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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: Similar to Figure 2, but for temperatures and UV/X-ray radiation fields. (a), (b) Gas temperature (dashed black line) and dust temperature for the 8 dust populations (solid lines). (c), (d) Wavelength-integrated FUV flux normalized by the Draine field (1.6 × 10−3 erg cm−2 s−1; Draine 1978) (red) and the X-ray ionization rate normalized by the nonattenuated CR ionization rate, which is set to 10−18 s−1 (black).
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: Radial profiles of the total abundances of selected icy molecules (i.e., the sum of the ice abundances on eight dust populations) in the static model (left), in the full model with α = 10−4 (middle), and in the full model with α = 10−3 (right) at 1 Myr. Arrows on the right-hand margin indicate the initial abundances of H2O, CO, and N2. The abundance of NH3 is below 10−6 and not shown in the figure.
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: Depletion factors of elemental carbon (red solid lines) and nitrogen (blue solid lines) in the full model with α = 10−2 (left) and with α = 10−4 (right) at 1 Myr. Dashed gray lines represent the depletion factors in the model with α = 10−3 at 1 Myr for comparisons. The dotted lines in the left panel show the depletion factors in the model with α = 10−2 at 0.1 Myr.
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: Radial profiles of the column densities of selected gas-phase molecules in the full model at 0.1, 0.3, 1, and 3 Myr. The column densities at 3 Myr are shown only at R = 50, 80, and 100 au. At the inner radii, the column density almost reaches the steady-state values within 1 Myr. For comparisons, black dashed lines show the column densities predicted by the static model without grain surface chemistry (i.e., no depletion of carbon and nitrogen in the warm molecular layers) at 1 Myr.
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: The depletion factors of elemental carbon (red solid line) and nitrogen (blue solid line) in the model where the initial H2O-to-dust mass ratio is uniform inside the disk at 1 Myr. For comparisons, dashed lines and dotted lines represent the depletion factors in the fiducial full model and the model without surface chemistry. In these two models, the initial H2O abundance is uniformly 10−4.
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: Radial profiles of abundances of selected icy molecules on small (0.1–0.32 μm), middle (3.2–10 μm), and large (0.32–1 mm) sized dust populations in the full model with α = 10−3 at 1 Myr.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: Panel (a) plots the Venus intensity, D V as a function of the solar-x position of Venus. Circles indicate positions above the limb, and crosses positions on the disk. Filled circles and diagonal crosses are additional points that were not part of the 20 minute cadence image series (see the main text). The cyan line is the Venus intensity after deconvolving the images. Panel (b) plots D V against the annular intensity, D ann. Symbols are the same as for panel (a). The cyan line is a straight line fit to only the crossed data points.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: An AIA 193 Å image from 2012 June 6, with Venus located at approximate position [40,590]. The track and direction of motion are indicated by the yellow line. A logarithmic intensity scaling has been applied to the image. The blue crosses show the locations of Venus as measured by EIS. The differences compared to the AIA track are due to the different orbits of the Hinode and SDO spacecraft (Section 6).
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: (Left) Vertical distribution of the gas-phase CO abundance in the fiducial model (solid line) and in the single-T  d  model (dashed line) at R = 80 au and at 1 Myr. In both models, grain surface chemistry is switched off. (Right) Adsorption rates of CO onto eight dust populations in the fiducial model are shown by dotted lines, while net adsorption rates (i.e., the adsorption rate of gas-phase CO minus the desorption rate of CO ice) are shown by solid lines.
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: Dependence of depletion factors of elemental carbon (red lines) and nitrogen (blue lines) on ﹩{a}_{\max }﹩ (left panel) and ﹩{a}_{\min }﹩ (right panel) at 1 Myr. In the left panel, the solid, dashed, and dotted lines represent the models with ﹩{a}_{\max }=1\,\mathrm{mm}﹩, 100 μm, and 10 μm, respectively. In the right panel, the solid and dashed lines represent the models with ﹩{a}_{\min }=0.1﹩                          μm and 0.01 μm, respectively.
