adsabs/AstroCLIMB huggingface dataset:
Paper: Current Sheet Alignment in Oblique Black Hole Magnetospheres: A Black Hole Pulsar?
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: The current sheet alignment timescale τ  χ  and the event horizon magnetic flux decay timescale τ Φ as a function of the numerical resolution indicated by the SMR level. This shows signs of numerical convergence beyond three SMR levels.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Magnetic field and plasma measurements during the shock encounter. Panels (A) and (B) provide a 9 hr overview of the magnetic field and the 1D proton energy flux, capturing the preevent solar wind, the in situ shock passage, the following sheath region, and the initial portion of the associated CME ejecta. The SPAN-i data downstream of the shock do not accurately represent reality, as the flow is largely deflected away from the detector’s FOV. Panels (C)–(E) offer an 80 minute close-up leading to the shock arrival, showing variations in the bulk ion distribution as captured by the SPAN-i and EPI-Lo instruments. Finally, panels (F)–(H) focus on a 2 minute snapshot close to the shock transition, emphasizing fluctuations in the total magnetic field as well as the change in proton temperature. The downstream proton temperature is marked with hatching due to significant instrumental uncertainties.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Energetic particles and the evolution of the wave foreshock. Panels (A)–(D) show the time–energy plots for high-energy electron counts detected by EPI-Hi, low-energy electron flux from EPI-Lo, proton flux from EPI-Lo, and the amplitude of transversal (⊥) and parallel (∥) magnetic fluctuations. In panel (E), we present the proton intensity spectra for three selected times (06:40, 07:10, and at the shock, averaged as 07:13–07:15 UT) with an E −1 power law shown for reference, which indicates the changes in energetic particle distribution. Panel (F) shows the Fourier power spectra of B R (estimating B ∥ power) and the sum of B T and B N (estimating B ⊥ power) in the foreshock and the background. Variations in the proton flux and magnetic fluctuations over a 2 minute period surrounding the shock transition are shown in panels (G) and (H).
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Analysis of the waves at the shock transition. Panels (A) and (B) show the magnetic and electric field components. The duration of the precursor whistlers (between 07:13:11.10 and 07:13:11.45) is annotated on top. Panel (A) also indicates the approximate spatial scale of the upstream in units of λ i estimated in the plasma frame. Panels (C) and (D) show the Morlet wavelet spectrum of the magnetic and electric fields. The θ  kB  angle between the wavevector  k  and the magnetic field  B  is shown in panel (E). In panel (F), we show the Poynting flux estimated in the spacecraft frame  S  sc. Finally, the hodographs of precursor whistler waves in the maximum vs. intermediate variance plane and the maximum vs. minimum variance planes are presented in panels (G) and (H), respectively. In both panels, the blue arrow denotes the mean field B 0.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Transition region of the quasi-parallel shock. Panel (A) displays the time evolution (depicted by the colors blue to red) of the transversal magnetic field components. The dotted line through the middle represents the mean field, B 0. Panel (B) illustrates a 2D schematic of the shock transition in the plasma frame. The spatial scales are in λ i (represented with 50λ i × 50λ i squares) and are estimated for the upstream and downstream separated at the edge of the quasi-parallel shock (Q ∥). The gray scale represents the change in  B  across the shock. The direction of  B  and the shock normal are also marked by arrows. The dark stripes in the middle represent the quasi-perpendicular structure at the ramp and the whistler precursors. Panel (C) presents the magnetic field magnitude upon which the schematic is based.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: In situ arrival of the shock as observed through high-frequency electric field data from the FIELDS/RFS. The top panel displays the coherence spectra, while the middle panel presents the normalized linear polarization, Stokes Q/I. The estimated upstream and downstream plasma frequencies (ω pe) are indicated by horizontal black lines, with arrows highlighting the observed electrostatic waves. The bottom panel juxtaposes the estimated electron density (n e)—with the range of uncertainty depicted as a red shaded area—against the ion density measured by SPAN-i.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Ion energy fluxes measured by EPI-Lo ChanR, the high time resolution channel. The vertical line indicates the moment of the in situ shock’s arrival. Gray shaded areas in the graph represent intervals where data were not available.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Ion energy fluxes measured by EPI-Lo ChanP, the high energy resolution channel. The vertical line indicates the moment of the in situ shock’s arrival. Gray shaded areas in the graph represent intervals where data were not available.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Window selection for Fourier analysis. The pink shaded areas indicate the fast Fourier transform windows utilized for estimating the power spectral density shown in Figure 2(F).
