{"total":67,"items":[{"citing_arxiv_id":"2605.23768","ref_index":263,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GMRT Survey of Radio Emission from Magnetic Massive Stars -- I: Emission from Single Stars at sub-GHz Frequencies","primary_cat":"astro-ph.SR","submitted_at":"2026-05-22T15:38:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GMRT sub-GHz survey of 44 magnetic hot stars detects emission in 11 cases and finds scaling of radio luminosity with magnetic field and rotation period consistent with higher-frequency work.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23637","ref_index":69,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Long-term optical and near-infrared photometric evolution of SN 2019vxm, an interacting Type IIn 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KIC 8957954 KIC 10593759 KIC 8302455 TIC 207398432 Mode Detached Binary Detached Binary Detached Binary Detached Binary g1 0.32 0.32 0.32 0.32 g2 0.32 0.32 0.32 0.32 A1 0.5 0.5 0.5 0.5 A2 0.5 0.5 0.5 0.5 i(deg) 88.79(38) 80.19(47) 84.30(4) 88.79(38) e . . .0.0015(3). . . . . . ω(rad). . .2.63(39). . . . . . T1(K) 5811(fixed) 5811(fixed) 5931(fixed) 6184(fixed) T2/T1 0.994(2) 1.002(6) 1.000(7) 0.770(29) q(M2/M1) 0.985(fixed) 0.978(fixed) 0.993(fixed) 0.992(fixed) Ω1 12.94(1.11) 11.71(90) 14.85(97) 16.81(36) Ω2 13.44(93) 11.67(25) 14.76(69) 5.37(2) L1/(L1 +L 2)band 0."},{"citing_arxiv_id":"2605.12391","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Trajectory-Agnostic Asteroid Detection in TESS with Deep Learning","primary_cat":"astro-ph.EP","submitted_at":"2026-05-12T16:56:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A W-Net deep learning model detects asteroids in TESS data independently of trajectory by rotating training image cubes and using adaptive normalization for data 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The Article number, page 15 A&A proofs:manuscript no. aa 1250 1500 1750 2000 2250 2500 2750 3000 3250 BJDTDB − 2457000.0 4 2 0 2 4 6 O-C (min) Tref TESS Fig. D.3: O−C plot displaying the observed (O) minus calculated (C) transit times, relative to the linear ephemeris of TOI-159 b. 10 1 100 101 Mass [MJ] 10 1 100 101 Planet density [g cm 3] TOI 159 b 10 S 150 S 1000 S 4000 5000 6000 7000 8000 Stellar Teff (K) Fig. D.4: Planet bulk density as a function of planetary mass of well-characterised irradiated (F ⋆ >2×10 8 erg s −1 cm−2) gi- ant planets. The stellarT eff is colour-coded, while the size of the dots reflects the planet insolation. The green shaded area highlights the mass-radius relation for giant planets in the ab-"},{"citing_arxiv_id":"2604.26398","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Phenomenological Classification of TESS Eclipsing Binaries","primary_cat":"astro-ph.SR","submitted_at":"2026-04-29T08:08:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A neural network classifies 20,196 TESS eclipsing binaries into 13,376 EA, 2,114 EB, and 4,706 EW systems after achieving 99% accuracy on held-out test data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25594","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Asteroseismic analysis of RY Leporis: the post-main sequence HADS in a binary system","primary_cat":"astro-ph.SR","submitted_at":"2026-04-28T13:02:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Asteroseismic modeling of RY Leporis gives a mass of ~2 solar masses and age of ~730 Myr, locating it in the post-main-sequence hydrogen shell-burning stage with consistent metallicity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24516","ref_index":32,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"StarCLR: Contrastive Learning Representation for Astronomical Light Curves","primary_cat":"astro-ph.SR","submitted_at":"2026-04-27T14:18:49+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"StarCLR pretrains on TESS light curves via contrastive learning on overlapping subsequences and improves variable star classification F1 scores over scratch-trained models when fine-tuned on TESS, ZTF, and Gaia.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20325","ref_index":268,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stellar flare-driven evolution of primordial early exo-Earth atmospheres: Insights from a Young M Dwarf Flare model","primary_cat":"astro-ph.EP","submitted_at":"2026-04-22T08:21:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Young M dwarf flares exert greater chemical stress on primordial exo-Earth atmospheres than previous models, with potential for lasting changes in mixing ratios especially for low-abundance species.