adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Comparison of the preferred multicomponent ice model from Section 3.3 with a model in which CO and CO2 are not trapped interior to their sublimation fronts. The “no entrapment” model contains CO2:CO and pure CO in zone 3, along with pure CO2 in zones 2–3 and pure H2O in zones 1–3. Ice abundances for each model are listed in Table 5 with the model names in parentheses.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: The 13CO2 ice band observed with JWST (gray) and simulated (colors). The 13CO2 abundances in the simulations are determined by scaling down the CO2 abundance from the pure ice model (S1) by the factors indicated.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Lab-measured absorbance spectra of different H2O, CO2, and CO ice mixtures, normalized to show differences in the band profiles. Polar mixtures are shown in the top row, and apolar mixtures in the bottom row. See Table 3 for more details on the mixing ratios.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Absorption and scattering opacities for the small- and large-grain populations within each of the four disk zones. Model M1 is used for illustration (Table 5).
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Normalized C IV line profiles in the VLT-UVES spectra plotted on a velocity scale relative to the quasar redshift z = 2.217. The spectra are shown in black, and the final fitting lines are shown in red. The blue dashed lines are identified components from 1 to 25, and the brackets show the line-locked doublets. The velocities pertain to the short-wavelength lines in the doublets.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Normalized N V line profiles in the VLT-UVES spectra plotted on a velocity scale relative to the quasar redshift z = 2.217. The spectra are shown in black, and the final fitting lines are shown in red. The blue dashed lines are identified components from 1 to 25, and the brackets show the line-locked doublets. The blue bracket in lower left indicates component 16 is blended with unrelated lines. The velocities pertain to the short-wavelength lines in the doublets.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: The component matrix shows all possible line locks in C IV, Si IV and N V based on their velocity separations. We consider that two systems are locked when their velocity separation is a close match (with errors less than 10%) to their laboratory doublet separation (see text for details). All line-locking pairs corresponding to the same ion doublet sat on the same line; the red line for the C IV doublet, the purple line for Si IV, and the green line for N V.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Three complex absorber systems line locked through multi-ion doublets detected in the spectrum of J221531-174408. All clouds are exposed to ionizing radiation from the left. We use blue color to mark the shielding clouds in the line-locked pair. The number inside the cloud box is the corresponding component index shown in Table 1. We also show if the cloud has had C IV, Si IV and N V doublets identified.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Normalized Si IV line profiles in the VLT-UVES spectra plotted on a velocity scale relative to the quasar redshift z = 2.217. The spectra are shown in black, and the final fitting lines are shown in red. The blue dashed lines are identified components from 1 to 25, and the brackets show the line-locked doublets. The velocities pertain to the short-wavelength lines in the doublets.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Results from the CLOUDY model for components 9, 10, 17, 21, and 24 at many log U–log N(H) points assuming solar metallicity. The red, purple, and blue symbols mark the results from simulating the column densities of C IV, Si IV, and N V, respectively. The area where different colored symbols meet shows the most likely model parameters.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Covering fraction C 0 vs. covering fraction C 0 of locked systems. The blue dashed line shows the 1:1 ratio. The blue shadow marks the 10% uncertainties.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: Logarithm of column density vs. logarithm of column density of locked systems. The blue dashed line shows the 1:1 ratio. The blue shadow marks the 10% uncertainties.
Paper: Comparison between the Emission Torus and the Measured Toroidal Magnetic Field for the Crab and Vela Nebulae
Authors: Wei Deng, Fei Xie, Kuan Liu, Mingyu Ge, Youli Tuo, Fabio La Monaca, Alessandro Di Marco, En-wei Liang
Figure caption: The intensity map of the Crab PWN (left) and the Vela PWN (right) in the 2–8 keV energy band, overlaid with the reconstructed polarization vectors (magnetic field, in black lines) cut at the 5σ significance level. The pulsars are located in the center, shown in white dots. The white inclined ellipses are the geometric models proposed in C. Y. Ng & R. W. Romani (2004) for Crab and Vela emission torus. The light-blue contours are obtained from the Chandra observations for Vela PWN. The black bar on the bottom left shows the maximum measured X-ray PD. The frame sizes are 3′ × 3′.
