adsabs/AstroCLIMB huggingface dataset:
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: In-situ observations by STEREO A on 2019 April 9. From top to bottom: omnidirectional 45–55 keV electron intensities, sectored intensities measured by the four telescopes of the STEREO/SEPT instrument (both using 10 minute averaging, respectively). Pitch angles scanned by the central axes of these four telescopes. Magnitude and components of the magnetic field vector in the spacecraft-centered RTN coordinate system. Pitch-angle distribution of suprathermal electrons at 246.6 eV (color for the logarithm of phase space density). Solar wind proton temperature, density, and speed. Distribution of iron charge states Q Fe as measured by STEREO A/PLASTIC. The yellow shaded period indicates a period with peculiar field direction studied in detail. The gray shaded bar and dashed lines, respectively, mark the onset of the SEP event (12:40-12:50 UT), magnetic sector boundary crossing (13:08 UT), and return of electron flux to background levels (15:00 UT).
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: Instantaneous ecliptic positions of the spacecraft constellation used in this work at 12:00 UT on 2019 April 9, expressed in Stonyhurst coordinates (Sun–Earth line at 0° longitude). Each spacecraft is connected back to the Sun by a 400 km s−1 reference Parker spiral. A black arrow and black dashed Parker spiral indicates the longitude and nominal trajectory of emission from AR 12738. Note the “Earth” location is a proxy for the locations of the Wind/WAVES, GOES-15/XRS, and LOFAR instruments. Figure generated using https://solar-mach.github.io.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: (a) Type III radio burst sources observed by LOFAR from 20 to 80 MHz overlaid on a PFSS magnetic field extrapolation using GONG magnetograms. The type III sources emanate from the active region near the east limb and are situated close to the negative open magnetic field rooted in the active region. (b) Deprojection of the radio sources using a Newkirk density model (Newkirk 1961), assuming emission at the second harmonic of the local plasma frequency. This places the radio sources on the open field lines ∼40°, which appear to originate from AR 12738. This agrees well with the trajectory of the radio sources in Figure 6. In panel (b), field-line tracing is performed with a higher density of grid points over a smaller area, hence more open field lines are resolved.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: TDOA localization in the ecliptic plane of a type III radio burst trajectory in the inner heliosphere as measured by PSP, WIND, and STEREO A. The solid markers in the bottom panel represent the central value, while the diffuse cloud shows the position uncertainty due to the impact of the instrument time resolution on the time-of-flight measurement, both colored based on the measured frequency. The LOFAR deprojections are visible for comparison in the zoomed in bottom panel. The coordinate frame is the Heliocentric Earth ecliptic (HEE).
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: Proposed schematic of stream structure at STEREO A during the time interval studied (yellow shading in Figure 7). STEREO A/SEPT FOVs indicated by the two black triangles. The red and blue lines show the kinked field lines of opposing polarities. The nominal Parker spiral is indicated by the green dotted curve. The purple ellipses with arrows indicate electron beams injected onto these field lines. The gray solid arrows indicate the proposed flow velocity across the kink and the overall advection direction of the structure.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: Schematic of the time-delay-of-arrival localization method and associated error region. The top panel shows a synthetic example using the positions of STEREO A/B and Wind in 2013 to clearly show how the hyberbola intersection defines the error region. The bottom panel shows the specific geometry for the event in this study using the measured time delays at 1.04 MHz. Each panel shows in the HEE frame: the spacecraft geometry, the hyperbola generated from each pair of time delays, the resulting source centroid, and the error region. The annotations on the plot also include the position of the Sun, and the dotted circle indicates 1 au.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: Example radio flux vs. time profile and onset extraction example. Each profile is normalized by its maximum value so they can be shown on the same axes. Profile is from the closest frequency channel to 0.96 MHz in each spacecraft receiver. The red, blue, and black profiles, respectively, show the PSP/FIELDS/RFS, S/WAVES, and Wind/WAVES observations. Data points are shown explicitly to demonstrate the differing instrument resolutions.
