adsabs/AstroCLIMB huggingface dataset:
Paper: Early Insights for Atmospheric Retrievals of Exoplanets Using JWST Transit Spectroscopy
Authors: Savvas Constantinou, Nikku Madhusudhan, Siddharth Gandhi
Figure caption: A transmission spectrum of WASP-39 b. The circles with error bars show the JWST NIRSpec PRISM spectrum in the 3–5 μm range reduced with the Tiberius pipeline (The JWST Transiting Exoplanet Community Early Release Science Team et al. 2022) along with prior HST/WFC3 observations in the 0.8–1.7 μm range (Wakeford et al. 2018). The solid curve in brown shows our retrieved best-fit spectrum, and the same spectrum but without opacity contributions from aerosols is shown in blue for reference (see Section 4.2.1). The heights of the prominent spectral features in the JWST and HST bands in terms of a characteristic atmospheric scale height are denoted by arrows; a nominal slant photospheric temperature of 800 K is assumed motivated by the retrieved constraints. The contributions of individual molecules are shown in Figure 6 in the Appendix.
Paper: Early Insights for Atmospheric Retrievals of Exoplanets Using JWST Transit Spectroscopy
Authors: Savvas Constantinou, Nikku Madhusudhan, Siddharth Gandhi
Figure caption: Retrieved spectral fits obtained for two of the retrievals considered in this work, using our canonical model described in Section 3. The top panel shows the retrieved spectral fit for JWST NIRSpec PRISM 3–5 μm observations reduced with the Tiberius pipeline (data shown in black error bars with yellow circles). Also shown are the same observations reduced with the Eureka pipeline (in green). The bottom two panels show different wavelength regions of the retrieved spectral fit to the combination of HST/WFC3 observations (0.8–1.7 μm) and JWST/NIRSpec PRISM observations reduced with Tiberius; see Section 2. In all three panels, the darkest orange line denotes the median retrieved spectrum while the two lighter orange regions denote the corresponding 1σ and 2σ contours.
Paper: Overmassive Black Holes in Dwarf Galaxies Out to z ∼ 0.9 in the VIPERS Survey
Authors: Mar Mezcua, Malgorzata Siudek, Hyewon Suh, Rosa Valiante, Daniele Spinoso, Silvia Bonoli
Figure caption: Top left: spectral energy distribution fitting of the rest-frame observed ultraviolet, optical, and infrared (when available) photometry (black points) with the best-fit model (black curve), including a combination of the galaxy template (green), an AGN accretion disk component (blue), and an AGN dust torus model (yellow). Top right: PDF for the stellar mass taking into account all possible fractions of AGN emission and providing an upper limit on the stellar mass. So the most probable value (MsPDF; blue dashed line) has a higher value than the best-fit stellar mass (MsBEST; red solid line). The 16th and 84th percentile intervals (gray shades) are also indicated. Middle: emission line fitting of the VIPERS spectrum including the continuum emission (in yellow; top panel), and the broad lines (in blue) decomposed into broad (in red) and narrow (in green) components (zoom-in in the bottom panels). Bottom: Subaru Hyper Suprime-Cam image in the i band.
Paper: Overmassive Black Holes in Dwarf Galaxies Out to z ∼ 0.9 in the VIPERS Survey
Authors: Mar Mezcua, Malgorzata Siudek, Hyewon Suh, Rosa Valiante, Daniele Spinoso, Silvia Bonoli
Figure caption: Cosmological semianalytical simulations of a plausible evolution history of one of the BLAGN dwarf galaxies. Its full history (blue pentagons and dotted line) shows that it is overmassive with respect to the M BH–M ∗ scaling relation of Suh et al. (2020; gray solid line) since at least z > 4. Extending the evolution of the simulations down to z = 0 (green pentagons and dotted line), the candidate tends to reach a stellar mass M ∗ > 1010 M ⊙ and to move toward the local M BH–M bulge relation of inactive massive early-type galaxies of Kormendy & Ho (2013; green dashed line). The median M BH–M ∗ relation for all the z = 0 galaxies simulated by L-Galaxies/Millennium-II is shown as a purple dashed line (with the purple area showing the 16th/84th percentiles of the distribution).