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Ion energy fluxes measured by EPI-Lo ChanT, the full time-of-flight data. The vertical line indicates the moment of the in situ shock’s arrival. Gray shaded areas in the graph represent intervals where data were not available.
Paper: Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere
Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale
Figure caption: Dynamic radio spectra constructed from the FIELDS/RFS receivers. The solar flare onset and the in situ shock arrival are indicated on top of the panel.
Paper: Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere
Authors: Fu Yu, Shihao Rao, Jie Zhao, Chuan Li, Yang Su, Jinsong Zhao, Ye Qiu, Mingde Ding, Cheng Fang, Hui Li, Weiqun Gan
Figure caption: Coronal-hole-related observations. Panels (a)–(d) are images from SDO/AIA 193 Å, SDO/HMI LOS magnetogram, CHASE Hα line center, and CHASE Hα-based Dopplergram. R1, R2, and R3 are three coronal hole regions, R ref is a selected reference region. The black dotted–dashed line represents the central axis of a stripe region due to the instrumental effect, which is excluded in the following statistics.
Paper: Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere
Authors: Fu Yu, Shihao Rao, Jie Zhao, Chuan Li, Yang Su, Jinsong Zhao, Ye Qiu, Mingde Ding, Cheng Fang, Hui Li, Weiqun Gan
Figure caption: The statistical results of Hα-based Doppler velocities (panels (a)–(c)) and LOS magnetic field magnitudes (panels (d)–(f)) for two coronal hole regions (i.e., R1, R2) and one reference region (i.e., R ref). The orange statistical charts show the results for the overall regions while the blue charts are filtered by regions of network boundaries identified by the Hα coadded line-wing image. The black dotted–dashed line with value = 0 in each panel is used for reference.
Paper: Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere
Authors: Fu Yu, Shihao Rao, Jie Zhao, Chuan Li, Yang Su, Jinsong Zhao, Ye Qiu, Mingde Ding, Cheng Fang, Hui Li, Weiqun Gan
Figure caption: Three subregions with a combined Hα line-wing image of ±0.5 Å as the background in different fields of view. The contours in orange and red highlight the coronal hole regions (i.e., R1 and R2), and the reference region (i.e., R ref), respectively. The green and cyan contours are from the LOS magnetogram with levels of ±20 G.
Paper: Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere
Authors: Fu Yu, Shihao Rao, Jie Zhao, Chuan Li, Yang Su, Jinsong Zhao, Ye Qiu, Mingde Ding, Cheng Fang, Hui Li, Weiqun Gan
Figure caption: The uncertainty estimation for the Doppler velocity in Figures 5(a)–(c). The background shows the uncertainty distribution of Doppler velocity in different velocity intervals, with darker colors indicating a higher probability. The pink error bars are given by the mean value and 1σ range of the errors in each considered velocity interval, which are also described by the pink shadows. The red error bar represents an average value (±1σ) of the errors from all sampling points.
Paper: Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere
Authors: Fu Yu, Shihao Rao, Jie Zhao, Chuan Li, Yang Su, Jinsong Zhao, Ye Qiu, Mingde Ding, Cheng Fang, Hui Li, Weiqun Gan
Figure caption: Similar to Figure 3, but using Dopplergram as the background and displaying the network boundaries with black contours.