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: Depletion factors of elemental carbon (red lines) and nitrogen (blue lines) in the model with the enhanced CR ionization rate ξ CR = 10−16 s−1 (solid lines) and the model with ξ CR = 10−18 s−1 (dashed lines). The left panel shows the static models, while the right panel shows the full models.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: An AIA 193 Å image from 04:00:06 UT on 2016 November 23, shown with a logarithmic intensity scaling. The cross denotes the location used as a check on the scattered light formula, the circles show the annular region used to estimate the short-range scattered light component.
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: Similar to Figure A2, but for R = 20 au. As R = 20 au is inside the CO snow line, only CO2 and H2O abundances 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 of CO2, CO, H2O, and N2 ices on eight dust populations at R = 80 au at 1 Myr in the full model.
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: Left panel: the CAMD for the VSX-Gaia crossmatch for CVs with P orb < 8 hr, indicated by the circles colored and sized according to P orb. For reference, the Gaia Catalogue of Nearby Stars (Gaia Collaboration et al. 2021b) is shown in gray. CVs primarily inhabit the space between the MS and the WD sequence. The relationship between the CAMD position and period is apparent on the CAMD, with longer-period CVs falling closer to the MS and shorter-period CVs falling closer to the WD sequence. Lines of constant P orb (from the model fit in Equation (1)) that enclose the CV period gap are shown as dotted red lines, along with their 5σ confidence bands. VSX CVs within the gap are indicated as triangles and are explored further in Figure 5. Right panel: full 2D representation of the Equation (1) model fit for P orb. The fit is only robust within the bounds of the data, and the intrinsic scatter, σ int, of the fit is indicated by random Gaussian noise of the pixel color. The dotted white lines indicate the bounds of the period gap.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: Panel (a) shows the Fe XII λ195.12 Venus intensity, I V, measured from EIS as a function of the solar-x position of Venus. Circles indicate positions above the limb, crosses positions on the disk, and triangles positions on the disk where a complete annular intensity, I ann, could not be measured. Panel (b) plots I V versus I ann. The solid line is the fit to the points inside the limb, and the dashed line is the fit from AIA data (Figure 2), normalized to cross the EIS line at I ann = 0.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: (a) An EIS λ195.12 image derived from a raster obtained between 00:39 and 00:41 UT. A logarithmic intensity scaling has been applied. The shadow of Venus is visible at an approximate position [−170, +550]. The black numbers identify the order of the six exposures that make up the raster. (b) A close-up from exposure 3 showing the Venus shadow with a linear intensity scaling. The white box identifies the region that yields I V. The region indicated by a vertical blue line is used to obtain I bg.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: Plots of the Venus Fe XIV λ274.20 intensity during the eclipse. An explanation of the symbols is given in Figure 5. The blue dashed line in panel (b) provides the linear fit from Fe XII λ195.12, scaled to intersect the λ274.20 fit (blue solid line) at I ann = 0.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: (a) an AIA 193 Å image with a logarithmic intensity scaling showing AR 11158. A blue cross marks the location at which the scattered light is estimated, and the concentric circles identify the annulus region used for assessing scattered light. (b) a synthetic intensity image for modeling scattered light. Black indicates a region of zero intensity, gray indicates quiet Sun emission, and white active region emission (see main text for details).
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: A raster image from EIS obtained between 03:08 and 05:15 UT on 2016 November 23 showing the intensity of Fe XII λ195.12 on a logarithmic scale. The dark region to the top right is part of a coronal hole, and the circles indicate the annular region used for obtaining the local scattered light component. The white box indicates the quiet Sun region used for normalizing the λ195.12 intensity with the AIA 193 Å channel.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: Comparisons of AIA annuli intensities for alternative choices of the annuli radii (﹩{D}_{\mathrm{ann}}^{* }﹩), with intensities for the original choice of annulus radii (D ann). Panels (a) and (b) show the results for reducing the inner radius to 10″ and 20″. Panels (c) and (d) show the results for increasing the outer radius to 70″ and 90″. Crosses/circles represent locations where Venus was inside/outside the solar limb.