Paper: Overmassive Black Holes in Dwarf Galaxies Out to z ∼ 0.9 in the VIPERS Survey
Authors: Mar Mezcua, Malgorzata Siudek, Hyewon Suh, Rosa Valiante, Daniele Spinoso, Silvia Bonoli
Figure caption: Ratio of M BH/M ∗ vs. redshift for the sample of BLAGN dwarf galaxies. We show for comparison the non-evolution found by Suh et al. (2020) for z ∼ 0–2.5 (black line, 1σ scatter ∼0.5 dex), Sun et al. (2015) for z ∼ 0–2 (brown line), and Setoguchi et al. (2021) for z ∼ 1.2–1.7 (red line), and the z-evolution found by Decarli et al. (2010) for z ∼ 0–3 (dashed blue line), Trakhtenbrot & Netzer (2010) for z ∼ 0.1–2 (dashed yellow line), and Bennert et al. (2011) for z ∼ 1–2 (dashed green line, including the data of Merloni et al. 2010). We note that the Suh+2020 sample is the only one for which the black hole and stellar masses have been computed using the same procedure and parameters as in our sample.
Paper: Overmassive Black Holes in Dwarf Galaxies Out to z ∼ 0.9 in the VIPERS Survey
Authors: Mar Mezcua, Malgorzata Siudek, Hyewon Suh, Rosa Valiante, Daniele Spinoso, Silvia Bonoli
Figure caption:  M BH vs. M ∗ for the VIPERS sample of BLAGN dwarf galaxies. We show for comparison the low-z AGN of Reines & Volonteri (2015; RV2015) and the high-z AGN of Suh et al. (2020; Suh+2020), whose masses have been computed using the same procedure and parameters as in our sample. The solid line shows the local + high-z M BH–M ∗ correlation found for the combination of the RV2015 and Suh+2020 samples with a 1σ scatter of 0.5 dex.
Paper: Indirect Evidence for Dark Matter Density Spikes around Stellar-mass Black Holes
Authors: Man Ho Chan, Chak Man Lee
Figure caption: The black and red solid lines indicate the relation between γ and ﹩\dot{P}﹩ for A0620-00 and XTE J1118+480, respectively. The horizontal dashed lines and dotted lines represent the mean values and the 1σ limits of the observed orbital decay rates (black: A0620-00; red: XTE J1118+480).
Paper: Early Results from GLASS-JWST. IX. First Spectroscopic Confirmation of Low-mass Quiescent Galaxies at z > 2 with NIRISS
Authors: Danilo Marchesini, Gabriel Brammer, Takahiro Morishita, Pietro Bergamini, Xin Wang, Marusa Bradac, Guido Roberts-Borsani, Victoria Strait, Tommaso Treu, Adriano Fontana, Tucker Jones, Paola Santini, Benedetta Vulcani, Ana Acebron, Antonello Calabrò, Marco Castellano, Karl Glazebrook, Claudio Grillo, Amata Mercurio, Themiya Nanayakkara, Piero Rosati, Chanita Tubthong, Eros Vanzella
Figure caption: Top: NIRISS F115W+F150W+F200W spectrum of HFF-DS 4877 (gray symbols) with Grizli best-fit model (red solid curve) and FAST best-fit model (blue solid curve) overplotted. The positions of major spectral features (e.g., [O II], Ca II HK, Hδ, Hγ, Hβ, [O III], Mgb, and NaD) are highlighted at the best-fit Grizli redshift. The gravitational lensing magnification factor and stellar mass, corrected for lensing magnification, derived assuming the spectroscopic redshift are listed. The top-left inset shows the Grizli redshift probability function p(z) in orange, with listed the best-fist Grizli spectroscopic redshift and upper and lower 3σ values. The bottom-right insets show false-color images (2″ × 2″) from HST-WFC3/NIR bands (left) and JWST-NIRISS bands (right). Bottom: same as the top panel, but for HFF-DS 5607. With a gravitational lensing corrected stellar mass below 1010 M ⊙, HFF-DS 5607 is the first low-mass quiescent galaxy spectroscopically confirmed at z > 2.
Paper: Early Results from GLASS-JWST. IX. First Spectroscopic Confirmation of Low-mass Quiescent Galaxies at z > 2 with NIRISS
Authors: Danilo Marchesini, Gabriel Brammer, Takahiro Morishita, Pietro Bergamini, Xin Wang, Marusa Bradac, Guido Roberts-Borsani, Victoria Strait, Tommaso Treu, Adriano Fontana, Tucker Jones, Paola Santini, Benedetta Vulcani, Ana Acebron, Antonello Calabrò, Marco Castellano, Karl Glazebrook, Claudio Grillo, Amata Mercurio, Themiya Nanayakkara, Piero Rosati, Chanita Tubthong, Eros Vanzella
Figure caption: Top: the sSFR vs. M star diagram of galaxies selected as explained in Section 2. The candidates of low-mass quiescent galaxies at z > 2 are shown color-coded as a function of redshift; larger colored filled circles indicate larger stellar masses. Bottom: UVJ diagram of the same galaxies plotted in the top panel, with the quiescent wedge as defined in Martis et al. (2016) plotted in gray. Eight robust candidates of low-mass quiescent galaxies at z > 2 are identified.