Paper: Comparison between the Emission Torus and the Measured Toroidal Magnetic Field for the Crab and Vela Nebulae
Authors: Wei Deng, Fei Xie, Kuan Liu, Mingyu Ge, Youli Tuo, Fabio La Monaca, Alessandro Di Marco, En-wei Liang
Figure caption: Image of the Crab Nebula (left) and Vela Nebula (right) observed by Chandra. The Crab Nebula exhibits a fully formed double-ring torus-jet feature, while the Vela Nebula presents an incomplete double-arc torus-jet characteristic. The black inclined ellipses are the geometric models proposed in C. Y. Ng & R. W. Romani (2004) for Crab and Vela emission torus. The solid elliptical arcs in the right panel represent Vela emission double arcs. The white points represent the centers of the circular regions for analysis, with the size marked by the white circles, and the centers are in red dots. Arrows are for the region-select direction.
Paper: Comparison between the Emission Torus and the Measured Toroidal Magnetic Field for the Crab and Vela Nebulae
Authors: Wei Deng, Fei Xie, Kuan Liu, Mingyu Ge, Youli Tuo, Fabio La Monaca, Alessandro Di Marco, En-wei Liang
Figure caption: The measured PD (top) and PA (center) of regions along the Crab tours as a function of the azimuth angle. The angle θ represents the normal line direction of the ellipse along the torus, and the δ χ (dots, bottom) represents the deviation of PA from θ. The PA swing model (solid line, bottom) due to different flow velocities β  R  = v/c is defined in N. Bucciantini et al.'s (2017) Equation (A5).
Paper: Comparison between the Emission Torus and the Measured Toroidal Magnetic Field for the Crab and Vela Nebulae
Authors: Wei Deng, Fei Xie, Kuan Liu, Mingyu Ge, Youli Tuo, Fabio La Monaca, Alessandro Di Marco, En-wei Liang
Figure caption: Comparison of the simulated PD (top) and PA (bottom) with the input model for Vela PWN inner arc (left) and outer arc (right), as a function of the azimuth angle of the geometry ellipse. The blue model data and the red simulated data are calculated from a round region with a radius of 5″, while the solid line represents the polarization properties of the model obtained within a circular region with a radius of 2.″5.
Paper: Comparison between the Emission Torus and the Measured Toroidal Magnetic Field for the Crab and Vela Nebulae
Authors: Wei Deng, Fei Xie, Kuan Liu, Mingyu Ge, Youli Tuo, Fabio La Monaca, Alessandro Di Marco, En-wei Liang
Figure caption: The measured PD (top) and PA (center) of regions along the Vela elliptical arcs as a function of the azimuth angle. The definitions of θ and δ χ are the same as Figure 3. These results are obtained from a joint analysis of three detector units in the 2–8 keV energy band. The measured PD values are significantly higher than the minimum detectable polarization at the 99% confidence level (MDP99).
Paper: The Twisting of Radio Waves in a Randomly Inhomogeneous Plasma
Authors: Ze-Lin Zhang, Ruo-Yu Liu
Figure caption: Upper panels: (a) the rms values of GDP ﹩\sqrt{\langle {\alpha }^{2}\rangle }﹩ against ϵ and diffractive length scale l  c ; (b) the rms values of GDP ﹩\sqrt{\langle {\alpha }^{2}\rangle }﹩ against ϵ and the heliocentric distance R ⊙ which is from the Sun to the Earth. Lower panels: (c) the rms values of quantity ﹩\langle {e}^{{\prime} 2}\rangle ﹩ against the heliocentric distance R ⊙ and the minimum wavenumber k m from the Sun to the Earth; (d) the rms values of quantity 〈e ″2〉 against the heliocentric distance R ⊙ and the minimum wavenumber k m from the Sun to the Earth.