Paper: Scattered Light in the Hinode/EIS and SDO/AIA Instruments Measured from the 2012 Venus Transit
Authors: Peter R. Young, Nicholeen M. Viall
Figure caption: Radial slices through synthetic AIA 193 and 304 Å images derived by convolving annulus intensity distributions with the PSFs of Grigis et al. (2012).
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: Different subclasses of CVs in the P orb–M  G  plane show how the data add a new dimension to the semiempirically derived donor sequence determined by Knigge et al. (2011) (shown as the dashed black line) that incorporate the physics from the WD primary and the accretion disk. The donor sequence was intended to provide a lower limit for absolute optical and NIR magnitudes as a function of P orb as derived from the theoretical donor parameters, such as donor mass or radius. An added color axis reveals that the offset from the minimum is correlated with color for DN and IP systems above the gap, with red systems generally being less luminous than blue systems in the same period bin. The data behind this Figure is available in machine-readable format.(The data used to create this figure are available.)
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: Estimated ﹩{\hat{P}}_{\mathrm{orb}}﹩ shown as a function of their distribution across binned measurements of P orb as provided by VSX. The inner 80th percentiles of ﹩{\hat{P}}_{\mathrm{orb}}﹩ at fixed measured P orb, symbolized in the black vertical lines within the violin distributions, indicate that generally our model estimates P orb within a few σ of the intrinsic scatter. Due to the lack of data with robust Gaia astrometry at longer P orb, the model underpredicts ﹩{\hat{P}}_{\mathrm{orb}}﹩ there. The sampling counts in each bin are annotated below the violin distributions (which are explained in the last paragraph of Section 2.2) and are shown in the histogram of VSX P orb in the upper panel. The violins in this figure are colored according to the fit shown in the right panel of Figure 1 to allow for easy comparison of the different fit visualizations.
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: Estimations of ﹩{\hat{P}}_{\mathrm{orb}}﹩ for the VSX sample shown for the model fit to the overall population (top panel), the population with accretion disks (DN, IP, NL; middle panel), and the residual between the estimate of P orb when fitted on the disked population and the population without disks (polars; bottom panel). The symbol colors and shapes indicate the underlying CV subtype. While the fit on the polar systems did not converge, we explore the central tendency of the fit to the population. We find that the fit on the overall population and on the CVs with disks still make reasonably accurate predictions of ﹩{\hat{P}}_{\mathrm{orb}}﹩ for polar systems, despite their lower sample size (n = 67) and therefore smaller influence on the overall fit. As discussed, CN below the gap fit poorly in all circumstances.
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: Gap CVs (2.15 < P orb < 3.18 hr) on the CAMD. The primary fit to ﹩{\hat{P}}_{\mathrm{orb}}﹩ for the limits of the gap is shown in the dotted lines, along with the 3σ confidence bands for those limits. The different subtypes are illustrated in the color and shape of the symbols. The fit to ﹩{\hat{P}}_{\mathrm{orb}}﹩ performs well across all CV subtypes, with the exception of a handful of outlying DNs, labeled here.
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: Three-dimensional view of the VSX CVs with P orb on the z-axis. CVs in the gap are shown as triangles. The change in slope, which describes the rapidity of a CV’s evolution to a tighter orbital period, of P orb ∼ M  G  + (G BP − G RP) above and below the gap is apparent in the data, even without a formal fit. The planar linear approximations above and below the gap are illustrated by best-fit planes, shown in purple above the gap and green below. The orientation for this figure is chosen to project the axis orthogonal to Equation (1), allowing the best-fit planes shown here to extend into the plane nearly orthogonal to this paper. The data are colored according to their P orb, with both data color and symbols (indicating gap CVs) following the same convention as Figure 1.
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: The CAMD location of different CV subtypes. The left-hand panel displays the most common types of CVs and DNs, while both magnetic CV flavors are shown in the middle panel: diskless polars and intermediate polars that generally show evidence of disks in their spectra. The right-hand panel shows NL CVs and classical novae. While some studies focus on volume-limited samples of CV populations as they fall on the CAMD, we choose to explore the positioning of our full catalog of VSX-Gaia because it contains greater representation of younger and therefore longer-period CVs. We show the subset of CVs within 300 pc in opaque and boldly stroked symbols, while more distant CVs are symbolized with semitransparent markers.
