adsabs/AstroCLIMB huggingface dataset:
Paper: Determining Dispersal Mechanisms of Protoplanetary Disks Using Accretion and Wind Mass Loss Rates
Authors: Yasuhiro Hasegawa, Thomas J. Haworth, Keri Hoadley, Jinyoung Serena Kim, Hina Goto, Aine Juzikenaite, Neal J. Turner, Ilaria Pascucci, and Erika T. Hamden
Figure caption: The synthesized results for the case that Ms = 1 M⊙. The shaded regions well represent the disk populations produced by the Monte-Carlo method.
Paper: Deuterium Fractionation as a Multiphase Component Tracer in the Galactic Center
Authors: Laura Colzi, Jesús Martín-Pintado, Víctor M. Rivilla, Izaskun Jiménez-Serra, Shaoshan Zeng, Lucas F. Rodríguez-Almeida, Fernando Rico-Villas, Sergio Martín, and Miguel A. Requena-Torres
Figure caption: Observed transitions of the isotopologues of HCN (left) and HNC (right) studied in this work. The transition shown in each panel is indicated in the upper right. The orange line is the best LTE fit to the prestellar component, the green line is the best LTE fit to the broad gas component, and the red line is the sum of the components. The blue line indicates the total modeled line emission, including also the contribution of all molecular species previously identified in the survey (e.g., Rivilla et al. 2021; Rodríguez-Almeida et al. 2021a, 2021b; Zeng et al. 2021).
Paper: Deuterium Fractionation as a Multiphase Component Tracer in the Galactic Center
Authors: Laura Colzi, Jesús Martín-Pintado, Víctor M. Rivilla, Izaskun Jiménez-Serra, Shaoshan Zeng, Lucas F. Rodríguez-Almeida, Fernando Rico-Villas, Sergio Martín, and Miguel A. Requena-Torres
Figure caption: Observed transitions of the isotopologues of HCO+ (left) and N2H+ (right) studied in this work. The transition shown in each panel is indicated in the upper right. The orange line is the best LTE fit to the prestellar component, the green line is the best LTE fit to the broad component, and the red line is the sum of the two profiles. The blue line indicates the total modeled line emission, including also the contribution of all molecular species previously identified in the survey (e.g., Rivilla et al. 2021; Rodríguez-Almeida et al. 2021a, 2021b; Zeng et al. 2021).
Paper: Deuterium Fractionation as a Multiphase Component Tracer in the Galactic Center
Authors: Laura Colzi, Jesús Martín-Pintado, Víctor M. Rivilla, Izaskun Jiménez-Serra, Shaoshan Zeng, Lucas F. Rodríguez-Almeida, Fernando Rico-Villas, Sergio Martín, and Miguel A. Requena-Torres
Figure caption: D/H ratios found for the different molecules, in the prestellar (orange) and broad (green) components. The red horizontal line indicates the primordial D/H value of (2.55 ± 0.03) × 10−5 (Zavarygin et al. 2018).
Paper: Deuterium Fractionation as a Multiphase Component Tracer in the Galactic Center
Authors: Laura Colzi, Jesús Martín-Pintado, Víctor M. Rivilla, Izaskun Jiménez-Serra, Shaoshan Zeng, Lucas F. Rodríguez-Almeida, Fernando Rico-Villas, Sergio Martín, and Miguel A. Requena-Torres
Figure caption: Observed transitions that are blended with other species. The molecule and transition shown in each panel are indicated in the upper right. Blending species are indicated in blue when known. The orange line is the best LTE fit to the prestellar component, the green line is the best LTE fit to the broad gas component, and the red line is the sum of the components. The blue line indicates the total modeled line emission, including also the contribution of all molecular species previously identified in the survey (e.g., Rodríguez-Almeida et al. 2021a, 2021b; Rivilla et al. 2021; Zeng et al. 2021).