Paper: Early Results from GLASS-JWST. IX. First Spectroscopic Confirmation of Low-mass Quiescent Galaxies at z > 2 with NIRISS
Authors: Danilo Marchesini, Gabriel Brammer, Takahiro Morishita, Pietro Bergamini, Xin Wang, Marusa Bradac, Guido Roberts-Borsani, Victoria Strait, Tommaso Treu, Adriano Fontana, Tucker Jones, Paola Santini, Benedetta Vulcani, Ana Acebron, Antonello Calabrò, Marco Castellano, Karl Glazebrook, Claudio Grillo, Amata Mercurio, Themiya Nanayakkara, Piero Rosati, Chanita Tubthong, Eros Vanzella
Figure caption: SEDs of the selected candidates of low-mass quiescent galaxies at z > 2. Filled colored circles represent the observed HFF-DeepSpace photometry; the gray and black curves show the best-fit EAZY and FAST models, respectively. The photometric redshifts and the corresponding 1σ errors are listed. The two galaxies (IDs = 4877 and 5607) with NIRISS spectroscopy presented in this Letter are highlighted in orange.
Paper: Early Results from GLASS-JWST. IX. First Spectroscopic Confirmation of Low-mass Quiescent Galaxies at z > 2 with NIRISS
Authors: Danilo Marchesini, Gabriel Brammer, Takahiro Morishita, Pietro Bergamini, Xin Wang, Marusa Bradac, Guido Roberts-Borsani, Victoria Strait, Tommaso Treu, Adriano Fontana, Tucker Jones, Paola Santini, Benedetta Vulcani, Ana Acebron, Antonello Calabrò, Marco Castellano, Karl Glazebrook, Claudio Grillo, Amata Mercurio, Themiya Nanayakkara, Piero Rosati, Chanita Tubthong, Eros Vanzella
Figure caption: Stellar population properties (stellar age vs. τ, left panels; stellar metallicity vs. dust obscuration, right panels) and corresponding errors derived from modeling the photometry alone (blue square and error bars, cyan dashed box) and the photometry combined with the NIRISS spectroscopy (red circle and error bars, pink dashed box). Error bars represent 1σ uncertainties, while the dashed boxes represent 1σ errors. Top panels show the results for ID = 4877; bottom panels show the results from ID = 5607.
Paper: GOALS-JWST: NIRCam and MIRI Imaging of the Circumnuclear Starburst Ring in NGC 7469
Authors: Thomas Bohn, Hanae Inami, Tanio Diaz-Santos, Lee Armus, S. T. Linden, Vivian U, Jason Surace, Kirsten L. Larson, Aaron S. Evans, Shunshi Hoshioka, Thomas Lai, Yiqing Song, Joseph M. Mazzarella, Loreto Barcos-Munoz, Vassilis Charmandaris, Justin H. Howell, Anne M. Medling, George C. Privon, Jeffrey A. Rich, Sabrina Stierwalt, Susanne Aalto, Torsten Böker, Michael J. I. Brown, Kazushi Iwasawa, Matthew A. Malkan, Paul P. van der Werf, Philip Appleton, Christopher C. Hayward, Francisca Kemper, David Law, Jason Marshall, Eric J. Murphy, David Sanders
Figure caption: NIRCam F200W/F150W vs. F444W/F200W color–color plot of the star-forming regions in the starburst ring of NGC 7469. The markers follow that of Figure 3, where red sources, F200W/F150W > 1.1 or F444W/F200W > 2.5, are labeled. Sources with fluxes below the 3σ detection threshold are treated as upper limits for the associated filter. The median colors of each source group are shown with the same markers, but in black. Two single-stellar population models (the green dashed line with f cov, the fraction of ionizing photons, equal to 1.0 and the dark blue solid line with f cov = 0.5) are also shown, where the crosses denote the locations where the stellar age is 3 and 5 Myr. The typical error and an attenuation vector representing A  V  = 3.0 are included. The dashed–dotted line indicates the effect of adding hot dust (800 K) to a 3 Myr population. The positions of the arrows indicate fractional contributions of 25% and 50% to the F444W flux. The majority of the JWST sources with red colors likely have young (3–5 Myr) stellar populations that are highly obscured and contain large amounts of hot dust.
