adsabs/AstroCLIMB huggingface dataset:
Paper: Successful Recovery of an Observed Meteorite Fall Using Drones and Machine Learning
Authors: Seamus L. Anderson, Martin C. Towner, John Fairweather, Philip A. Bland, Hadrien A. R. Devillepoix, Eleanor K. Sansom, Martin Cupák, Patrick M. Shober, Gretchen K. Benedix
Figure caption: The recovered meteorite as seen in person (top two panels), and from the survey drone (bottom panel). For scale, a 15 cm long felt pen is placed next to the meteorite (top right). The yellow box in the bottom image is 22 cm on one side.
Paper: Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train
Authors: Xinping Zhou, Yuandeng Shen, Ying D. Liu, Huidong Hu, Jiangtao Su, Zehao Tang, Chengrui Zhou, Yadan Duan, Song Tan
Figure caption: Panels (a)–(c) are time–distance stack plots respectively obtained from AIA 211, 193, and 171 Å running-difference images along sector S1 located in the quiet Sun. The white dashed lines in panels (a)–(c) point to the positions where the intensity profile is used to analyze the periodicities of the wave train, while the black dashed lines indicate the location of the BP. Panels (e)–(g) are running- (panels (e) and (f)) and base-difference (panel (g)) images created along sectors S2 and S3, in which the black dashed lines mark the location of the far-side CH boundary, and the inset in panel (e) is an enlarged view of the wave train inside the CH. Panels (d) and (h) show the evolution of two refracted waves propagated along sectors S4 and S5. The speeds in the different stages are listed in each corresponding panel with different colors.
Paper: Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train
Authors: Xinping Zhou, Yuandeng Shen, Ying D. Liu, Huidong Hu, Jiangtao Su, Zehao Tang, Chengrui Zhou, Yadan Duan, Song Tan
Figure caption: Panels (a) and (b) are the RHESSI hard X-ray fluxes and normalized light curves within the eruption source region as outlined by the white box in Figure 1(b) measured from different AIA channels, respectively. Panel (c) shows the GOES 1–8 Å flux (purple) and its derivative curve (red). The middle column (panels (d1)–(d3)) shows the power maps of detrended intensity profiles along the horizontal white dashed lines as shown in Figures 3(a)–(c), while the right column (panels (e1)–(e3)) shows the wavelet power maps of RHESSI hard X-ray fluxes in the energy band of 12–100 keV. In each wavelet power map, the period is highlighted by a white horizontal dashed line, and the corresponding period P is also listed in the figure.
Paper: Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train
Authors: Xinping Zhou, Yuandeng Shen, Ying D. Liu, Huidong Hu, Jiangtao Su, Zehao Tang, Chengrui Zhou, Yadan Duan, Song Tan
Figure caption: Panel (a) shows the running-difference time–distance stack plot of 193 Å along a rectangular slice (not shown here) that tracked the angular bisector of sector S1. Note that the starting point of the y-axis is not at the flare kernel. Panel (b) shows the profile of the wave front at 07:35 UT, indicated as the vertical white line in panel (a), in which the red plus signs, corresponding the location of the red plus signs in panel (a), mark the positions of the trough at a distance of 50, 108, and 166 Mm, respectively. The blue curve in panel (b) is the result of fitting the wave profile using the harmonic function, which shows the wavelength of 58 Mm. Panel (c) shows the time profile of the relative amplitude extracted from the position 50 Mm in a base-difference stack plot, as shown in panel (a). Panel (d) shows the variation in density (green) and temperature (orange) estimated in the region outlined by the red box in Figure 1(b) using the DEM version developed by Hannah & Kontar (2012). The percentage increase in density and temperature due to the wave’s passage and the magnetosonic Mach number estimated using Equation (4) are shown in the figure.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Same as Figure 3 but for the thick model with a surface layer gas-to-dust ratio of 105.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Same as Figure 3 but for the thick model with a surface layer gas-to-dust ratio of 104.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Same as Figure 3 but for the thin model with a surface layer gas-to-dust ratio of 104.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Gas temperature (left) and water abundance (right) for the thin model with a surface layer gas-to-dust ratio of 105 for variations in the chemical and heating–cooling models. The vertical blue lines show the midplane H2O snow-line location in the model. Above a z/r of ∼0.2, hydrogen is dominantly in atomic form and the gas is hot (>1000 K). Below this, models show a warm layer where the gas and dust temperatures are strongly decoupled, but the gas is molecular (region enclosed in the white box). This layer is critical for the inner disk emission. The gas in this layer is heated by UV photons, as such, water UV-shielding cools down this layer, while extra chemical heating leads to higher temperatures. In the right panels, the orange line shows the continuum τ = 1 line at 17 μm, and the red contours show the origin of 90% of the 113,9–100,10 17.2 μm water-line flux. Including the effect of water UV-shielding strongly increases the abundance of H2O between a z/r of 0.1 and 0.15 at radii >0.3 au.