Paper: Evidence for Cold-stream to Hot-accretion Transition as Traced by Lyα Emission from Groups and Clusters at 2 < z < 3.3
Authors: E. Daddi, R. M. Rich, F. Valentino, S. Jin, I. Delvecchio, D. Liu, V. Strazzullo, J. Neill, R. Gobat, A. Finoguenov, F. Bournaud, D. Elbaz, B. S. Kalita, D. O'Sullivan, and T. Wang
Figure caption: Color images of spectroscopically confirmed targets for which KCWI Lyα observations are first presented here (BzK for most, or close variations; north is up and east is left). Cl-1449 is from HST; the rest is ground-based. See D21 for a similar RO-1001 image. The blue soft layer shows Lyα emission, with contours displayed in log steps from –18.5 to –17.5 erg s−1 arcsec−2 as labeled. The dotted lines show the KCWI field. The orientation of the RO fields was chosen to maximize overlap with the radio detections.
Paper: Evidence for Cold-stream to Hot-accretion Transition as Traced by Lyα Emission from Groups and Clusters at 2 < z < 3.3
Authors: E. Daddi, R. M. Rich, F. Valentino, S. Jin, I. Delvecchio, D. Liu, V. Strazzullo, J. Neill, R. Gobat, A. Finoguenov, F. Bournaud, D. Elbaz, B. S. Kalita, D. O'Sullivan, and T. Wang
Figure caption: (Left) Our sample in the DB06 diagram. Symbol sizes are proportional to LLyα (Table 1). The blue diagonal line defines Mstream (Equation (2)). (Right) The ratio of the extended Lyα luminosity in the structures is plotted vs. the Mstream to halo-mass ratio. The relation in Equation (4) is fitted (solid black line). Typical uncertainties are shown: 0.2 dex along the slope above Mstream, 0.3 dex along the y-axis below Mstream. Predictions for MDM < Mstream (cold-stream regime) are shown (colored dashed lines).
Paper: Evidence for Cold-stream to Hot-accretion Transition as Traced by Lyα Emission from Groups and Clusters at 2 < z < 3.3
Authors: E. Daddi, R. M. Rich, F. Valentino, S. Jin, I. Delvecchio, D. Liu, V. Strazzullo, J. Neill, R. Gobat, A. Finoguenov, F. Bournaud, D. Elbaz, B. S. Kalita, D. O'Sullivan, and T. Wang
Figure caption: As in Figure 2, right, but for SFR (left) and AGNs (right). Notice the especially poor correlation with LAGN/BAR.
Paper: Evidence for Cold-stream to Hot-accretion Transition as Traced by Lyα Emission from Groups and Clusters at 2 < z < 3.3
Authors: E. Daddi, R. M. Rich, F. Valentino, S. Jin, I. Delvecchio, D. Liu, V. Strazzullo, J. Neill, R. Gobat, A. Finoguenov, F. Bournaud, D. Elbaz, B. S. Kalita, D. O'Sullivan, and T. Wang
Figure caption: (Left) The Lyα luminosity vs. the AGN ionizing photon rates for our sample (black points estimated from the ultraviolet luminosity, blue empty points connected by dashed lines are computed from Lbol,AGN; see the text). The diagonal lines show the Lyα luminosity that AGNs can ionize: theoretical maximum (dotted) and (solid) assuming a 30% escape fraction (Smith et al. 2020) and an opening angle Ω = 30% (Simpson 2005). (Right) The Lyα luminosity vs. the cold accretion rate, as resulting from Equation (3). The solid (dotted) line(s) shows the average linear trend (1σ range). The colored dashed lines are models as in Figure 2-, right (Dijkstra & Loeb 2009; Goerdt et al. 2010; Rosdahl & Blaizot 2012). In both panels, QSO-selected Lyα nebulae are shown, individually in the left panel and averaged in the right panel where the QSOs’ average hosting MDM, hence BAR, are estimated from Eftekharzadeh et al. (2015).
Paper: Asteroids and Life: How Special Is the Solar System?
Authors: Rebecca G. Martin, and Mario Livio
Figure caption: Location of the resonance as a fraction of the inner giant’s semimajor axis, aν6/a1. The colored regions show where the resonance is in the radial range ﹩0.29\lt {a}_{{\nu }_{6}}/{a}_{1}\lt 0.63﹩ for varying mass and semimajor axis of the outer giant planet scaled to those of the inner planet. The dashed vertical lines represent the 2:1 MMR between the two giants. The inner planet has a mass of m1 = 0.01 M⋆ (top left), m1 = 0.001 M⋆ (bottom left), and m1 = 0.0001 M⋆ (top right). The green points shows the solar system. Bottom right: relative mass and semimajor axis of exoplanet planet pairs shown in Table 1 (red points). The shaded regions show where the ν6 resonance lies within the asteroid belt region for inner planet masses m1 = 0.0001 M⋆ (blue), m1 = 0.001 M⋆ (yellow), and m1 = 0.01 M⋆ (red).