Paper: GOALS-JWST: NIRCam and MIRI Imaging of the Circumnuclear Starburst Ring in NGC 7469
Authors: Thomas Bohn, Hanae Inami, Tanio Diaz-Santos, Lee Armus, S. T. Linden, Vivian U, Jason Surace, Kirsten L. Larson, Aaron S. Evans, Shunshi Hoshioka, Thomas Lai, Yiqing Song, Joseph M. Mazzarella, Loreto Barcos-Munoz, Vassilis Charmandaris, Justin H. Howell, Anne M. Medling, George C. Privon, Jeffrey A. Rich, Sabrina Stierwalt, Susanne Aalto, Torsten Böker, Michael J. I. Brown, Kazushi Iwasawa, Matthew A. Malkan, Paul P. van der Werf, Philip Appleton, Christopher C. Hayward, Francisca Kemper, David Law, Jason Marshall, Eric J. Murphy, David Sanders
Figure caption: NIRCam and MIRI image mosaic of the starburst ring in four filters: NIRCam/F150W, NIRCam/F444W, MIRI/F560W, and MIRI/F770W. The AGN has been masked out in each filter. The source locations for both the NIRCam and MIRI region catalogs are overplotted. Note that the marker sizes are not representative of the extraction sizes. In the top panels, sources identified with HST at 1.1 μm by DS07 that span a range of ages <5 Myr (cyan squares) to >5 Myr (cyan triangles) are shown. We also include five sources from DS07 where age estimation could not be determined (cyan diamonds). Star-forming regions newly identified with JWST are shown as red circles (F150W-selected) and stars (F444W-selected). In the bottom panels, star-forming regions identified in the F560W filter are shown as red circles and are labeled from the brightest, M1, to the faintest, M11. In total, we detect 66 star-forming regions in NIRCam. This more than doubles the 30 sources previously identified by HST.
Paper: GOALS-JWST: NIRCam and MIRI Imaging of the Circumnuclear Starburst Ring in NGC 7469
Authors: Thomas Bohn, Hanae Inami, Tanio Diaz-Santos, Lee Armus, S. T. Linden, Vivian U, Jason Surace, Kirsten L. Larson, Aaron S. Evans, Shunshi Hoshioka, Thomas Lai, Yiqing Song, Joseph M. Mazzarella, Loreto Barcos-Munoz, Vassilis Charmandaris, Justin H. Howell, Anne M. Medling, George C. Privon, Jeffrey A. Rich, Sabrina Stierwalt, Susanne Aalto, Torsten Böker, Michael J. I. Brown, Kazushi Iwasawa, Matthew A. Malkan, Paul P. van der Werf, Philip Appleton, Christopher C. Hayward, Francisca Kemper, David Law, Jason Marshall, Eric J. Murphy, David Sanders
Figure caption: NIRCam/F150W image where F150W-selected and NIRCam/F444W-selected star-forming regions with red colors (F200W/F150W > 1.1 or F444W/F200W > 2.5) are labeled. The markers are the same as Figure 2 and the contour levels show the MIRI/F560W emission. Groups of sources with red NIR colors are somewhat clustered in the north and southwest regions, which coincide with the peaks of MIR and radio emission. The markers sizes are not representative of the extraction sizes.
Paper: GOALS-JWST: NIRCam and MIRI Imaging of the Circumnuclear Starburst Ring in NGC 7469
Authors: Thomas Bohn, Hanae Inami, Tanio Diaz-Santos, Lee Armus, S. T. Linden, Vivian U, Jason Surace, Kirsten L. Larson, Aaron S. Evans, Shunshi Hoshioka, Thomas Lai, Yiqing Song, Joseph M. Mazzarella, Loreto Barcos-Munoz, Vassilis Charmandaris, Justin H. Howell, Anne M. Medling, George C. Privon, Jeffrey A. Rich, Sabrina Stierwalt, Susanne Aalto, Torsten Böker, Michael J. I. Brown, Kazushi Iwasawa, Matthew A. Malkan, Paul P. van der Werf, Philip Appleton, Christopher C. Hayward, Francisca Kemper, David Law, Jason Marshall, Eric J. Murphy, David Sanders
Figure caption: False-color images of NGC 7469 taken with MIRI/BRIGHTSKY (a) and NIRCam/SUB160P subarray modes (b). The MIRI image contains all three observed filters: F560W (blue), F770W (green), and F1500W (red). The central box on the left represents the size of the subarray image on the right. The NIRCam imaging includes the F150W (blue), F200W (green), and F444W (red) filters. Fifty-nine and 22 pixels are saturated in the MIRI/F1500W and NIRCam/F444W filters, which have the most saturation, due to the central AGN, respectively. Note that the AGN is not subtracted in these images. North is up and the east is to the left.
