adsabs/AstroCLIMB huggingface dataset:
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: Our subexposure Lyα light curves folded on HST’s orbital period of 95.42 minutes. Each color corresponds to one full exposure (one orbit) and each point corresponds to a subexposure normalized by the average flux of each orbit. The dashed line depicts the best-fit polynomial as determined by our method outlined in Section 2.2 compared to a flat line. The blue shaded region represents the 1σ uncertainties in the fit evaluated at each subexposure. The star data points represent the flaring subexposures that were not considered when fitting for breathing.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic Lyα, O I, and C II light curves observed by HST/STIS in 2023 May around the transit of AU Mic c. The gray region indicates the white-light transit duration of AU Mic c. Sample fits to the AU Mic c transit are shown in faded yellow with bright gold representing the best-fit light curves.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: The neutral and ionized hydrogen fractions of AU Mic c’s exosphere as modeled by p-winds using the XUV irradiation estimate from A. D. Feinstein et al. (2022). The solid lines represent the planet receiving quiescent irradiation, while the dashed lines represent flare irradiation.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic’s reconstructed intrinsic Lyα emission line for the last orbit of the 1998 September (purple), 2020 July (orange), 2021 October (pink), and 2023 May (green) visits.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Example oscillation spectra of stars at three different evolutionary stages. The frequency axis is centered on νmax and is shown in units of Δν. The power density is shown in dark gray, and the modes are labeled according to their angular degree, where modes of ℓ = 0, ℓ = 1, and ℓ = 2 are shown as orange, green, and purple squares respectively. The ℓ = 0 modes, highlighted by the shaded regions, have been aligned between the three frames for clearer comparison. Top: A spectrum of the MS star KIC 5184732 where all modes appear with a regular pattern. Middle: A spectrum of the SG star KIC 5723165 where the dipole modes begin to deviate from the otherwise regular pattern of the ℓ = 2, 0 mode pairs. Bottom: A spectrum of the RG star KIC 4448777 where the regular pattern of the ℓ = 1 modes has almost completely disappeared.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Scaled matrix elements Lij and Dij for a red giant stellar structure model (Model I of J. M. J. Ong et al. 2022). (a) Matrix elements Lij, scaled to produce dimensionless quantities. The upper panel shows this quantity scaled by ﹩1/{\omega }_{\,\rm{max}\,}^{2}=1/{(2\pi {\nu }_{{\rm{\max }}})}^{2}﹩ and exhibits strong dependence on the g-mode frequency index and weak-dependence on that of the p-modes. The lower panel shows the same matrix elements scaled by ﹩1/{\omega }_{{\rm{g}},j}^{2}﹩, as described in the main text. The dynamic range of its dependence on the mode indices can be seen to be significantly suppressed. (b) Similar scalings applied to matrix elements Dij, which are already dimensionless. The upper panel shows this quantity exhibiting strong dependence on both p- and g-mode indices. The lower panel shows the same matrix elements scaled by ωp,i/ωg,j, as described in the main text, again showing far milder dependencies on either index.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic spectra observed by HST/STIS on 1998 September (left; no transit), 2020 July (second-from-left; undetected AU Mic b transit), and 2021 October (middle; detected AU Mic b transit) and 2023 May (right; during AU Mic c transit). C III, N V, He II, and C I are shown. The gray regions show the wavelength ranges integrated over to obtain the light curves in Figure A2. Each line color corresponds to same orbit from Figure 3.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic spectra observed by HST/STIS on 1998 September (left; no transit), 2020 July (second-from-left; undetected AU Mic b transit), and 2021 October (middle; detected AU Mic b transit) and 2023 May (right; during AU Mic c transit). C III, N V, He II, and C I are shown. The gray regions indicate the white-light transit durations of AU Mic b and c. Flares are highlighted in gold.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Models used in PBjam for the MS star KIC 5184732. The top frame shows the smoothed PDS (gray) and a set of models (red) constructed from samples of the posterior distribution resulting from sampling Equations (2) and (4), which constitutes the first stage of the mode identification in PBjam. The first, second, and third Harvey-like profiles are shown in dashed blue, orange, and green respectively, and the shot noise level is shown in dashed purple. The middle frame shows a smaller range around the oscillation envelope of the same model as in the top frame, for clarity. The lower frame shows the residual S/N spectrum in gray after dividing the PDS by the median background and ℓ = 2, 0 models, along with similarly drawn samples of the ℓ = 1 model posterior shown in red.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Èchelle diagram of an MS star KIC 5184732 shown in gray, and the result of applying the MS model for mode identification. The colored points are samples drawn from the marginalized mode frequency posterior distributions, and so a wider collection of points denotes a larger uncertainty on the location of the mode. For clarity, only modes of azimuthal order m = 0 are shown. These frequency samples correspond to those used in the top frame of Figure 1 and to construct the models shown in Figure 2.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Èchelle diagram of the subgiant star KIC 5723165 (gray) along with the application of the SG model for mode identification shown in colored points as in Figure 3.