Paper: Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Samuel T. Badman, Eoin Carley, Luis Alberto Cañizares, Nina Dresing, Lan K. Jian, David Lario, Peter T. Gallagher, Juan C. Martínez Oliveros, Marc Pulupa, Stuart D. Bale
Figure caption: Onset time feature extraction (blue) and quadratic fitting (red) to the type III burst studied in this work as observed by PSP, STEREO A, and Wind. The error bars show the instrument time resolution. Fitting is only done over the frequency range clearly observed in all three spacecraft.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Computed and literature BEs (in kelvin). For each species, the solid black line covers the min/max ZPE-corrected BE values for the amorphous ice model, while blue stars correspond to the ZPE-corrected BEs on the crystalline ice model.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Adsorption geometry of S-bearing vs. O-bearing species at P-ice (010) surface. Side view is at the top; the top view is at the bottom. Complexes on the right (O-bearing species) are adapted from Ferrero et al. (2020). Distances are given in angstrom units. (i) CH3SH vs. CH3OH; (ii) CS vs. CO.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: (a) Distribution of BEs computed on the amorphous ice model for S-bearing species (orange) and the species of Ferrero et al. (2020; blue). (b) Distribution of the dispersive (left panel) and nondispersive (right panel) contributions to the crystalline BEs for closed-shell species.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Adsorption geometry of S-bearing vs. O-bearing species at P-ice (010) surface. Side view is at the top; the top view is at the bottom. Adsorption complexes on the right (O-bearing species) are adapted from Ferrero et al. (2020). Distances are given in angstrom units. (i) H2S vs. H2O; (ii) adsorption geometry of OCS vs. CO2.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Analysis of ZPE corrections. Correlation between DFT//DFT BE(0) and BE for the adsorption at the crystalline ice. The intercept is set to zero.
Paper: Binding Energies of Interstellar Relevant S-bearing Species on Water Ice Mantles: A Quantum Mechanical Investigation
Authors: Jessica Perrero, Joan Enrique-Romero, Stefano Ferrero, Cecilia Ceccarelli, Linda Podio, Claudio Codella, Albert Rimola, Piero Ugliengo
Figure caption: Adsorption geometry of S-bearing vs. O-bearing species at P-ice (010) surface. Side view is at the top; the top view is at the bottom. Adsorption complexes on the right (O-bearing species) are adapted from Ferrero et al. (2020). Distances are given in angstrom units. (i) First and (ii) second adsorption geometry of H2CS vs. H2CO.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption:  M 200 (upper panels) and σ cl (lower panels) for simulated clusters (the dashed line and the shaded region) in five zero redshift mass subsamples as a function of redshift. Red circles show the observed HeCS-omnibus clusters.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Redshift evolution of the (a) BCG stellar mass (M *,BCG) and (b) BCG stellar velocity dispersion (σ *,BCG) to cluster mass (M 200) relations. Lines connect the median values computed for each redshift snapshot. Different colors indicate the relations derived for each mass subsample. Redshift evolution of (c) M*,BCG and (d) σ *,BCG as a function of BCG total mass. Line colors are the same as in (a) and (b).
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Evolution of BCG physical properties including (a) R *,h , (b) ﹩\mathrm{log}{M}_{* ,h}﹩, and (c) σ *,BCG as a function of redshift for z < 2. The dashed lines indicate the median evolution; the shaded regions show the 1σ distribution. The lower row displays the normalized evolution of (d) R *,h /R *,h (z = 0), (e) M *,h /M *,h (z = 0), and (f) σ *,BCG/σ *,BCG(z = 0).
