S. Kochanek, K. Z. Stanek, and P. Garnavich
Figure caption: Evolution of the average flux for the Fe-dominated 4000–5500 Å region (dotted blue) compared to the feature at ≈7300 Å (dashed red).
Paper: A Rapid Ionization Change in the Nebular-phase Spectra of the Type Ia SN 2011fe
Authors: M. A. Tucker, C. Ashall, B. J. Shappee, C. S. Kochanek, K. Z. Stanek, and P. Garnavich
Figure caption: Nondetections of Hα (inverted triangles) compared to the models of Dessart et al. (2020, dotted lines, ﹩100\,\mathrm{days}\lesssim {t}_{\max }\lesssim 300\,\mathrm{days}﹩) and Botyánszki et al. (2018, dashed lines, ﹩200\,\mathrm{days}\lesssim {t}_{\max }\lesssim 500\,\mathrm{days}﹩) for ablated masses of (10−1, 10−2, 10−3) M⊙, from top to bottom. Flux limits for Hα, He Iλ5876, and [O I]λ6300 are provided as data behind the figure.(The data used to create this figure are available.)
Paper: The Ultramassive White Dwarfs of the Alpha Persei Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, and Pier-Emmanuel Tremblay
Figure caption: The candidate white dwarf escapees and members from the Alpha Persei cluster. The effects of extinction have been removed using the mean value of AV from the Gentile Fusillo et al. (2021) catalog. The five white dwarfs that are both more massive than 0.85 M⊙ and younger than 250 Myr (according to Gaia EDR3 data) are indicated in the cutout. Contours of constant mass run from the top left to the bottom right with 0.4 M⊙ at the top and increasing in increments of 0.1 M⊙–1.2 M⊙. Contours of constant age run from the bottom left toward the top right with 50 Myr, 100 Myr, 250 Myr, 500 Myr, 1 Gyr, 2.5 Gyr, and 5 Gyr from top to bottom. A reddening of E(B − V) = 0.1 corresponds to E(Bp − Rp) = 0.15, so the positions of the stars in this diagram depend sensitively on the assumed reddening; the masses inferred from photometry alone are likely to be imprecise.
Paper: The Ultramassive White Dwarfs of the Alpha Persei Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, and Pier-Emmanuel Tremblay
Figure caption: Left to right: Balmer series from Hα to Hϵ (bottom to top) for WD1 (GMOS on Gemini-North), and Hβ (bottom) to Hϵ (top) for WD2 (GMOS on Gemini-North), WD3 and WD4 (Palomar DBSP), and WD5 (Keck LRIS) with the best-fitting hydrogen atmosphere models superimposed.
Paper: The Ultramassive White Dwarfs of the Alpha Persei Cluster
Authors: David R. Miller, Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, and Pier-Emmanuel Tremblay
Figure caption: Initial–final mass relation for white dwarfs. The ONe-model masses are plotted from Table 2. Those labeled “Pleiades” are from Heyl et al. (2021a), those from “Various” clusters are from Richer et al. (2021), and the remainder are from Cummings et al. (2018). The black line and blue region denote the empirical initial–final mass relation from El-Badry et al. (2018) (up to 8 M⊙) and its uncertainty bounds.
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: Schematic diagram of a protoplanetary disk and the wind mechanisms examined in this work. We consider only three channels (mass accretion, inner magnetic winds, and outer thermal winds) for disk accretion and dispersal; internal photoevaporation can be prevented due to the inner (massive) winds. The inner magnetic winds should be radially extended to reproduce the observed accretion rate.
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: The maximum value of the ratio between external photoevaporative mass loss rates and stellar accretion rates. The FRIED grid is used to estimate the mass loss rate, and the observed correlation is used to convert the disk mass to the stellar accretion rate. The ratio is an increasing function of disk radius and external far-UV radiation. The black solid line defines the region where the ratio becomes larger than unity; below the line, disks are considered to have been already truncated by external photoevaporation.
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: The ratio of the wind mass loss rate to the stellar accretion rate as a function of the external UV flux (also see Table 1 and Figure 2). The MCW case is denoted by the red shaded region, the MRI case the purple shaded region, and the EPE case the blue shaded region. For the EPE case, the disk radius dependence is explicitly denoted by the lines. The parameter space that is not covered by the current FRIED grid is denoted by the light blue shaded regions. Two inner magnetic winds can be differentiated by measuring the resulting mass loss rate, and the outer thermal winds and the resulting mass loss rate can be constrained by observing the disk radius.
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: The distribution of the data currently available in the literature and the fractional population in the left and right panels, respectively. The observed systems are summarized in Tables 4 and 5 (denoted by the green and blue points, respectively), and the error estimation is described in Appendices D and E. The current, large uncertainties prevent one from determining the dominant accretion and dispersal mechanisms, while the data already show some structure, distributed mainly in the MRI and EPE regions.
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: Disk populations for inner magnetic winds. The populations are generated by the Monte-Carlo approach (Table 2). In Case 1, only the values of rA/r and ϵ vary. In Cases 2 and 2a, those of rin and rout change in addition to the values of rA/r and ϵ. In Cases 3 and 3a, the effect of variation of h0 is examined. In Case 4, all the parameters are altered. The variation of parameters leads to two overlapping populations (i.e., MCW and MRI). However, the overlap can be disentangled, by observing a sufficient number of disks.
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: Disk populations for outer thermal winds. The populations are generated by the Monte-Carlo method (Table 3). The top panel shows the results for the case that Ms = 0.5 M⊙, the middle one is for the case that Ms = 1 M⊙, and the bottom is for the case that Ms = 1.6 M⊙. In the left panel, the disk populations are distributed in the ﹩{\dot{M}}_{\mathrm{loss}}/{\dot{M}}_{\mathrm{acc}}\mbox{--}{F}_{\mathrm{FUV}}﹩ diagram. Both rd and Md vary in all the plots; compared with the left plot, the ranges of rd and Md shrink on the central and right plots, respectively. In the right panel, the fractional populations are shown, in order to examine the effect of the range of model parameters. As expected, the resulting disk populations are most sensitive to the disk radius. The blue shaded region is a good representative of disk populations for wide ranges of rd and Md.