Paper: Far-ultraviolet Flares and Variability of the Young M Dwarf AU Mic: A Nondetection of Planet C in Transit at Lyα
Authors: Keighley E. Rockcliffe, Elisabeth R. Newton, Allison Youngblood, Girish M. Duvvuri, Emily A. Gilbert, Peter Plavchan, Peter Gao, Hans-R. Müller, Adina D. Feinstein, Thomas Barclay, Eric D. Lopez
Figure caption: AU Mic’s FUV emission over time during the 2020 July (top; AU Mic b transit), 2021 October (middle; AU Mic b transit), and 2023 May (bottom; AU Mic c transit) visits. Flares identified in Section 3.1 are highlighted in gold.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: The frequency of νmax of the prior sample represented as a function of  Teff. The black points are stars in the sample that have been observed with Kepler or TESS and for which the ℓ = 2, 0 model parameters are complete. The blue points are model grid samples taken from C. J. Lindsay et al. (2024) to supplement the ℓ = 1 model parameters for SG stars.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Left: The result of the detailed peakbagging performed for the subgiant KIC 5723165. The smoothed spectrum is shown in black, with models generated from 30 samples of the posterior distribution shown in red. Right: Èchelle diagram like that shown in Figure 5, but with the mode frequencies derived from the peakbagging posterior distribution.
Paper: Asteroseismology with PBjam 2.0: Measuring Dipole Mode Frequencies in Coupling Regimes from Main-sequence to Low-luminosity Red Giant Stars
Authors: M. B. Nielsen, J. M. J. Ong, 加冕 王, E. J. Hatt, G. R. Davies, W. J. Chaplin, G. T. Hookway, A. Stokholm, O. J. Scutt, M. N. Lund, R. A. García
Figure caption: Èchelle diagram of the red giant KIC 4448777 (gray) along with the mode identification derived from the RG model shown in colored points as in Figure 3.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Period ratios P2/P1 of neighboring planets, either observed today for planets with radii <4R⊕ in the 2024 March NASA Exoplanet Archive (bottom panel), or simulated from Run A, which is initialized with TOI-1136 analogs from the disk–planet simulations of D23 (top panel), and integrated for 100 Myr (middle panel). The Run A systems mostly do not change over time; they are too tightly locked in resonance. The histogram bins have widths of 0.02.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Reprinted from Figure 7 of F. Dai et al. (2024): the observed decline with age of the fraction of neighboring planet pairs in first-order resonance (blue diamonds), and the concomitant decline in the fraction of planetary systems containing at least one pair in a first or second-order resonance (orange stars, offset from blue diamonds for clarity). F. Dai et al. (2024) classify a pair as being in first-order resonance if −0.015 ≤Δ ≤ 0.03 and in second-order resonance if −0.015 ≤ Δ ≤ 0.015.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Neighboring planet period ratios for (a) our semiempirical Runs B-D at the start of our integrations (note how all pairs are initialized with Δ+ > 0; see Table 2); (b) the final state of Run B, which assumes collisions result in perfect mergers; (c) the final state of Run C, where major mergers produce coplanar debris particles that undergo scattering and minor mergers; (d) the final state of Run D, where major mergers produce debris particles ejected isotropically in 3D; and (e) the observations as downloaded for planets with radii <4R⊕ from the NASA Exoplanet Archive in 2024 March. Positions of first-, second-, and third-order resonances are shown with dotted vertical lines. Note the absence of resonances between P2/P1 = 1.8 and 2.0; we propose that the observed “trough” just narrow of the 2:1 (and absent from the 3:2) arises from this desert.