Paper: Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere
Authors: Fu Yu, Shihao Rao, Jie Zhao, Chuan Li, Yang Su, Jinsong Zhao, Ye Qiu, Mingde Ding, Cheng Fang, Hui Li, Weiqun Gan
Figure caption: Similar to Figure 2, but with the cyan contours representing the network boundaries extracted from the background Hα image.
Paper: On the Pair-instability Supernova Origin of J1010+2358 
Authors: Ása Skúladóttir, Ioanna Koutsouridou, Irene Vanni, Anish M. Amarsi, Romain Lucchesi, Stefania Salvadori, David S. Aguado
Figure caption: Key spectral lines in the UVES spectrum (black) of J1010+2358. Synthetic spectra assume LTE and are shown in colors. Red are the best fits, and gray without the depicted element. Blue solid line (top left) shows the CH band if the star was a pure descendant of a 260 M ⊙ PISN (Heger & Woosley 2002), assuming the same 3D corrections for CH as adopted in Table 1. Orange lines show synthetic spectra for the measurements (Si) or upper limits (Na, Sc, Sr) from Xing et al. (2023) by assuming their adopted stellar parameters (Teff = 5860 K, ﹩\mathrm{log}\ {\rm{g}}﹩ = 3.6, and v  t  = 1.5 km s−1), but different Si lines were used in their analysis. All other depicted synthetic spectra (red, blue, gray) assume the stellar parameters of this work (Teff = 5839 K, ﹩\mathrm{log}g﹩ = 4.72,and v  t  = 1.37 km s−1).
Paper: On the Pair-instability Supernova Origin of J1010+2358 
Authors: Ása Skúladóttir, Ioanna Koutsouridou, Irene Vanni, Anish M. Amarsi, Romain Lucchesi, Stefania Salvadori, David S. Aguado
Figure caption: Abundance pattern of J1010+2358 (red) compared with the best fit (blue), where 50% of the metals originate from a 13 M ⊙ Population II ccSN and the rest comes from a Population III ccSN (m ⋆ = 39 M ⊙, ﹩{{\rm{E}}}_{{SN}}=0.9\times {10}^{51}\ ﹩ erg). Additionally shown are environments enriched by (i) a 260 M ⊙ PISN (50%) and a Population III ccSN (orange); (ii) a Population III SN Ia (40%) and a high-energy Population III SN (green); (iii) the 13 M ⊙ Population II SN (100%), which is present in all our best fits (﹩{\chi }_{\mathrm{rel}}^{2}\lt 2﹩); and (iv) a 260  M ⊙ PISN (100%), as the originally proposed origin of J1010+2358 by Xing et al. (2023; gray dashed).
Paper: On the Pair-instability Supernova Origin of J1010+2358 
Authors: Ása Skúladóttir, Ioanna Koutsouridou, Irene Vanni, Anish M. Amarsi, Romain Lucchesi, Stefania Salvadori, David S. Aguado
Figure caption: Comparison between the chemical abundance pattern of J1010+2358 as measured by this work (red stars) and (Xing et al. 2023, orange squares). Dashed gray line marks the [Fe I/H] of Xing et al. (2023); and for Ti, the abundances from Ti II lines are shown.
Paper: On the Pair-instability Supernova Origin of J1010+2358 
Authors: Ása Skúladóttir, Ioanna Koutsouridou, Irene Vanni, Anish M. Amarsi, Romain Lucchesi, Stefania Salvadori, David S. Aguado
Figure caption: Minimum ﹩{\chi }_{\mathrm{rel}}^{2}﹩ over all fits containing two progenitors: (i) a PISN of a given mass ﹩{m}_{\mathrm{PISN}}﹩ and fraction of enrichment, ﹩{f}_{\mathrm{PISN}}﹩, (ii) another star providing the remaining metals.
