adsabs/AstroCLIMB huggingface dataset:
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: Azimuthal and vertical average of the azimuthal velocity normalized by the tidal amplitude squared ﹩\langle {v}_{\varphi }/{C}_{{\rm{t}}}^{2}{\rangle }_{z,\varphi }﹩ (left), or by ﹩\langle {v}_{\varphi }/\sqrt{{C}_{{\rm{t}}}}{\rangle }_{z,\varphi }﹩ (right), against the distance to the rotation axis s, for low (left) and moderate to high (right) values of the tidal amplitude C t in different colors. The tidal frequency, core size, and Ekman number are set to ω = −0.25, α = 0.7, and E = 10−5, respectively, in both panels.
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: The same as Figure 1 but for α = 0.9 and C t = 10−2. E  dr  is maximal when ω = −0.26 with E  dr  = 7.8 · 10−3 and minimal when ω = 0.26 with E  dr  = 4.3 · 10−10.
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: Left: nonaxisymmetric component of the tidal flow magnitude u 1 against the tidal amplitude C t, when filtering out the zonal flow m = 0 component from the kinetic energy spectrum summed over m ≠ 0 components. Right: energy in the differential rotation E  dr  against tidal amplitude C t. The different nonlinear regimes are indicated with colored lines in both panels. The tidal frequency, core size, and Ekman number are set to ω = −0.25, α = 0.7, and E = 10−5, respectively.
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: Energy in the differential rotation E  dr  against time for different tidal forcing amplitudes C t shown in different colors. The tidal frequency, core size, and Ekman number are set to ω = −0.25, α = 0.7, and E = 10−5, respectively.
Paper: The Enhanced Population of Extreme Mass-ratio Inspirals in the LISA Band from Supermassive Black Hole Binaries
Authors: Smadar Naoz, Zoltán Haiman
Figure caption: An illustration of the system. The hierarchical nature of galaxy formation suggests that a galaxy will undergo multiple mergers with smaller structures, such as dwarf galaxies or global clusters. If these smaller objects host SMBHs (or IMBHs) at their centers, the central galaxy’s SMBH can have several lower-mass SMBH (or IMBH) companions.
Paper: The Enhanced Population of Extreme Mass-ratio Inspirals in the LISA Band from Supermassive Black Hole Binaries
Authors: Smadar Naoz, Zoltán Haiman
Figure caption: Bottom panel: the expected number of EMRIs per unit redshift per year. We consider the SMBH binary scenario (wide purple band), where the upper limit assumes η bin = 1, f LISA = f EKL = 1 and the lower limit assumes η bin = 0.5, f LISA = 0.4 and f EKL = 0.5 (the latter two choices being motivated by N22). The thin green line shows the corresponding rate for single SMBHs via the two-body relaxation channel. Middle panel: the volumetric rate of EMRIs as a function of redshift (see Equation (2)). The bottom panel is obtained by integrating this rate over volume and allowing one year of LISA operation (Equation (3)). Top panel: the enhancement of the EMRI rate in the binary scenario relative to the single-SMBH case. The numbers in this figure do not take into account LISA’s sensitivity (see Section 3).
Paper: The Enhanced Population of Extreme Mass-ratio Inspirals in the LISA Band from Supermassive Black Hole Binaries
Authors: Smadar Naoz, Zoltán Haiman
Figure caption: Characteristic GW strain and noise level for LISA. We show characteristic strains in the LISA band as a function of frequency. We show 2000 randomly chosen EMRI systems and adopt T obs = 4 yr. The thin gray lines show the unresolved systems, while the purple lines above the LISA sensitivity curve show the resolved systems with S/N >8. The thick red solid line shows ﹩\sqrt{S(f)\times f}﹩, as described in the text. The dashed blue line shows ﹩\sqrt{\sum \,\max \ {({h}_{c})}^{2}}﹩ for those 2000 randomly chosen systems, where ﹩\max \ ({h}_{c})﹩ is the maximum characteristic strain of each system. The dashed–dotted magenta line shows ﹩\sqrt{\sum {({h}_{c})}^{2}}﹩, including all the relevant frequencies of the strain for each realization. The black line shows LISA’s sensitivity curve, following Robson et al. (2019).