Paper: The Twisting of Radio Waves in a Randomly Inhomogeneous Plasma
Authors: Ze-Lin Zhang, Ruo-Yu Liu
Figure caption: (a) The unit tangent vectors ( k  1 and  k  2) of the ray at different moments in unit  k -space (the tantrix sphere of the ray, or the sphere of tangent directions  k ). (b) The ray in ﹩{{\mathbb{R}}}^{3}﹩ space and its projections onto the three mutually perpendicular coordinate planes (x –O–y, y–O–z and z–O–x) are drawn by orange curves. Δs is the arc-length between  k  1 and  k  2. The green arrows represent the unit wavevectors of light at different moments. The polar angle θ and azimuthal angle ϕ in the two subplots correspond to each other.
Paper: The Twisting of Radio Waves in a Randomly Inhomogeneous Plasma
Authors: Ze-Lin Zhang, Ruo-Yu Liu
Figure caption: Top side: the variation of the normalized quantity ﹩{C}_{n}^{2}(r)/{n}^{2}(r)﹩ with the heliocentric distance R ⊙ which varies from the Sun to the Earth. Bottom side: the spatial evolution trend of squared fractional density perturbation amplitude ﹩\langle \delta {n}_{i}^{2}\rangle /{n}^{2}﹩ as it changes with the heliocentric distance R ⊙, where ﹩{l}_{i}(r)=2.5\,\times \,{10}^{4}{\left(r/{R}_{\odot }-1\right)}^{1.3}\,\mathrm{cm}﹩, see Equation (21) and E. P. Kontar et al. (2023). The data presented in the figure is derived from W. A. Coles & J. K. Harmon (1989), E. Marsch & C. Y. Tu (1990), S. R. Spangler (2002), and P. J. Kellogg & T. S. Horbury (2005). The deviation between data and simulation is essentially controlled within an order of magnitude.
Paper: The Twisting of Radio Waves in a Randomly Inhomogeneous Plasma
Authors: Ze-Lin Zhang, Ruo-Yu Liu
Figure caption: Cartoon illustration of depolarization effects. (a) Ideal case: the propagation of radio waves in an anisotropic plasma with uniform distribution along the line-of-sight. The dynamical phase φ DP caused by Faraday rotation effect. (b) Actual case: total phase of depolarization in a turbulent magnetized plasma equals to the dynamical phase φ DP caused by Faraday rotation effect plus the geometric phase φ GP (blue arrows represent the nontrivial rotation to the polarization plane) caused by the twisting path with nonzero torsion (the diagram has, to some extent, magnified the degree of distortion of the path of the ray).
Paper: The Twisting of Radio Waves in a Randomly Inhomogeneous Plasma
Authors: Ze-Lin Zhang, Ruo-Yu Liu
Figure caption: Polarization trihedral (represented by green, blue, and gray arrows, separately) transports along the ray (represented by orange curve) in ﹩{{\mathbb{R}}}^{3}﹩ space with nonzero torsion. The angle Δα between the electric-field vectors  e  1 and  e  2 at different moments is equal to the geometric phase.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Illustration of disk zoning. Different colormaps show the density of solids in the small-grain population for each disk zone, where the four zones are indicated by z0, z1, z2, and z3. The allowed solids that may be present within each zone are listed under each colorbar. Each zone contains new ices along with the solids present in any interior zones (e.g., zone 1 contains water-dominated ices along with refractory dust from zone 0). Inset shows a zoom-in of the inner 10 au.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Simulated HH 48 NE ice band profiles (colors) compared to the spectrum observed with JWST (gray). Top: varying mixing ratios within the polar ice components (H2O:CO2 and H2O:CO). Bottom: varying mixing ratios within the apolar ice component (CO2 and CO). All spectra include an additional H2O-only component. Ice abundances for each model are listed in Table 5 with the model names in parentheses. Model M1 corresponds to the preferred multicomponent ice composition.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Illustration of ice spectrum interpolation. The relative absorbance of an ice band can be expressed as a function of wavelength and mixing ratio with other ice components. Top: experimental ice profiles for different mixing ratios. Bottom: 2D interpolation map of normalized band profiles verses mixing ratio.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Top: ice-phase C/O ratios retrieved from the single-component and preferred multicomponent ice models. Bottom: comparison of HH 48 NE ice C/O ratios to the ice C/O ratios in the model of K. I. Öberg et al. (2011b).