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Gas temperature as a function of the cumulative vertical H2O column at the location of the midplane H2O ice line (0.4 au). The H2O column is a proxy for the location in the disk, the higher column being deeper into the disk. Due to the different abundance profiles in the models these H2O columns map to different total gas columns for the different models. Solid and dashed–dotted lines show the gas-temperature profiles, and the dotted lines show the dust temperature. The black star with the error bar gives the range of columns and excitation temperatures extracted from the Spitzer-IRS spectra (Salyk et al. 2011). The vertical orange line shows the approximate location where the dust becomes optically thick at 17 μm. Up to a column of 1017 cm−2, the standard DALI and the water UV-shielding models are indistinguishable. At higher water columns, the shielding of H2O kicks in and heating by UV photons is suppressed.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Water spectrum over most of the JWST-MIRI observable range for the thin model with a gas-to-dust ratio of 105 in the surface layers (blue). The spectrum between 5 and 8 μm (left) is convolved to a resolving power of R = 3000, comparable to MIRI, the 10–28 μm spectrum on the right is convolved to an R = 600, to ease comparison with Spitzer spectra. The orange spectrum shows a water spectrum as computed from a typical slab model (Salyk et al. 2011), with an excitation temperature of 500 K and a H2O column of 3 × 1018 cm−2. In the Spitzer range, the model standard DALI and water UV-shielding models underpredict the H2O flux, except for the 10–12 μm regions. The extra heating models, however, overestimate the H2O flux, but the model with both extra heating and water UV-shielding fits the slab model better than the model with just water UV-shielding.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Gas density (left) and dust temperature (right) for the different gas and dust structures. The top row shows the thin model (h  c  = 0.08), and the bottom row shows the thick model (h  c  = 0.16). The gas-to-dust ratio in the surface layers after settling the large dust is denoted in the top left of the dust temperature panels. Orange lines show the continuum τ = 1 line at 15 μm for the g/d = 104 (solid) and 105 (dashed) dust distributions.
Paper: Water UV-shielding in the Terrestrial Planet-forming Zone: Implications from Water Emission
Authors: Arthur D. Bosman, Edwin A. Bergin, Jenny Calahan, Sara E. Duval
Figure caption: Same as Figure 2 but for the thick model with a surface layer gas-to-dust ratio of 105.
Paper: Detection of Stellar-like Abundance Anomalies in the Slow Solar Wind
Authors: David H. Brooks, Deborah Baker, Lidia van Driel-Gesztelyi, Harry P. Warren, Stephanie L. Yardley
Figure caption: Top panels: SOHO/MDI full solar disk magnetograms with accompanying photospheric continuum images (colored insets). We show the longitudinal magnetic field in the solar photosphere at the times of the likely departure of the back-mapped solar wind of the events in 2002, 2003, and 2006, with the red circles indicating the likely source regions. These images highlight the complexity of the magnetic field on the Sun during the IFIP events. White indicates positive polarity, and black indicates negative polarity. The images are scaled from −500 to 500 G. Bottom panels: open coronal magnetic field lines taken from the PFSS model for each active region (AR 10119, 10484, and 10923). The blue field lines indicate negative polarity, and the pink field lines represent positive polarity magnetic field. The grayscale images are reduced-resolution MDI full-disk observations of the longitudinal magnetic field in the solar photosphere with white showing positive polarity and black showing negative polarity, scaled from −200 to 200 G.
Paper: Detection of Stellar-like Abundance Anomalies in the Slow Solar Wind
Authors: David H. Brooks, Deborah Baker, Lidia van Driel-Gesztelyi, Harry P. Warren, Stephanie L. Yardley
Figure caption: Solar wind velocity, interplanetary magnetic field direction, and Fe/O ratios during the IFIP events. Top panel: He++ velocity measured by SWICS in situ around the time period of the three IFIP events shown in Figure 2. Middle panel: B  x  measured by ACE/MAG in situ around the time period of the three IFIP events shown in Figure 2. Bottom panel: the three IFIP events in Figure 2 plotted for ease of cross-reference. We show all the data on a common timescale that corresponds to the ranges in Figure 2.