Paper: The Enhanced Population of Extreme Mass-ratio Inspirals in the LISA Band from Supermassive Black Hole Binaries
Authors: Smadar Naoz, Zoltán Haiman
Figure caption: The astrophysical consequences of binary EMRIs. The x-axis shows the SMBH binary fraction, η bin, which incorporates all of the uncertainties mentioned in this work. This term can be larger than unity if the SMBHs in galactic nuclei typically have multiple companion SMBHs/IMBHs. The left y-axis (red) shows the EMRI noise level at ∼0.012 Hz estimated from the noise calculation described in Section 3.2 and shown in Figure 3, as a function of η bin. LISA’s sensitivity at ∼0.012 Hz (black horizontal line) is overplotted. This frequency corresponds to the largest difference between the EMRI noise level and the LISA sensitivity curve. The right y-axis (blue) shows the estimated number of EMRIs with S/N >8, and T obs = 4 yr, as a function of η bin. The thick vertical yellow lines mark the approximate fractions of PSB galaxies in the local Universe (z ≲ 1) and at z ∼ 2.
Paper: The Enhanced Population of Extreme Mass-ratio Inspirals in the LISA Band from Supermassive Black Hole Binaries
Authors: Smadar Naoz, Zoltán Haiman
Figure caption: Examples of the mass function fits used in these calculations. These are fits for Merloni & Heinz (2008).
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Experimental merged-beams DR rate coefficient α mb(E d) for stored OH+ ions. The present results are plotted as blue symbols with error bars representing one-sigma statistical uncertainties. The absolute scaling of the results has a systematic accuracy of 17% at all energies. For comparison, the relative results of Amitay et al. (1996) from the room-temperature TSR study are added as the full red line, after applying a common scaling factor at all energies to their values to best match the present data in the 1 to 3 eV region. For E d > 5 eV, our results may contain an additional contribution from DE, as is discussed in the text. At the top of the figure, we have plotted the energy-dependent energy resolution ΔE for both experiments. For the CSR results, the energy resolution, shown in blue, is calculated as the FWHM of the simulated collision-energy distribution. For the TSR results, we calculated the energy resolution, shown in red, using the FWHM from the experimental parameters of Amitay et al. (1996). The square symbols show the selected values of E d, and the horizontal lines show the FWHM region of the corresponding collision-energy distributions.(The data used to create this figure are available.)
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Increase of the inferred CRIR from OH+ observations in diffuse clouds using our updated DR rate coefficient for single-zone models. The multiplicative increase R is calculated from the ratio of the destruction rates (see Equation (8)) for the present (α k) and the previous (﹩{k}_{3}^{\mathrm{old}}﹩) DR rate coefficients, adopting the single-zone model of Bacalla et al. (2019), which use the DR data of Mitchell (1990) for ﹩{k}_{3}^{\mathrm{old}}﹩. The result is plotted as the blue full line. The vertical dotted lines enclose the relevant range of ﹩{f}_{{{\rm{H}}}_{2}}﹩ values inferred by Indriolo et al. (2015). The dashed orange line shows the CRIR increase relative to using the DR rate coefficient of Guberman (1995) for ﹩{k}_{3}^{\mathrm{old}}﹩.
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Comparison of the kinetic-temperature-dependent DR rate coefficient α k from our present experiment to previously published works. The shaded area around the present results corresponds to the total systematic uncertainty of the measurement, mainly due to the absolute scaling of α mb and the uncertainty of T ⊥. The particular relative contributions of the uncertainties have been discussed by Paul et al. (2022). The single-pass merged-beams results of Mitchell (1990) have been incorporated into the UMIST database (McElroy et al. 2013). The theoretical results of Guberman (1995) have been incorporated into the KIDA database (Wakelam et al. 2012).
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: OH+ DR rate coefficient α mb(E d) for low electron current measurements. (a) Comparison of α mb from two storage-time windows, from ≈25 to ≈33 s (red triangles) and from ≈145 to ≈250 s (green squares). (b) Comparison of α mb from the storage-time window with equilibrated populations (from ≈145 to ≈250 s, green squares) and the fitted ﹩{\alpha }_{0}^{\mathrm{mb}}﹩ (orange pentagons). (c) Comparison of α mb from the high electron current measurements (blue circles) with the fitted ﹩{\alpha }_{0}^{\mathrm{mb}}﹩ (orange pentagons). All error bars represent one-sigma statistical uncertainties.
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Collisional-radiative model of OH+ rotational level population evolution as a function of ion storage time for the high electron current DR measurements. The dashed and solid lines are for the mean model with the parameters k B T ⊥ = 2 meV, T low = 6 K, ε = 1.0 × 10−2, and an initial rotational temperature of 3000 K. The accompanying shaded areas indicate the uncertainty of the predictions when varying these parameters, the dipole moment, the electron-impact rotational excitation cross sections, and the initial rotational temperature, all within their estimated uncertainties. The dashed or solid lines differentiate between periods with or without electrons, respectively.