Paper: Asteroids and Life: How Special Is the Solar System?
Authors: Rebecca G. Martin, and Mario Livio
Figure caption: The width of the resonance, w/a1, defined to be where ef > 0.08. The inner planet has a mass of m1 = 0.01 M⋆ (top left), m1 = 0.001 M⋆ (bottom left), and m1 = 0.0001 M⋆ (top right), and the outer planet has eccentricity e2 = 0.05. The bottom right panel shows m1 = 0.001 M⋆ and e2 = 0.25. The inner-planet eccentricity is e1 = 0.05 in all cases.
Paper: Asteroids and Life: How Special Is the Solar System?
Authors: Rebecca G. Martin, and Mario Livio
Figure caption: Asteroid outcomes as a function of time and their original semimajor axis, a, for run1 (left), run2 (middle), and run3 (right). Blue points show asteroids that are ejected. Red points show asteroids that collide with the Sun, green points show asteroids that collide with Earth, and yellow points show asteroids that collide with Jupiter or Saturn.
Paper: A Novel Way of Measuring the Gas Disk Mass of Protoplanetary Disks Using N2H+ and C18O
Authors: Leon Trapman, Ke Zhang, Merel L. R. van't Hoff, Michiel R. Hogerheijde, and Edwin A. Bergin
Figure caption: Concept of how N2H+ and C18O enable us to distinguish between disks with low disk masses and low CO abundance. Starting from the fiducial model (diamond) on the right, points show the change in N2H+ 3 − 2 and C18O 2 − 1 line flux when either the disk mass (circles) or CO abundance (squares) is decreased, with decrements of factors of 10. Relevant disk parameters of the fiducial model are shown in the bottom left.
Paper: A Novel Way of Measuring the Gas Disk Mass of Protoplanetary Disks Using N2H+ and C18O
Authors: Leon Trapman, Ke Zhang, Merel L. R. van't Hoff, Michiel R. Hogerheijde, and Edwin A. Bergin
Figure caption: Comparison between the observed C18O J = 2 − 1 integrated line flux and our models with different combinations of disk gas mass and CO abundance. Colors show how close the model C18O line flux is to the observations, expressed in terms of the uncertainty on the C18O line flux. (σobs). Dashed black lines highlight the part of the Mgas-xCO parameters space where model C18O fluxes are within 3σobs. Darker shades of blue (red) marks parameter space where the model underproduces (overproduces) the observed flux.
Paper: A Novel Way of Measuring the Gas Disk Mass of Protoplanetary Disks Using N2H+ and C18O
Authors: Leon Trapman, Ke Zhang, Merel L. R. van't Hoff, Michiel R. Hogerheijde, and Edwin A. Bergin
Figure caption: N2H+(3 − 2)/C18O(2 − 1) flux ratio vs. the CO abundance. Points denote individual models, where the shape shows the assumed cosmic-ray ionization rate (ζCR). The colors show the gas mass of the disk. The observed N2H+(3 − 2)/C18O(2 − 1) ratio is shown as a black dashed line, with the gray shaded region showing the 3σ uncertainty. For reference we included the lowest and highest disk mass that reproduce these observations, assuming 10−19 s−1 ≤ ζCR ≤ 10−17 s−1. The smaller panels under each main panel show the CO abundance ranges that reproduce the observations. Here the orange bar corresponds to N2H+(3 − 2) and C18O(2 − 1), with 10−19 s−1 ≤ ζCR ≤ 10−17 s−1. The black bar instead shows the CO abundance constrained by HD 1 − 0 and C18O(2 − 1).