Paper: Detection of Stellar-like Abundance Anomalies in the Slow Solar Wind
Authors: David H. Brooks, Deborah Baker, Lidia van Driel-Gesztelyi, Harry P. Warren, Stephanie L. Yardley
Figure caption: ACE/SWICS measurements of Fe/O normalized to their photospheric ratio. The data were obtained between 1998 February and 2011 August. The red solid line indicates the level we have defined for IFIP detection. Whether the measurements fall below this level depends on the assumed photospheric Fe/O abundance, and these vary in the literature, so for reference, we also show the threshold that would need to be reached if a more extreme lower value is chosen (see Section 2).
Paper: Detection of Stellar-like Abundance Anomalies in the Slow Solar Wind
Authors: David H. Brooks, Deborah Baker, Lidia van Driel-Gesztelyi, Harry P. Warren, Stephanie L. Yardley
Figure caption: Elemental abundance ratios compared to the ponderomotive force model. Fe/O, Fe/Si, and Fe/Mg abundance ratios measured by SWICS in situ in the solar wind during the 2003 October IFIP event and normalized to their photospheric abundance ratios. We compare the measurements to theoretical values predicted from the ponderomotive force model of IFIP due to Laming (2015). We show the theoretical predictions for two different values of the fast-mode wave amplitude in the models. Measurement uncertainties are shown by the error bars.
Paper: Detection of Stellar-like Abundance Anomalies in the Slow Solar Wind
Authors: David H. Brooks, Deborah Baker, Lidia van Driel-Gesztelyi, Harry P. Warren, Stephanie L. Yardley
Figure caption: IFIP events detected in the solar wind by ACE/SWICS. Fe/O abundance ratios measured by SWICS in situ in the solar wind normalized to their photospheric abundance ratio. Measurement uncertainties are shown by the error bars. The red solid and dashed lines correspond to the same levels as shown in Figure 1. We removed all data flagged as poor/marginal quality or missing due to numerical errors, low statistics, or anomalous operations.
Paper: Multipoint Analysis of the Interaction between a Shock and an ICME-like Structure around 2011 March 22
Authors: Mengjiao Xu, Chenglong Shen, Can Wang, Yutian Chi, Zhihui Zhong, Yuming Wang
Figure caption: Left: magnetic field measurements by VEX from 2011 March 21 to 24. The overlying green dashed lines are the fitting results of the force-free model. The gray and yellow shaded regions represent an ICME-like structure (ICMELS) and an ICME, respectively. The vertical black line and orange line indicate two fast forward shocks. Right: the black solid curves are the magnetic field and solar wind measurements by STEREO-A from 2011 March 22 to 25. The red solid lines between the orange solid vertical line and the orange dashed vertical line in panels (g)–(n) represent the recovered states of the S-ICMELS complex structure. The overlaid green and blue dashed lines in panels (g)–(l) show the fitting results of the force-free model. The ICMELS and the ICME are indicated by gray and yellow shaded regions. The vertical black and orange solid lines indicate the two fast forward shocks, and the vertical orange dashed line shows the recovered trailing edge of the ICMELS.
Paper: Multipoint Analysis of the Interaction between a Shock and an ICME-like Structure around 2011 March 22
Authors: Mengjiao Xu, Chenglong Shen, Can Wang, Yutian Chi, Zhihui Zhong, Yuming Wang
Figure caption: Positions of Earth, STEREO-A, STEREO-B, and Venus on March 22, 2011.
Paper: Multipoint Analysis of the Interaction between a Shock and an ICME-like Structure around 2011 March 22
Authors: Mengjiao Xu, Chenglong Shen, Can Wang, Yutian Chi, Zhihui Zhong, Yuming Wang
Figure caption: Left: the distribution of the calculated shock directions θ BN (top) and magnetic compression ratios (bottom) of shock 2 at VEX by selecting different upstream and downstream intervals. The shock direction θ BN is fitted with the magnetic coplanarity method. Right: the distribution of the calculated shock directions θ BN (top) and magnetic compression ratios (bottom) of shock 2 at STEREO-A by selecting different upstream and downstream intervals. The shock direction θ BN is fitted with the mixed-mode method. In all subplots, the horizontal coordinate represents the selected downstream intervals, the time period (in minutes) after the shock. The ordinate represents the selected upstream intervals, the time period (in minutes) before the shock.