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: A history of violence: how planetary mergers alter period ratios. Top panel: the final P2/P1 distribution at t = 100 Myr for Run B, color-coded according to the planets that contribute to a given period ratio. Combined letters denote a merger product; e.g., “bc” indicates the merged product of planets b and c, and “bcd” the merger of planets b, c, and d. Since every period ratio involves two planets, the histogram in the top panel is twice the height of the histogram for Run B as shown in the second panel of Figure 3. Bottom panel: tracing the planet pairs contributing to a given period ratio at t = 100 Myr back to their original period ratios at t = 0. If a pair at t = 100 Myr involves merger products, we assign both members of the pair to the original period ratio that connects the pair; thus, e.g., a pair consisting of planet d and merger ef in the top panel are mapped to the original period ratio between d and e (3/2 + Δ+) in the bottom panel, and not the ratio between e and f (7/5 + Δ+). In this way, we have a one-to-one correspondence between the two panels, excepting the rare mergers of nonneighboring planets (4 df and 10 eg planets) for which assigning unique initial period ratios is too ambiguous.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Initial 3:2 resonant libration amplitudes of the innermost b:c planet pairs for Run A (top panel) and Run B (bottom panel). There are two resonant arguments for the coplanar 3:2 resonance, one which depends on the longitude of periapse of the inner planet b (blue histogram), and another which depends on that for the outer planet c (orange histogram). Libration amplitudes are determined by sinusoidal fits to the resonant argument vs. time, and evaluated as the deviation from libration center. In the top panel, only the 124 systems (out of a total of 160 in Run A) that have the b:c pair near a 3:2 resonance are plotted, and of these only 1 system is in circulation, which we assign a libration amplitude of 180°. For the observation-based simulations in Run B, 27 out of 256 systems are in circulation, including those that switch between libration and circulation. The larger initial libration amplitudes in Run B explain why its resonant chains break more easily than those in Run A.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Snapshots seen in various x–y–z projections of one example simulation from Run D, featuring two major merger events at 3.888 × 104 yr (creating planet de) and 1.038 × 107 yr (creating planet fg). The orbits of the initial planets (b), (c), (d), (e), (f), and (g) are shown in thin solid lines, the orbits of merger products (de, fg) are drawn in thick solid lines, and the orbits of debris particles are plotted in dotted lines with colors that match those of their parent merger products.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Times when major mergers occur in Runs B-E, color-coded according to whether a merger occurred chronologically first, second, third, or (in rare cases) fourth within a given system. Too many resonance-breaking mergers occur at times <106 yr to be consistent with the observed decline in resonance fraction over 108 yr timescales (Figure 1).