Paper: On the Pair-instability Supernova Origin of J1010+2358 
Authors: Ása Skúladóttir, Ioanna Koutsouridou, Irene Vanni, Anish M. Amarsi, Romain Lucchesi, Stefania Salvadori, David S. Aguado
Figure caption: Yonsei–Yale isochrones for stars with M ⋆ = 0.8 M ⊙ and age 13 Gyr. Black line shows the interpolated isochrone for a star with [Fe/H] = − 2.4, and black points show our adopted temperature of Teff = 5839 K. Enhancement of [α/Fe] = + 0.3 is assumed, except in the case of [Fe/H] = 0 where [α/Fe] = 0.
Paper: Peas-in-a-pod across the Radius Valley: Rocky Systems Are Less Uniform in Mass but More Uniform in Size and Spacing
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Left: compositional dichotomy between small, rocky planets and intermediate-sized, volatile-rich planets, as defined by a transition radius R cut = 1.6 R ⊕ (Section 3). In accord with the findings of Rodríguez Martínez et al. (2023) and Rubenzahl et al. (2024), we leverage the tight correspondence of observed rocky worlds with the semiempirical Earth-composition (30% Fe, 70% MgSiO3) M–R relation (gold curve) presented by Zeng et al. (2016) to robustly infer planetary masses M  p  and associated 1σ mass uncertainties δ M  p  for 118 small (R  p  ≤ 1.6 R ⊕) worlds (gold points) across 48 CKS systems (Weiss et al. 2018a; see Section 5.1 of this work). Our NEA volatile-rich sample (blue points; see Section 5.2 of this work) exhibits qualitatively stronger clustering in planetary mass than the CKS rocky worlds, indicative of a greater degree of planetary mass diversity for rocky systems, which we assess rigorously in Section 5.3. We explore in Appendix A.1 the usage of iron-rich (red curve; 50% Fe, 50% MgSiO3) and pure rock (green curve) relations from Zeng et al. (2016) as alternative compositional models for the mass inference of our CKS rocky planets, finding that the enhanced mass diversity of rocky systems increases with the simultaneous consideration of multiple possible bulk planetary compositions as opposed to an Earth-like M–R profile alone.
Paper: Peas-in-a-pod across the Radius Valley: Rocky Systems Are Less Uniform in Mass but More Uniform in Size and Spacing
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Rocky systems generally favor configurations more uniform in planetary size, less uniform in planetary mass, and more uniform in planetary spacing than their volatile-rich counterparts. Left column: The distribution of ﹩{{ \mathcal G }}_{R}﹩ values within our CKS rocky sample (gold) is 73% and 92% contained within the respective high-uniformity regimes of ﹩{{ \mathcal G }}_{M}\leqslant 0.1﹩ and ﹩{{ \mathcal G }}_{M}\leqslant 0.2﹩, compared to only 49% and 84% of the CKS volatile-rich sample distribution (blue). Following the uncertainty propogation procedure described in Section 4.2, we find that rocky systems exhibit enhanced intra-system size uniformity compared to volatile-rich systems at the level of 4.04σ significance. Middle column: 27% of the CKS rocky mass Gini distribution lies above the maximum value for the NEA volatile-rich systems (﹩{{ \mathcal G }}_{M}=0.36﹩). As described in Section 5.3, rocky systems exhibit greater planetary mass diversity compared to volatile-rich systems at the level of 2.61σ significance. Right column: the distribution of ﹩{{ \mathcal G }}_{{ \mathcal P }}﹩ values within our rocky sample (gold) is completely contained within ﹩{{ \mathcal G }}_{{ \mathcal P }}\leqslant 0.1﹩, a value above which 53% of the volatile-rich population resides. As described in Section 6.2, rocky systems exhibit enhanced intra-system spacing uniformity compared to volatile-rich systems at the level of 3.0σ confidence. Gray dashed lines indicate size (﹩{{ \mathcal G }}_{M}=0.25﹩), mass (﹩{{ \mathcal G }}_{M}=0.60﹩), or spacing (﹩{{ \mathcal G }}_{{ \mathcal P }}=0.15﹩) Gini values for the four terrestrial planets in our solar system. We further discuss the contextualization of the inner solar system in Section 8.1.