Paper: A Novel Way of Measuring the Gas Disk Mass of Protoplanetary Disks Using N2H+ and C18O
Authors: Leon Trapman, Ke Zhang, Merel L. R. van't Hoff, Michiel R. Hogerheijde, and Edwin A. Bergin
Figure caption: Comparison of the mass ranges obtained from HD 1 − 0 (gray shaded region) and the combination of N2H+ and C18O (orange box). Note that for N2H+ and C18O we have assumed 10−19 s−1 ≤ ζCR ≤ 10−17 s−1. Points show individual models, with their color showing the CO abundance. For DM Tau, the transition from dark to light gray shows where Mdisk = 0.2 M⊙. For a higher disk mass there should be signs of gravitational instability in the disk, which have not been seen in observations (see Section 3 for more details).
Paper: A Novel Way of Measuring the Gas Disk Mass of Protoplanetary Disks Using N2H+ and C18O
Authors: Leon Trapman, Ke Zhang, Merel L. R. van't Hoff, Michiel R. Hogerheijde, and Edwin A. Bergin
Figure caption: Gas mass ranges of TW Hya, DM Tau and GM Aur obtained by comparing model HD 1 − 0 integrated fluxes to the observations (Bergin et al. 2013; McClure et al. 2016). Observations are shown in black, with the gray shaded region showing the 3σ uncertainty. Blue points show individual model fluxes, to which we have fitted the power law shown as the blue dashed line. The orange vertical line and shaded region show the best fitting gas mass and 3σ uncertainty, respectively.
Paper: Kinetic-scale Current Sheets in the Solar Wind at 1 au: Scale-dependent Properties and Critical Current Density
Authors: I. Y. Vasko, K. Alimov, T. Phan, S. D. Bale, F. S. Mozer, and A. V. Artemyev
Figure caption: An example of a current sheet observed aboard the Wind spacecraft on 2011 February 1 around 05:22 UT. (a) Magnetic field magnitude and three magnetic field components measured at 1/11 s resolution (the Geocentric Solar Ecliptic coordinates); (b) three magnetic field components in the local coordinate system xyz defined in Section 2; (c) current densities Jx and Jy computed using Equation (1); (d) current densities parallel and perpendicular to the local magnetic field, computed as J∣∣ = (JxBx + JyBy)/B and J⊥ =(JyBx − JxBy)/B. The central region of the CS, ∣ Bx − 〈Bx〉 ∣ < 0.2 ΔBx, is indicated in panels (b)–(d), where 〈Bx〉 is the mean of the Bx values at the CS boundaries, and ΔBx is the absolute value of their difference. The bottom horizontal axis presents the spatial coordinate across the CS, z = −Vnt, where t = 0 corresponds to Bx = 〈Bx〉 and Vn is the normal component of proton flow velocity measured at the moment closest to the CS.
Paper: Kinetic-scale Current Sheets in the Solar Wind at 1 au: Scale-dependent Properties and Critical Current Density
Authors: I. Y. Vasko, K. Alimov, T. Phan, S. D. Bale, F. S. Mozer, and A. V. Artemyev
Figure caption: Statistical distributions of various parameters of 17,043 solar wind CSs: (a) ﹩{\rm{\Delta }}{B}_{\max }/\langle B\rangle ﹩, the maximum relative variation of the magnetic field magnitude within the CS, and parameter 〈Bx〉/ΔBx, characterizing the CS asymmetry, where 〈Bx〉 is the mean of the Bx values at the CS boundaries and ΔBx is the absolute value of their difference; (b) absolute value J0 of parallel current density J∣∣ averaged over the CS’s central region (see, e.g., Figure 1) and peak value Jpeak of parallel current density J∣∣ within the CS; (c) CS thickness λ. The bottom panels present cumulative distribution functions of the statistical distributions in the upper panels.
Paper: Kinetic-scale Current Sheets in the Solar Wind at 1 au: Scale-dependent Properties and Critical Current Density
Authors: I. Y. Vasko, K. Alimov, T. Phan, S. D. Bale, F. S. Mozer, and A. V. Artemyev
Figure caption: Panel (a) presents a scatter plot of the CS thickness λ vs. local proton inertial length λp. The green curve shows the trend that is obtained by sorting the CSs into bins corresponding to various spatial scales and computing the averaged thickness of the CSs within each bin. The number of CSs within each bin is shown in the bottom panel. The black dashed line represents λ = λp for reference. Panel (b) presents a statistical distribution of the CS thickness in units of proton inertial length. The bottom panel presents the corresponding cumulative distribution function.