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 DNs in the VSX-Gaia gold sample. Following Gaia's 5σ clipping technique as outlined in Riello et al. (2018), we find that Gaia's rejection thresholding tends to select for observation epochs where DNs are in quiescence, as estimated by eye. Such systems are shown in the upper four panels of this figure, where rejected epochs are shown in light gray, and the median of the data is shown in the dashed line. Thresholding can remove outburst, superoutburst, and eclipsing epochs as long as the number of observations at quiescence is a majority portion of the observations. The bottom two panels show two DNs where the thresholding was unsuccessful at removing outbursting epochs, but despite this the reported measurement in EDR3 is fairly close to the quiescent magnitude in these cases, as is shown in the dotted black 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: DN populations above the gap, by type. The Z Cam types are shown in the blue histogram, and the SS Cyg types are shown in the red histogram. These types occupy distinct color spaces, with some overlap; however, the bluest systems are only Z Cam types, known to have high ﹩\dot{M}﹩, and the reddest systems are SS Cyg types, known to lack high ﹩\dot{M}﹩. This indicates that optical color above the gap is at least partially dependent on the accretion rate of the disk.
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 polars in the VSX-Gaia gold sample. We find that Gaia's rejection thresholding is less successful at removing high states in polars than in removing outburst in DNs.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: Flux tube geometries that could lead to the formation of δ-spots are shown: (a) An “island”-δ that is the first category of Zirin & Liggett (1987), also known as the “spot–spot” type by Toriumi et al. (2017), formed by a kink instability acting on a twisted, rising Ω-loop or convective buffeting; image reproduced from López Fuentes et al. (2000). (b) An inverted kink instability; reproduced from Poisson et al. (2013). Bottom row: two multisegment buoyant configurations with different subsurface connectivity; images reproduced from Toriumi et al. (2017), who named them (c) “spot satellite” and (d) “quadrupole.” These last two multisegment buoyancy configurations represent the second and third categories of Zirin & Liggett (1987). The configuration in panel (a) would appear in a magnetogram as a primarily bipolar magnetic configuration, whereas the other three would present as quadrupolar. These schematics do not show crucial aspects of flux emergence such as the buildup of flux at the shoulders of the rising loops, moving dipolar features, etc.
Paper: Characterizing the Umbral Magnetic Knots of δ-Sunspots
Authors: Aimee A. Norton, Peter J. Levens, Kalman J. Knizhnik, Mark G. Linton, Yang Liu
Figure caption: Tilt angles are determined with a 0°–360° range such that the calculated centroid for the flux-weighted negative magnetic polarity “N” is always at the origin. A 0° tilt is an AR in which the “N” and “P” have the same longitude, with the “P” at a more northern latitude. Two drawn configurations are shown (left) and can be understood by considering that in Solar Cycle 24 the dominant leading polarity in the northern hemisphere is “N,” so that the example on the left-hand side depicts a common tilt (0°–90°) for most ARs in the northern hemisphere. Historically, using white-light images and a limited range of angles (0°–90° or 0°–180°), the angle may have been recorded as 20° measured from the east–west line, but our angle determination would be 70°. In contrast, the drawn angle depicted in the 270°–359° quadrant shows a typical southern hemisphere configuration, where the “P” is leading and the “N” is closer to the pole, but instead of a 20° angle that may have been reported historically, the angle based on magnetic polarity and a 0°–360° range is 290°. While most northern (southern) hemisphere ARs obeying Hale’s law and Joy’s law would have values of 60°–90° (270°–300°) in Solar Cycle 24, δ-spots frequently disobey Hale’s law and Joy’s law. At right, the radial magnetic field strength for NOAA AR 11429 is shown. It is a northern hemispheric AR and has a tilt angle of 268°, with the yellow (red) cross representing the negative (positive) centroids as calculated using all umbrae (not only the δ-portion). This is anti-Hale, as tilts of 180°–359° (90°–179°) for northern hemisphere spots in cycle 24 are anti-Hale (anti-Joy), as indicated by the labeling of the magnetogram quadrants for ARs in the northern hemisphere.