Paper: Peas-in-a-pod across the Radius Valley: Rocky Systems Are Less Uniform in Mass but More Uniform in Size and Spacing
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Orbital architectures of the 13 high-multiplicity (N ≥ 3) systems in our CKS rocky sample (gold) and the 30 high-multiplicity systems in our CKS volatile-rich sample (blue). This high-N restriction is imposed to avoid concurrent illustration of over 150 systems; the full CKS rocky and volatile-rich samples are described in Section 4.1. Marker sizes and transparency respectively correspond to planetary size and system-wide size uniformity (greater opacity indicates higher ﹩{{ \mathcal G }}_{R}﹩). The generally lighter shading of the rocky systems indicates a qualitative preference for enhanced size uniformity, which we verify with greater statistical rigor in Section 4.2. Within both samples, systems are also plotted in vertical order of decreasing spacing uniformity (increasing ﹩{{ \mathcal G }}_{{ \mathcal P }}﹩). We observe that all rocky systems have ﹩{{ \mathcal G }}_{{ \mathcal P }}\lt 0.1﹩, while approximately half of the volatile-rich systems reside above this regime, indicating comparatively greater intra-system spacing uniformity for the former population.
Paper: Peas-in-a-pod across the Radius Valley: Rocky Systems Are Less Uniform in Mass but More Uniform in Size and Spacing
Authors: Armaan V. Goyal, Songhu Wang
Figure caption: Enhanced size uniformity and mass diversity of the CKS rocky systems are driven by the respective presence of super-Earths and sub-Earths. Left: subject to the testing procedure outlined in Section 4.2, CKS rocky systems containing only sub-Earths (SubEs, R  p  < 1 R ⊕) are more diverse in planetary size than systems containing only super-Earths (SEs, 1 R ⊕ ≤ R  p  ≤ 1.6 R ⊕) with ∼2.0σ significance. Taking our 118 CKS volatile-rich systems as a representative sample of systems containing only sub-Neptunes (SNs), we find that the size uniformity of SubE-only and SN-only systems are consistent within 0.9σ. Right: compared to SE systems, SubE systems are more diverse in planetary mass at the level of ∼2.5σ significance. Taking our 16 NEA volatile-rich systems as a representative sample of systems containing only SNs, we find that the mass uniformity of SE-only and SN-only systems are consistent within 0.9σ.
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Self-consistent atmospheric models of LHS 1140 b compared to the JWST 							data. The top panel shows the massive H2-rich atmosphere 							models with varied metallicities, as well as the small 							H2-dominated atmosphere with CO2 model (“Hycean 							world”). χ 2 = 1406, 506, and 287 for the 1×, 10×, and 100× solar 							metallicity models, respectively, and χ 2 = 470 for the Hycean model (considering 75 degrees of 							freedom). These models are ruled out by the data with a p-value < 0.00001. The bottom panel shows 							the N2- and CO2-dominated atmosphere models. 								χ 2 = 118 for both models.
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Modeled pressure–temperature profiles for LHS 1140 b, considering massive 								H2-rich atmospheres with 1×, 10×, and 100× solar 							metallicity abundances and small (2.2 bars) H2-, 								N2-, and CO2-dominated atmospheres. The small 								H2-dominated atmosphere has 1% CO2, 							corresponding to the proposed “Hycean world” scenario for temperate 							sub-Neptunes (Hu et al. 2021; Madhusudhan et al. 2021). The temperature profiles 							indicate a cold trap at the pressure of ∼104 Pa for the 								H2-rich atmospheres and ∼104.5 Pa for 								N2- and CO2-dominated atmospheres. The 							resulting transmission spectra of these models are shown in Figure 6.