Paper: Multipoint Analysis of the Interaction between a Shock and an ICME-like Structure around 2011 March 22
Authors: Mengjiao Xu, Chenglong Shen, Can Wang, Yutian Chi, Zhihui Zhong, Yuming Wang
Figure caption: Superposed epoch plot of the ICMELS observed by VEX, together with the observation and recovered state of S-ICME observed by STEREO-A.
Paper: Misaligned Spinning Binary Black Hole Mergers in Hot Magnetized Plasma
Authors: Federico Cattorini, Sofia Maggioni, Bruno Giacomazzo, Francesco Haardt, Monica Colpi, Stefano Covino
Figure caption: Top left: time-dependent accretion rates ﹩\dot{M}﹩ in units of solar masses per year for the five configurations. The magnitudes of ﹩\dot{M}﹩ are scaled to a binary of total mass 106 M ⊙ and a gas with an initial uniform rest-mass density ρ = 10−11 g cm−3. The premerger accretion rate is calculated onto both BH horizons; the postmerger accretion rate is calculated onto the remnant Kerr BH horizon. The dashed lines mark the merger times, and colors highlight the different configurations. Top right: comparison of ﹩\dot{M}﹩ in the late inspiral, merger, and postmerger stages; time is rescaled with the merger time t merger. Bottom left: time evolution of the Poynting luminosity L Poynt for the five configurations. The luminosity is extracted on a sphere of radius R ext = 30 M centered on the origin of the system. The values of L Poynt are in units of ﹩{L}_{0}\equiv 2.347\,\times \,{10}^{43}{\rho }_{-11}{M}_{6}^{2}﹩ erg s−1, with M 6 ≡ M/106 M ⊙, and ρ −11 ≡ ρ/1011 g cm−3. Bottom right: comparison of L Poynt in the late inspiral, merger, and postmerger stages.
Paper: Misaligned Spinning Binary Black Hole Mergers in Hot Magnetized Plasma
Authors: Federico Cattorini, Sofia Maggioni, Bruno Giacomazzo, Francesco Haardt, Monica Colpi, Stefano Covino
Figure caption: Top row: evolution of the rest-mass density ρ (normalized to its initial value ρ 0) on the xz-plane. Middle row: evolution of the fluid velocity field ﹩\vec{v}﹩ on the xz-plane. The color bar refers to the magnitude ﹩v={({v}_{x}^{2}+{v}_{z}^{2})}^{1/2}﹩. Arrows refer to the gas velocity field. Bottom row: evolution of the magnetic field lines on the xz-plane. The color bar refers to the magnetic-to-gas pressure ratio β −1. The regions inside the BH horizons have been masked out. All snapshots refer to our UUMIS configuration (﹩{\hat{a}}_{1}=(-0.42,0,+0.42)﹩, ﹩{\hat{a}}_{2}=(+0.42,0,+0.42)﹩, ﹩{\beta }_{0}^{-1}=0.31﹩); snapshots were taken, respectively, after ∼one orbit (left column), after ∼eight orbits (middle column), and at a time equal to ∼1000 M after merger (right column). The white arrows over the BHs in the left and middle columns denote spin vectors.
Paper: Misaligned Spinning Binary Black Hole Mergers in Hot Magnetized Plasma
Authors: Federico Cattorini, Sofia Maggioni, Bruno Giacomazzo, Francesco Haardt, Monica Colpi, Stefano Covino
Figure caption: Top left: GW strain of the UUMIS run extracted via the Weyl scalar Ψ4 with the WeylScal4 thorn and normalized to its maximum value at merger. Top right: time-dependent premerger mass accretion rate ﹩{\dot{M}}^{* }=\dot{M}-{p}_{6}﹩ over both BH horizons for the UUMIS run, also normalized to its maximum value. Bottom left: time-frequency representation of the GW strain via WPSD, showing the frequency increase of the signal over time. Bottom right: time-frequency representation of ﹩{\dot{M}}^{* }﹩ via WPSD, showing a similarity with the GW strain in the frequency increase over time. Time and frequency units are normalized to a binary system with total mass M = 106 M ⊙, and M 6 ≡ M/106 M ⊙.