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: (a) Median distribution of σ *,BCG/σ cl as a function of median σ cl for clusters in the five mass subsamples; different colors indicate the mass subsamples. Individual points are derived from the redshift snapshots for z < 2. From left to right, the systems evolve from z = 2 to z = 0. For direct comparison, we normalize the x-axis (σ cl) by the σ cl at z = 0. (b) Median σ *,BCG/σ cl of the clusters in mass subsamples as a function of redshift.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Cluster and BCG velocity dispersion as a function of M 200. Blue circles show σ cl and yellow squares show σ *,BCG. Dashed and dotted lines display the best-fit relations; each panel lists the slopes.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: The σ *,BCG/σ cl ratio as a function of σ cl. Circles show individual clusters color coded by their mass at z = 0; a darker color indicates a more massive cluster at the current epoch. Red dashed lines and the shaded regions mark the best fit and the scatter derived from the MCMC approach. For comparison, black dotted lines display the relation at z = 0.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Redshift evolution of σ *,BCG − σ cl relation for five randomly selected simulated clusters. In each panel, clusters evolve from z = 2 to z = 0 (from left to right). Spikes at some redshifts reflect a change in σ *,BCG resulting from dynamical interaction with neighboring galaxies. Red vertical lines indicate the occurrence of a major merger.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: The M * (upper panels) and the σ *,BCG (lower panels) of simulated BCGs (the dashed line and the shaded region) in five mass subsamples as a function of redshift. Red circles show the observed HeCS-omnibus clusters.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Redshift evolution of (a) R 200, (b) M 200, and (c) σ cl of 270 simulated cluster halos. Different colors indicate the mass subsamples (shown in (b)) from Table 1. The shaded regions show the 1σ distribution; the dashed lines indicate the median evolution. (d)–(f) are the same as (a)–(c), but y-axes show the normalized size, mass, and velocity dispersion relative the same quantities measured at z = 0.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: (a) R 200, (b) M 200, and (c) σ  cl,200 distributions of 270 massive clusters in TNG300 at z = 0. Vertical lines in (b) show the boundaries we use for constructing mass subsamples.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Distributions of (a) half mass–radius (R *,half,0), (b) stellar mass within the half mass–radius (M *,h ), and (c) stellar velocity dispersion of the BCGs (﹩{\sigma }_{* ,\,\mathrm{BCG},\,{{\rm{R}}}_{\mathrm{half}}}﹩) in 270 massive clusters at z = 0.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: Mean density distribution of stellar particles belonging to the most massive cluster in IllustrisTNG-300 z = 0 snapshot. The darker color indicates higher density. Two circles indicate the R 200 and 2R200 of the cluster halo.
Paper: Informing the Cataclysmic Variable Sequence from Gaia Data: The Orbital-period–Color–Absolute-magnitude Relationship
Authors: Ellianna S. Abrahams, Joshua S. Bloom, Paula Szkody, Hans-Walter Rix, Nami Mowlavi
Figure caption: Triangle plot: the posterior distributions of the model parameter fits for Equation (1) from both DR2 and EDR3. The median estimates for each coefficient lie within the 90% confidence intervals from each release, illustrating the stability of the fit when the underlying photometry is sampled at a sparser rate. Inset panel: the CAMD positions of the 23 objects in the sample that moved more than 10% in color space and/or M  G  space on the CAMD. While most of these CVs appear to just migrate in color space, a smaller fraction grow orders of magnitude fainter in the G band in EDR3. This likely means that a significant fraction of their DR2 observations were caught in outburst over the 22 months of DR2, and as the mission releases photometry based on a longer baseline, we expect that more of their quiescent emission will contribute to the G-band measurement.
Paper: Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids
Authors: Zehao lin, Ye Xu, Chaojie Hao, Dejian Liu, Yingjie Li, Shuaibo Bian
Figure caption: Examples of DCEP and OC combinations. (a) Example of the DCEPs CS Vel and the OC Ruprecht 79, showing the spatial distribution (top right), the proper-motion distribution (bottom right), and the color–magnitude diagram (left). The gray dots are the member stars of the OC, and the red asterisks represent the DCEPs. (b) The same distributions for the DCEP OGLE-GD-CEP-1175 and the OC NGC 6193. In the color–magnitude diagram in panel (b), OGLE-GD-CEP-1175 is fainter than the turnoff point of its OC.
Paper: Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids
Authors: Zehao lin, Ye Xu, Chaojie Hao, Dejian Liu, Yingjie Li, Shuaibo Bian
Figure caption: PW relation of the OC-DCEP candidates in the G bands. From left to right, the top three panels are: (a) the PW relations obtained by fitting the F+1O-mode OC-DCEP candidates, where the distances are adopted from the cluster-averaged parallaxes; (b) the DCEP parallaxes; and (c) the DMs, respectively. The bottom three panels are similar to the top panels, but the PW relations were obtained by fitting just the F-mode OC-DCEP candidates. The gray dots represent the extended OC-DCEP candidate sample with several dimensions more than 3σ, but less than 4σ, in the five-dimensional parameter space.
Paper: Informing the Cataclysmic Variable Sequence from Gaia Data: The Orbital-period–Color–Absolute-magnitude Relationship
Authors: Ellianna S. Abrahams, Joshua S. Bloom, Paula Szkody, Hans-Walter Rix, Nami Mowlavi
Figure caption: Figure 7 is further disambiguated with more specific CV subtypes in each taxonomical category. Where sources lack more specific subclassifications, their initial symbols from Figure 7 are left in place. Systems that are outliers in either color or P orb–M  G  space are labeled for further discussion.