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Comparison of diffuse cloud model results with the observations of Indriolo et al. (2015) in the plane of the column density ratios N(OH+)/N(H2O+) and N(OH+)/N(H). The observations of Indriolo et al. (2015) are plotted as diamond symbols with error bars. The model results are plotted as the blue and red curves. The blue curves are loci of constant ζ  p (H)/n 50 in units of 10−16 s−1 labeled by their corresponding values. The red curves are loci of constant A V(tot) in magnitudes labeled by their corresponding values. (a) Predictions of the present model. (b) Predictions of Neufeld & Wolfire (2017).
Paper: Dissociative Recombination of Rotationally Cold OH+ and Its Implications for the Cosmic Ray Ionization Rate in Diffuse Clouds
Authors: Ábel Kálosi, Lisa Gamer, Manfred Grieser, Robert von Hahn, Leonard W. Isberner, Julia I. Jäger, Holger Kreckel, David A. Neufeld, Daniel Paul, Daniel W. Savin, Stefan Schippers, Viviane C. Schmidt, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Same as Figure 5, but for the low electron current DR measurements.
Paper: Far-ultraviolet to Near-infrared Observations of SN 2023ixf: A High-energy Explosion Engulfed in Complex Circumstellar Material
Authors: Rishabh Singh Teja, Avinash Singh, Judhajeet Basu, G. C. Anupama, D. K. Sahu, Anirban Dutta, Vishwajeet Swain, Tatsuya Nakaoka, Utkarsh Pathak, Varun Bhalerao, Sudhanshu Barway, Harsh Kumar, Nayana A. J., Ryo Imazawa, Brajesh Kumar, Koji S. Kawabata
Figure caption: Optical spectral evolution for SN 2023ixf from HCT, Perley & Gal-Yam (2023), and Stritzinger et al. (2023). The spectra are corrected for the redshift of the host galaxy, M101, and the epochs are labeled with respect to our adopted explosion epoch. Top left: early-time spectral sequence of flash features in SN 2023ixf with line identification of high-ionization features and Balmer lines. The inset depicts the Hα profile at +7.9 days having a broad P Cygni feature and intermediate-width Lorentzian emission. Top right: evolution of the line profile of Hα during the flash phase. Bottom left: spectral sequence of SN 2023ixf during the photospheric phase. Bottom right: evolution of the multipeaked emission profile of Hα during the photospheric phase. Here HV and PV refer to the high- and photospheric-velocity components in the blueshifted absorption wing of Hα.
Paper: Far-ultraviolet to Near-infrared Observations of SN 2023ixf: A High-energy Explosion Engulfed in Complex Circumstellar Material
Authors: Rishabh Singh Teja, Avinash Singh, Judhajeet Basu, G. C. Anupama, D. K. Sahu, Anirban Dutta, Vishwajeet Swain, Tatsuya Nakaoka, Utkarsh Pathak, Varun Bhalerao, Sudhanshu Barway, Harsh Kumar, Nayana A. J., Ryo Imazawa, Brajesh Kumar, Koji S. Kawabata
Figure caption: Left: NUV spectral evolution for SN 2023ixf obtained using Swift/UVOT. Top right: FUV spectral evolution obtained using Astrosat/UVIT and the SYNAPPS fit to the spectra of ∼7 and ∼12 days. Bottom right: spectral comparison of NUV spectra with other Type II SNe.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Spectra for the polar and equatorial viewing directions for the 3D AD1 and 3D AD2 models at 0.8 days. The height of each wavelength point is colored according to the emitting species of the last interactions of the emerging radiation packets. The area under the horizontal axis shows the distribution of frequencies (colored by absorbing/scattering ion) just prior to the last interactions of the emerging packets. The 11 most-significant ions are separately colored, while the “Other” group combines many smaller contributions from other ions.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Mollweide projections of direction-dependent quantities for 3D AD2 UVOIR packets arriving at the observer between 1.3 and 1.7 days: radiant intensity times 4π solid angle (top), mean temperature at last interaction (middle), and line-of-sight velocity at last interaction (bottom). For these figures, we use 32 × 32 direction bins, uniformly spaced in azimuthal angle (horizontal) and cosine of the polar angle (vertical) to give the same solid angle in each bin.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Time series of spectra in the polar direction of the 3D AD2 model compared to reddening- and redshift-corrected spectra of AT2017gfo (Pian et al. 2017; Smartt et al. 2017). The area under the spectra has been colored by the emitting species of the last interactions of the emerging packets. The times of the ARTIS and AT2017gfo spectra intentionally do not match.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Comparison between the nuclear mass fractions from the ARTIS decay-only treatment and the full nuclear network calculation for a cell at z = 0 and radial velocity v  r  = 0.24c with Y  e  = 0.13.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Comparison of the energy release rates of the ARTIS treatment in 3D AD2 vs. the output of the full nuclear network (GSI network). Neglecting fission reactions has only a negligible effect on the total energy release rates.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Spherically averaged spectra at 0.8 days for the 3D AD1 (solid blue), 3D AD2 (solid orange), 1D AD1 (dashed blue), and 1D AD2 (dashed orange) models.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Direction-integrated luminosity vs. time for the models 3D AD1, 3D AD2, 1D AD1, and 1D AD2, the 3D gray opacity model of Collins et al. (2023), and inferred bolometric luminosity of AT2017gfo (Smartt et al. 2017).