Paper: Kinetic-scale Current Sheets in the Solar Wind at 1 au: Scale-dependent Properties and Critical Current Density
Authors: I. Y. Vasko, K. Alimov, T. Phan, S. D. Bale, F. S. Mozer, and A. V. Artemyev
Figure caption: Scatter plots of (a) averaged current density J0 vs. CS thickness λ; (b) peak current density Jpeak vs. local Alfén current density JA = eNpVA, where e is the proton charge, Np is the proton density, VA is the local Alfvén speed; (c) the peak value of the drift velocity between ions and electrons Jpeak/eNp vs. local Alfvén speed VA. For each of the scatter plots, we sorted the CSs into bins corresponding to different values of the quantities on the x-axis and computed median values of the quantities on the y-axis for the CSs within each bin. The CSs were sorted in such a way that each bin contains a sufficiently large (i.e., more than 100) number of CSs, and the number of CSs within each bin is presented in the bottom panels (only the last bin in panel (a) contains fewer than 100 CSs). The corresponding median profiles are presented by green curves in panels (a)–(c), while error bars correspond to 15th and 85th percentiles of the quantities within each bin. The red line in panel (a) presents the best fit of the scattered data by a power-law function, and the best-fit parameters are indicated in the panel.
Paper: Kinetic-scale Current Sheets in the Solar Wind at 1 au: Scale-dependent Properties and Critical Current Density
Authors: I. Y. Vasko, K. Alimov, T. Phan, S. D. Bale, F. S. Mozer, and A. V. Artemyev
Figure caption: Scatter plots of (a) the current density normalized to Alfvén current density J0/JA vs. normalized CS thickness λ/λp; (b) the CS amplitude normalized to the mean magnetic field magnitude ΔBx/〈B〉 vs. λ/λp; (c) magnetic shear angle Δθ vs. λ/λp. The CSs were sorted into bins corresponding to different values of normalized CS thickness, and median values of the quantities in panels (a)–(c) were computed within each bin. The CSs were sorted in such a way that each bin contains a sufficiently large (i.e., more than 100) number of CSs within each bin, and the number of CSs within each bin is presented in panel (d) (only the last bin contains fewer than 100 CSs). Panels (a)–(c) present the median profiles (green curves) along with error bars corresponding to 15th and 85th percentiles within each bin. The panels also indicate the best power-law fits of the scattered data (red curves) along with the best-fit parameters. The dashed line in panel (c) corresponds to Δθ = 2λ/λp, which corresponds to J∣∣ = JA.
Paper: Three-body Resonances in the Saturnian System
Authors: Matija Ćuk, and Maryame El Moutamid
Figure caption: Two simulations of capture into semisecular three-body resonance between Mimas, Dione, and Titan, illustrated by the evolution of the eccentricity of Mimas (top panel) and the resonant argument 3λD − λM − ϖM − ϖT (bottom panel). In the simulation plotted in black both Mimas and Dione are assumed to have very low eccentricities (e ≤ 10−3) before the resonance was encountered, while Titan was assumed to be on its present orbit, but with an eccentricity of e = 0.033 (to account for subsequent eccentricity damping). The resulting three-body resonance persists until the end of the simulation. In the simulation plotted in gray, Dione was assumed to initially have eD = 0.01, enhancing secondary resonances, seen in the resonant argument plot as jumps in the libration argument, and breaking the three-body resonance just before 10 Myr. The small kick to the eccentricity of Mimas at 10 Myr is due to the 3λD − λM − ϖM − ϖD subresonance, while the larger kick at 14 Myr is due to one with the argument 3λD − λM − 2ϖM.
Paper: Three-body Resonances in the Saturnian System
Authors: Matija Ćuk, and Maryame El Moutamid
Figure caption: A simulation of capture into a three-body resonance between Enceladus (light blue), Tethys (magenta), and Dione (dark green). The three-body resonant argument (bottom panel) is 4λE − 11λΘ + 8λD − ϖE. This three-body resonance is a consequence of Enceladus and Tethys crossing their 11:8 MMR while Enceladus and Dione are locked in their 2:1 MMR (second panel from the bottom). Three-body resonance breaks at about 10.5 Myr, and the subsequent kicks to the eccentricity of Tethys are caused by various subresonances of the Enceladus–Tethys 11:8 MMR.