Paper: Misaligned Spinning Binary Black Hole Mergers in Hot Magnetized Plasma
Authors: Federico Cattorini, Sofia Maggioni, Bruno Giacomazzo, Francesco Haardt, Monica Colpi, Stefano Covino
Figure caption: Top row: evolution of the rest-mass density ρ (normalized to its initial value ρ 0) on the xy-plane for the UUMIS configuration (﹩{\hat{a}}_{1}=(-0.42,0,+0.42)﹩, ﹩{\hat{a}}_{2}=(+0.42,0,+0.42)﹩, ﹩{\beta }_{0}^{-1}=0.31﹩); snapshots were taken, respectively, after ∼one orbit (left), after ∼11 orbits (center), and at the time of merger (right). Bottom row: close-ups at the same epochs as the top panels of the region in the vicinity of the first BH’s apparent horizon (left and middle panels) and of the remnant BH (right panel). Arrows denote velocity vectors. The black circles denote the interior of the apparent horizons. In the top panel, a colored dot is added inside the BH with initial spin ﹩{\hat{a}}_{1}﹩.
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Dust density vs. distance for three different LOSs toward the California cloud (overplotted in Figure 2). The black line shows the mean, and the shading represents one standard deviation (also computed by the Gaussian process model). The red curve is toward the lowest part of the bubble, the blue curve represents the elongated length of the sheet, and the gray curve shows the density for an LOS toward the left (eastern) end of the cloud. The density in the secondary axis is calculated assuming N  H (cm−2) = 2 × 1022 A  K , which is an average value for the hydrogen column density in the literature (e.g., Reina & Tarenghi 1973; Gorenstein 1975; Predehl & Schmitt 1995; Güver & Ozel 2009).
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: 3D dust density predictions for the California cloud projected from the y-axis (left panel) and the z-axis (right panel) (perpendicular to the Galactic plane). More angles can be seen in the Appendix A (Figure 6). The color represents densities in K  s -band magnitude per parsec. The Sun is at (0,0,0) and X increases toward the Galactic Cent. The dotted lines demonstrate what we refer to as a sheet. The predictions are made on regular grids for every 0.5° in the Galactic l and b, and every 5 pc in distance. The 3D image is then produced by applying a smoothing kernel to handle the missing pixels. In order not to produce extra smoothing from that of the method, the length scale of the smoothing kernel is chosen to be much smaller (3 pc) than the correlation length. For illustration purposes, values below 0.0005 are set to be transparent. For N  H (cm−2) = 2 × 1022 A  K , the dust density of 0.001 mag pc−1 corresponds to a gas volume density of ∼6 cm−3 (see Figure 3).
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Dust density predictions in the plane of the sky. Each panel represents a slice through the cloud at fixed distances (every 20 pc). The bubble on the right side is apparent at the 455 pc slice, while the rest of the cloud is seen through multiple panels demonstrating the extent of the sheet, especially toward (l, b) = (161.5, −8.5). The three symbols (square, circle, and triangle) represent specific LOSs along the cloud investigated in Figure 3. For illustration purposes, the image is smoothed with the scale length of 0.4°. For N  H (cm−2) = 2 × 1022 A  K , the dust density of 0.001 mag pc−1 corresponds to a gas volume density of ∼6 cm−3.
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Two projected views of the 3D distribution of dust toward the California and Orion A clouds. The Sun is at (0,0,0), the z-axis is perpendicular to the Galactic plane, and X increases toward the Galactic center. For illustration purposes, values below 0.0005 are set to be transparent.
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Star formation surface density as a function of mass surface density (Kennicutt–Schmidt relation) for the local molecular clouds from Lada et al. (2013). The red arrow shows how the location of a cloud like California would change on this diagram when seen from an angle perpendicular to the LOS.
Paper: Three-dimensional Shape Explains Star Formation Mystery of California and Orion A
Authors: Sara Rezaei Kh., Jouni Kainulainen
Figure caption: Reconstructed extinction using the 3D density predictions (in the K  s  band). Extinctions are calculated using the sum of the predicted 3D densities along each LOS. The 2D representation of the 3D predictions nicely recover the plane-of-the-sky features of California. The dashed lines are contours of 0.3 mag extinctions from Green et al. (2019) using the “dustmaps” interface of Green (2018). For consistency, the second map is smoothed to the same resolution as our map.