Paper: Ultracool Dwarfs Observed with the Spitzer Infrared Spectrograph: Equatorial Latitudes in L Dwarf Atmospheres Are Cloudier
Authors: Genaro Suárez, Johanna M. Vos, Stanimir Metchev, Jacqueline K. Faherty, Kelle Cruz
Figure caption: Correlation between the spin axis inclination and the silicate index for 10 L3–L7 young (squares) and old (circles) dwarfs with Spitzer IRS spectra (Table 1). The auxiliary axis indicates the 2MASS J − K s (left panel) and the WISE W1−W2 (right panel) color anomaly defined as the observed color of each object minus the average color (Table 2) for its spectral type and surface gravity according to Faherty et al. (2016). The star symbol indicates the only object (VHS1256b) on the plot with a silicate index measurement not from Spitzer IRS spectra but from the JWST Mid-Infrared Instrument (MIRI; Section 4.3).
Paper: Far-ultraviolet to Near-infrared Observations of SN 2023ixf: A High-energy Explosion Engulfed in Complex Circumstellar Material
Authors: Rishabh Singh Teja, Avinash Singh, Judhajeet Basu, G. C. Anupama, D. K. Sahu, Anirban Dutta, Vishwajeet Swain, Tatsuya Nakaoka, Utkarsh Pathak, Varun Bhalerao, Sudhanshu Barway, Harsh Kumar, Nayana A. J., Ryo Imazawa, Brajesh Kumar, Koji S. Kawabata
Figure caption: Left: multiband photometry is shown along with the data compiled from public sources. The middle panel shows the bolometric light-curve evolution. The bottom panel shows the color evolution of SN 2023ixf along with the other SNe with observed flash features. Right: best model light curves that could represent the g-band light-curve evolution of SN 2023ixf obtained out of a large sample of >170,000 models presented in Moriya et al. (2023) for different progenitor masses. The photometric data obtained using AstroSat, GIT, Kanata, and Swift are available as data behind the figure.(The data used to create this figure are available.)
Paper: Snowflakes in a Furnace: Formation of CO and Dust in a Recurrent Nova Eruption
Authors: D. P. K. Banerjee, C. E. Woodward, V. Joshi, A. Evans, F. M. Walter, G. H. Marion, E. Y. Hsiao, N. M. Ashok, R. D. Gehrz, S. Starrfield
Figure caption: The left panel shows the entire NIR spectrum (available as data behind the figure) of V745 Sco 8.7 days after the 2014 eruption (Banerjee et al. 2014). The right panel shows a magnified view of the first overtone CO emission (black). Superposed on the emission are the absorption bandheads of 12CO and 13CO (vertical ticks). The spectrum of a typical M6 III, HD 18191 (blue), is also included to show the expected CO absorption bandheads. The red line is an LTE model fit to the CO emission. The flux axes in both panels have the same units.(The data used to create this figure are available.)
Paper: Observations of Twist, Current Helicity, and Writhe in the Magnetic Knots of δ-sunspots Consistent with the Kink Instability of a Highly Twisted Flux Rope
Authors: Peter J. Levens, Aimee A. Norton, Mark G. Linton, Kalman J. Knizhnik, Yang Liu
Figure caption: The magnetic knots of NOAA 11158 (top), 11267 (middle), and 11476 (lower) are shown as observed in the HMI continuum intensity (column 1), magnetogram of B  r  (column 2), and the calculated values of α  r  (column 3) and J  r  (column 4). In the latter two columns, red and blue indicate (+) and (−) values, respectively, with high values of α  r  across the neutral lines due to high shear and in quiet-Sun due to low magnetic field strengths. The green contours identify the magnetic knots, i.e., the umbrae forming the δ-spot. The average value of α  r  for the two ends of each of the knots through their lifetime are the same sign and the value of J  r  for the two ends of the knots through each of their lifetimes are the opposite sign. Each image axis is in units of pixels with the length of 1 pixel being roughly 0.36 Mm on the surface of the Sun as per the Lambert cylindrical equal-area projection of these HMI data products.