Paper: Evidence for Enrichment of Niobium-92 in the Outer Protosolar Disk
Authors: Yuki Hibiya, Tsuyoshi Iizuka, Hatsuki Enomoto, Takehito Hayakawa
Figure caption: Zirconium isotope ratios after interference corrections for ((a)–(c)) Mo- and (d) Ru-doped NIST SRM 3169 Zr standard solutions. Each data point represents a single measurement. The error bars represent 2σ. The yellow bands indicate the ranges of the measured isotopic ratios for samples analyzed in this study. The 95Mo/90Zr and 99Ru/90Zr ratios of our sample solutions after purification are smaller than the accurate correction limits.
Paper: Evidence for Enrichment of Niobium-92 in the Outer Protosolar Disk
Authors: Yuki Hibiya, Tsuyoshi Iizuka, Hatsuki Enomoto, Takehito Hayakawa
Figure caption: Comparison of the initial 92Nb/93Nb ratios of the meteorites. (a) Initial 92Nb/93Nb vs. U–Pb age plots for the meteorites. (b) 92Nb/93Nb ratios at the time of CAI formation (4567.3 Myr; Connelly et al. 2012), (92Nb/93Nb)0, derived from the meteorites. The data are from this study and Schönbächler et al. (2002), Iizuka et al. (2016), and Haba et al. (2021) for the initial 92Nb/93Nb ratios and Amelin et al. (2019), Blinova et al. (2007), Iizuka et al. (2019), Brennecka et al. (2020), Iizuka et al. (2014, and Haba et al. (2019) for data for the U–Pb ages. All errors represent 2σ. The red and blue lines represent the 92Nb/93Nb decay curves passing through the data points of the “noncarbonaceous” mesosiderites and “carbonaceous” meteorite NWA 6704, yielding (92Nb/93Nb)0 of (1.66 ± 0.10) × 10−5 and (2.96 ± 0.27) × 10−5, respectively.
Paper: Evidence for Enrichment of Niobium-92 in the Outer Protosolar Disk
Authors: Yuki Hibiya, Tsuyoshi Iizuka, Hatsuki Enomoto, Takehito Hayakawa
Figure caption: Zirconium isotope ratios measured for ((a)–(c)) Fe-, ((d)–(f)) Cr-, and ((g)–(i)) Ti-doped NIST SRM 3169 Zr standard solutions. Each data point represents a single measurement. The error bars represent 2σ. The yellow bands indicate the ranges of the samples used for the discussion in this study.
Paper: Possible Evidence for Lorentz Invariance Violation in Gamma-Ray Burst 221009A
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: The SED for GRB 221009A with the Fermi-LAT spectrum and the LHAASO, and Carpet 2 95% lower limits. The dashed curve indicates the extrapolation of the LAT spectrum to higher energies without γ γ absorption, and with γ γ absorption assuming E QG/E Planck = 49, as indicated. The absorption assuming no LIV is identical to this curve at E < 3 × 105 GeV, but does not have the E > 105 GeV part shown on the plot. We have also plotted the spectrum for the nearby HAWC source HWC3 J1928+178 and its extrapolation to higher energies.
Paper: Possible Evidence for Lorentz Invariance Violation in Gamma-Ray Burst 221009A
Authors: Justin D. Finke, Soebur Razzaque
Figure caption: The γ-ray absorption optical depth at z = 0.1505 and E = 251 TeV (solid black curves). The left figure shows the result assuming the leading order correction is linear (n = 1); the right shows the result assuming the leading order correction is quadratic (n = 2). Dashed blue lines with arrows show the τ  γ γ  upper limit from the Carpet 2 observations.
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: Left panel: evolutionary tracks of a 1.8 M ⊙ star computed with the OPAL, OP, and OPLIB opacity tables. Right panel: the evolution of a frequency ratio of the fundamental and first-overtone radial modes. Gray dots represent models with the effective temperature, T eff = 7020 K, and luminosity, ﹩\mathrm{log}L/﹩                   L ⊙ = 1.2, marked with a dot in the left panel.