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Initial (left column) and final (right column) period ratio distributions for Runs B, B1, B2, and B3 (top to bottom rows; see also Table 1). These experiments demonstrate that the presence of a weak second-order resonance like the 7:5 (absent in Runs B1-B2), and sufficiently large initial eccentricities (absent in Run B3), help promote instability and the breaking of resonant chains.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: The evolution of Δ for the innermost b:c = 3:2 planet pair in the Run D simulation shown in Figure 7. Minor mergers alter Δ, lowering it when a debris particle collides with b (green dashed line) and later raising it when another debris particle collides with c (black dashed line). For the final transit timing variations (TTVs) of this pair, see Figure 15.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Minor mergers between debris particles and planets occur mostly Δt < 104 yr after the debris particles are born in parent major merger events. Debris particles in Runs D, D1, and E are not coplanar with planets and take longer to accrete than in Run C where they are coplanar.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Comparison of final period ratio histograms between Run D with initially coplanar planets and Run D1 with initially noncoplanar planets (see Table 1). Both runs exhibit the 2:1 trough, while the nonresonant continuum is smoother and less bimodal in Run D1, better matching observations.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Comparison of time-averaged TTV phases 〈ΦTTV〉 between observations (top row) and Run D simulations (bottom row), for planets with −0.015 ≤ Δ ≤  + 0.03 near the 2:1 and 3:2 commensurabilities (the same Δ criterion for first-order resonance is used in F. Dai et al. 2024). Subscript 1 denotes the inner member of the pair, and subscript 2 denotes the outer member. The TTV phases plotted here are all well-defined, i.e., consistent between inner and outer members of pairs (left column). The histograms in the middle column (which plot both ﹩{\langle {{\rm{\Phi }}}_{{\rm{TTV}}}\rangle }_{1}﹩ and ﹩{\langle {{\rm{\Phi }}}_{{\rm{TTV}}}\rangle }_{2}﹩) show encouraging agreement between observed and simulated TTV phases—a concentration near 0°, and broad wings that extend to ± 180∘. We detect no trend between TTV phase and orbital period, either in the observations or in the simulations (right column). The simulated resonant pairs all derive from TOI-1136 analogs; most of those with well-defined TTV phases are the innermost surviving b:c = 3:2 pairs. The list of objects/simulations and their TTV phase curves are available here for the top row and here for the bottom row.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Neighboring planet period ratios for (a) Run E before integration, (b) Run E after 100 Myr of integration, and (c) observed gigayear-old planets with radii <4R⊕ in the 2024 March NASA Exoplanet Archive. In the upper two panels, histograms are color-coded according to whether a long chain (six-planet, type i) or short chain (four-planet, type ii) contributes. Short chains (green) fill in the period ratio gap just wide of the 3:2 left open by long chains (orange). The prominent 2:1 trough arises predominantly from the dissolution of long chains.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Transit timing variations of four 3:2 pairs from Run D, labeled (a)–(d), that survived the full 100 Myr duration of the integrations. Their TTVs at t = 100 Myr (bottom halves of each panel) differ strongly from initial behaviors at t = 0 (top halves), a consequence of the wholesale disruption and reorganization of parent chains. After 100 Myr of mergers, systems contain fewer numbers of planets, and resonant pairs are more isolated from their neighbors, allowing their TTV phases to be better defined; see pairs (c) and (d). The four pairs shown here are drawn from the 75 from Run D having well-defined TTV phases at t = 100 Myr; of these 75 pairs, only 7 had well-defined TTV phases at t = 0.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: Similar to Figure 13, but showing an alternative, simpler selection of chains from our library. Run E1 as shown here does not use the χ2 algorithm underlying Run E of Figure 13, but instead combines all of the type-i long-chain outcomes (unweighted) with all of the type-ii short-chain outcomes that yield at least one planet pair having a period ratio between the 3:2 and 5:3 resonances. The latter restriction is made in an attempt to fill the 1.54 < P2/P1 < 1.67 gap left by long chains (Figure 12, bottom left panel). Run E1 does about as well as Run E in reproducing the observations.
Paper: The Resonant Remains of Broken Chains from Major and Minor Mergers
Authors: Rixin Li, 日新 李, Eugene Chiang, 詒曾 蔣, Nick Choksi, Fei Dai, 飞 戴
Figure caption: When resonant chains of close-in sub-Neptunes break, nonresonant planets are created from mergers and are more massive than resonant planets that survive mergers. This is borne out in our simulations, including Run E whose resonant (orange) vs. nonresonant (blue) planet mass distributions are shown here. Dashed vertical lines indicate median masses in the top panel histograms, and bottom panel shows cumulative distribution functions (CDFs). Overplotted in dashed–dotted lines are the CDFs of the observed “controlled sample” from A. Leleu et al. (2024), recategorized into resonant and nonresonant planets using the F. Dai et al. (2024) Δ criteria. The slope change at 8M⊕ in our modeled resonant CDF separates the unmerged survivors from merger products that by chance land near a resonance. A similar slope change is evident in the observed resonant sample.