Paper: Three-body Resonances in the Saturnian System
Authors: Matija Ćuk, and Maryame El Moutamid
Figure caption: A simulation of capture into an isolated three-body resonance between Tethys (magenta), Dione (dark green), and Rhea (black). The resonant argument, shown in the bottom panel, is 5λD − 3λΘ − λR − ϖD. If we assume that Saturn’s moons are evolving though equilibrium tides, this resonance should have happened about 20 Myr ago. Note that Dione was given a low eccentricity (eD = 0.001) at the beginning of the simulation; present-day eccentricity eD = 0.0022 usually leads to passage without capture. Depending on the eccentricity damping within Dione, this TBR could be the source of Dione’s present eccentricity, or may have been passed without capture if Dione’s eccentricity predates this resonance.
Paper: Three-body Resonances in the Saturnian System
Authors: Matija Ćuk, and Maryame El Moutamid
Figure caption: A simulation of capture into an isolated three-body resonance between Enceladus (light blue), Tethys (magenta), and Titan (black). The three-body resonance has the argument 7λE − 10λΘ + 3λT + ϖE − ϖT (bottom panel), making it a second-order TBR. Enceladus is also in 2:1 MMR with Dione (second panel from the bottom), which does not participate in the three-body resonance. While the resonance acts to decrease the eccentricity of Enceladus, Enceladus actually becomes more eccentric as it is pushes deeper into the resonance with Dione. This resonance may have happened within the past Myr, opening the possibility that Enceladus’s eccentricity and current heating are not currently in equilibrium.
Paper: Origins of Hot Jupiters from the Stellar Obliquity Distribution
Authors: Malena Rice, Songhu Wang, and Gregory Laughlin
Figure caption: Comparison of the obliquity distributions for stars hosting exoplanets on circular vs. eccentric orbits. Top: full sample of spin–orbit angles included in this study. Planets with M < 0.3MJ are shown with diamond markers. The data behind this panel are available together with all other planet parameters used in this work, drawn from archival studies. Middle and bottom: cumulative sums of ∣λ∣ for eccentric exoplanets, compared with 5000 randomly sampled sets of circular exoplanets (sampled without replacement). Histograms on the right provide vertical cuts through the sums at the Kraft break. In each panel, a linear model fitting the e ≥ 0.1 cumulative sum is shown in light purple, while the running median of the e = 0 population is provided in light blue together with the shaded region within 1σ of the median.(The data used to create this figure are available.)
Paper: Origins of Hot Jupiters from the Stellar Obliquity Distribution
Authors: Malena Rice, Songhu Wang, and Gregory Laughlin
Figure caption: Distribution of ∣λ∣ values for each population, segmented by eccentricity and host star temperature. The central ∣λ∣ distribution for each set of planets is shown in bold. To quantify uncertainties, we iteratively drew from a Gaussian distribution around each measured ∣λ∣ value and recalculated the probability distribution based on these new draws, plotting the resulting distributions with lower opacity. Fifty iterations are displayed per set of planets. The theoretical projected obliquity distributions are overlaid for the Kozai–Lidov effect with a stellar (Naoz et al. 2012) or planetary (Naoz et al. 2011; Petrovich & Tremaine 2016) companion, secular chaos (Teyssandier et al. 2019), and planet–planet scattering (Nagasawa & Ida 2011).
Paper: Origins of Hot Jupiters from the Stellar Obliquity Distribution
Authors: Malena Rice, Songhu Wang, and Gregory Laughlin
Figure caption: Demonstration that systems with long obliquity damping timescales around cool stars are significantly more misaligned than those with shorter damping timescales. Top: tidal realignment timescales for cool (Teff < 6100 K) star systems in our sample. Planets with e ≥ 0.1 are outlined with a black border. The mean eccentricity damping timescale ﹩\overline{{\tau }_{e}}﹩ for each of the four evenly sized, 15-planet bins is provided along the top of the panel. Bottom: stars with the 20 longest tidal realignment timescales (τλ > 1011 yr) as compared with random draws without replacement from the population of systems with shorter tidal timescales.