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: Left panel: the run of the Rosseland mean opacity from OPAL, OP, and OPLIB data inside the model with a mass 1.8 M ⊙, effective temperature T eff = 7020 K, and luminosity ﹩\mathrm{log}L/﹩                   L ⊙ = 1.2. Right panel: the corresponding differences in ﹩\mathrm{log}\kappa ﹩.
Paper: As a Matter of Dynamical Range – Scale Dependent Energy Dynamics in MHD Turbulence
Authors: Philipp Grete, Brian W. O'Shea, Kris Beckwith
Figure caption: Illustrative sketches of the energy spectrum (top), cross-scale energy flux (middle), and absolute rate of change in energy (bottom) for idealized turbulence. Energy is injected to the system on the largest scales (in our simulations through a mechanical stochastic forcing process) resulting in large-scale eddies. Phenomenologically, these eddies break up into smaller and smaller eddies transferring energy to smaller scales at a constant energy flux on intermediate scales. At the smallest scales energy is dissipated. In direct numerical simulations (DNSs) the dissipative scales are resolved whereas in implicit large eddy simulation (ILES) dissipation is numerical in nature. In the stationary regime, the system is in balance, i.e., the integrated rate of change in energy injected to the system (bottom left) corresponds to the energy being dissipated (bottom right).
Paper: As a Matter of Dynamical Range – Scale Dependent Energy Dynamics in MHD Turbulence
Authors: Philipp Grete, Brian W. O'Shea, Kris Beckwith
Figure caption: Mean kinetic (top) and magnetic (bottom) energy spectra in the stationary regime for simulations with varying dynamical range (left panels with the x-axis scaled to the forcing scale, k  f , and center panels scaled to the peak dissipative scale, k  d ) and fixed dynamical range but varying resolution (right). The left and right spectra are normalized to the mean energy between 1.5k  f  ≤ k ≤ 6k  f  and the center spectra are normalized to unity at k  d . The (barely visible) shaded regions show the standard deviation of the spectra over time.
Paper: As a Matter of Dynamical Range – Scale Dependent Energy Dynamics in MHD Turbulence
Authors: Philipp Grete, Brian W. O'Shea, Kris Beckwith
Figure caption: Fitting the rate of change in energy from the dissipative transfer terms, ﹩{{ \mathcal T }}_{\nu {\rm{U}}}﹩ and ﹩{{ \mathcal T }}_{\eta {\rm{B}}}﹩, to the residual in an ILES (top), an almost-resolved DNS (center), and a DNS (bottom). For the DNS the residual is calculated from all fluxes excluding the dissipative terms whereas in the ILES the residual is a true residual from the analysis.
Paper: As a Matter of Dynamical Range – Scale Dependent Energy Dynamics in MHD Turbulence
Authors: Philipp Grete, Brian W. O'Shea, Kris Beckwith
Figure caption: Mean cross-scale fluxes of the simulations with varying dynamical range (left) and identical range but varying resolution (right) for, from top to bottom, kinetic-to-kinetic, magnetic-to-magnetic, magnetic-to-kinetic via magnetic tension, kinetic-to-magnetic via magnetic tension, and all-to-all (total) energy fluxes.
Paper: As a Matter of Dynamical Range – Scale Dependent Energy Dynamics in MHD Turbulence
Authors: Philipp Grete, Brian W. O'Shea, Kris Beckwith
Figure caption: Calculated effective ν and η in the ILES with large-scale forcing and varying resolution (cell width Δ x ) and power-law fits to the data.
Paper: As a Matter of Dynamical Range – Scale Dependent Energy Dynamics in MHD Turbulence
Authors: Philipp Grete, Brian W. O'Shea, Kris Beckwith
Figure caption: Mean (temporal) cross-scale fluxes of DNSs (with varying η and ν) and ILESs (with varying resolution).
Paper: A Need to Revise Stellar Opacities from Asteroseismology of δ Scuti Stars
Authors: Jadwiga Daszyńska-Daszkiewicz, Przemysław Walczak, Alexey Pamyatnykh, Wojciech Szewczuk, Wojciech Niewiadomski
Figure caption: The normalized histograms for the mass (in M ⊙) of BP Peg, AE UMa, RV Ari, and SX Phe. All seismic models were computed with the OPAL opacities.