Paper: Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids
Authors: Zehao lin, Ye Xu, Chaojie Hao, Dejian Liu, Yingjie Li, Shuaibo Bian
Figure caption: The deviation between the observed ﹩{W}_{{G}_{\mathrm{obs}}}﹩ and the W  G  obtained from the PW relation (i.e., ﹩{\rm{\Delta }}W={W}_{{G}_{\mathrm{obs}}}-{W}_{G}﹩) and distance, where the different colors denote the colors of the OC-DCEP candidates. The samples with and without using parallax zeropoint correction are shown in panels (a) and (b), respectively.
Paper: Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids
Authors: Zehao lin, Ye Xu, Chaojie Hao, Dejian Liu, Yingjie Li, Shuaibo Bian
Figure caption: Comparison between the OC-DCEP distances as provided by Skowron et al. (2019), D  S , and as obtained by cluster-averaged parallaxes after considering a parallax zeropoint correction. The dashed line corresponds to the identity line.
Paper: Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids
Authors: Zehao lin, Ye Xu, Chaojie Hao, Dejian Liu, Yingjie Li, Shuaibo Bian
Figure caption: Left: comparison of the distances between adopting the cluster-averaged parallax and using the individual DCEP parallaxes. Middle: comparison of the distances between the cluster-averaged parallaxes and the DMs. Right: comparison between the DCEP parallax distances and the DM distances. The dashed line corresponds to the identity line.
Paper: Informing the Cataclysmic Variable Sequence from Gaia Data: The Orbital-period–Color–Absolute-magnitude Relationship
Authors: Ellianna S. Abrahams, Joshua S. Bloom, Paula Szkody, Hans-Walter Rix, Nami Mowlavi
Figure caption: Representative Gaia Alerts light curves of NLs in the VSX-Gaia gold sample. We find that Gaia's rejection thresholding completely removes high and low states from NL photometry; however, this statement cannot be shown to be robust across all NLs, as our sample size is only three sources.
Paper: Different Degrees of Nitrogen and Carbon Depletion in the Warm Molecular Layers of Protoplanetary Disks
Authors: Kenji Furuya, Seokho Lee, Hideko Nomura
Figure caption: An outline of the modeling processes.
Paper: Different Degrees of Nitrogen and Carbon Depletion in the Warm Molecular Layers of Protoplanetary Disks
Authors: Kenji Furuya, Seokho Lee, Hideko Nomura
Figure caption: Vertical physical structures of a disk at R = 20 au (left panels) and 80 au (right panels) as functions of Z/R. (a), (b) Gas density. (c), (d) Dust-to-gas mass ratio for the eight dust populations. Black dashed lines represent the sum of the dust-to-gas mass ratio for the eight dust populations. (e), (f) Total cross section for the eight dust populations per hydrogen nuclei. For comparison, when the size of all dust grains is 0.1 μm and the dust-to-gas mass ratio is 0.01, the total cross section is ∼3 × 10−22 cm−2 per hydrogen nuclei.
Paper: Different Degrees of Nitrogen and Carbon Depletion in the Warm Molecular Layers of Protoplanetary Disks
Authors: Kenji Furuya, Seokho Lee, Hideko Nomura
Figure caption: Vertical distributions of the abundances of selected species with respect to hydrogen nuclei at R = 20 au (left panels) and 80 au (right panels) at 1 Myr. The top, middle, and bottom panels show the static model (i.e., only chemistry is considered), the model without grain surface chemistry, and our full model, respectively. Gas-phase species are shown by solid lines, while icy species are shown by dashed lines. For icy species, the total abundances (i.e., the sum of the ice abundances on eight dust populations) are shown.
Paper: Different Degrees of Nitrogen and Carbon Depletion in the Warm Molecular Layers of Protoplanetary Disks
Authors: Kenji Furuya, Seokho Lee, Hideko Nomura
Figure caption: Abundances (top) and depletion factors (bottom) of elemental carbon (red lines) and nitrogen (blue lines) above the snow surfaces of CO and N2, respectively, in the static model (left), the model without grain surface chemistry (middle), and in the full model (right) at 0.1 Myr, 0.3 Myr, and 1 Myr. The depletion factors monotonically increase with time.