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Test of ice spectrum interpolation scheme. Top: ice absorption bands for a ∼10:2:2 H2O:CO2:CO mixture. The experimental spectrum (Exp. 5) is shown in pink. The synthetic spectrum (black) is made by interpolating between the 10:1:1 and 10:3:3 spectra. Bottom: Differences between the synthetic and experimental spectrum.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: The CO2 ice band observed with JWST (gray) compared to the preferred multicomponent ice mixture from Section 3.3 (orange), and including an additional component of warmed CO2:CO ice (purple).
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Power spectra of NM count rates for several stations, using hourly data, normalized to the mean count rate for each station independently. See the text for details.
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Asymptotic directions on 2015 December 20 at 18:00 UT for MCMU (red) and JBGO (blue) for rigidity ranging from 1 to 100 GV. Several specific rigidity points are noted. Plus signs indicate response-weighted asymptotic directions at this time.
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Histogram of the difference in response-weighted asymptotic longitudes between MCMU and JBGO stations from 2015 December 16 to 2017 January 8, together with a fit (black line) to a normal distribution. The longitude difference is expressed in terms of the rotation of the Earth, with the center of the normal distribution at −169.41 ± 0.31 minutes, with a standard error of 0.31 minute.
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Autocorrelations of NM count rates as a function of time lag: (left) MCMU-MCMU and (right) JBGO-JBGO, showing (from top) the data and fit, residual (data minus fit), and individual terms of the fit function (Equation (2)) with parameter values from Table 2.
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Hourly count rates of JBGO (blue) and MCMU (red) NMs for several days surrounding a Forbush decrease on 2015 December 20. Lightly colored bands show statistical errors.
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Like Figure 4 for cross correlation of NM count rates at MCMU and JBGO. The best fit has an offset in the peak of the exponential term and phase shift of the cosine term.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: Estimation of s  H , E 0 from the limited points of T  e (s), n  e (s) calculated by hydrostatic model for ﹩{s}_{H}^{\mathrm{mod}}=10\ \mathrm{Mm},{E}_{0}^{\mathrm{mod}}=1.0\times {10}^{-2}\ \mathrm{erg}\ {\mathrm{cm}}^{-3}\ {{\rm{s}}}^{-1}﹩, and ﹩{L}_{\mathrm{half}}^{\mathrm{mod}}=55\ \mathrm{Mm}﹩ case. The loop end height h end is set to be 5 Mm from the photosphere. We shift the calculated data points randomly in the error range described below. Top: The 2D histograms show the probability distributions of T  e (s) and n  e (s) derived by a Bayesian analysis. Darker is a higher probability than bright. The green lines show T  e (s) and n  e (s) obtained by E 0 and s  H  that best explain the observations. The green error bars are ﹩{\rm{\Delta }}\mathrm{log}{T}_{e}\ ({\rm{K}})=0.03﹩ and ﹩{\rm{\Delta }}\mathrm{log}{n}_{e}\ ({\mathrm{cm}}^{-3})=0.1﹩, which are comparable to the observations. Bottom: The red solid lines show the best fit and the dashed blue and red lines indicate the 68% and 95% credible intervals.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: The agreement between the hydrostatic model and the observations at various loop end heights h end (top and bottom: T  e (s) and n  e (s) of Loop 3. left to right: h end = 1.3, 5, 8, 10, and 12 Mm). The red lines show T  e (s) and n  e (s) obtained by E 0 and s  H  that best explain the observations as h end = 1.3, 5, 8, 10, and 12 Mm. The error bars of T  e (s) and n  e (s) indicate the ±1σ errors resulting from the photon noise. The horizontal bar shows the length of the segment.