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20314","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Shortest period for outer orbit in compact hierarchical triple? Discovery of SB1 around V0885 Per","primary_cat":"astro-ph.SR","submitted_at":"2026-04-22T08:12:26+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19918","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stability of Multiplanet Systems Through Hot Jupiter Destruction","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T18:53:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Roche lobe overflow destruction of hot Jupiters clears all companions from the sub-Jovian desert inside ~4 days while most observed companions remain stable, unlike tidal disruption during high-eccentricity migration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19255","ref_index":102,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Rapidly oscillating Ap stars observed with TESS. The LAMOST Ap sample and 49 Cam","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T09:18:30+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An algorithm applied to TESS data identifies four new rapidly oscillating Ap stars from LAMOST-classified Ap stars and known candidates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19179","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A tidally detached super Neptune on a strongly misaligned retrograde orbit","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T07:44:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TOI-1710 b has a true obliquity of 149 degrees indicating retrograde motion, favoring high-eccentricity migration via planet-planet scattering and Kozai-Lidov cycles for this tidally detached super-Neptune.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18281","ref_index":22,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Two Potential Exoplanets around A-type Stars Selected from 18 Planetary Candidates","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T13:54:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Two TESS candidates around A-type stars are flagged as promising exoplanets after low false-positive probabilities are calculated for 18 screened objects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.17382","ref_index":86,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Red Giant Interiors with G-Dominated Mixed Modes I: The Cases of KIC 9145955, KIC 9970396, KIC 9882316 and KIC 11968334","primary_cat":"astro-ph.SR","submitted_at":"2026-04-19T11:16:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Asteroseismic fits to g-dominated mixed modes in four red giants suggest convective overshooting rises with mass and yield a core rotation rate of 0.7409 μHz for KIC 11968334.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16073","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Machine learning isotope shifts in molecular energy levels","primary_cat":"astro-ph.EP","submitted_at":"2026-04-17T13:58:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Neural network corrects residual errors in isotopologue energy extrapolations for CO2 (MAE reduction in >87% of levels vs Marvel) and transfers patterns to improve CO predictions in >93% of samples.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Since the detection of 51 Pegasi b in 1995 [1], which marked the first confirmation of a planet orbiting a main-sequence star other than our Sun, the catalogue of con- firmed exoplanets has expanded rapidly. The number of confirmed exoplanets has now passed 6000, a milestone achieved through the tireless operations of space-based missions such as Ke- pler [2] and the Transiting Exoplanet Survey Satellite (TESS) [3], alongside ground-based radial velocity surveys [4]. This initial era of discovery, focused primarily on demographics and orbital dynamics, has now given way to a new phase: atmospheric characterization. Beyond addressing long-standing questions about habitability and the potential for life, the chemical composition of an exoplanetary atmosphere also provides a fossil record of the planet's"},{"citing_arxiv_id":"2604.13650","ref_index":96,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Prospects for GRB Afterglow Discovery with the Eric and Wendy Schmidt Observatory System","primary_cat":"astro-ph.HE","submitted_at":"2026-04-15T09:17:44+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The Argus Array and DSA are projected to detect 47 and 82 long GRB afterglows per year respectively from Fermi triggers, along with over 100 independent detections annually and some short GRB counterparts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.13631","ref_index":44,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Fundamental effective temperature measurements for eclipsing binary stars -- VIII. NIRPS spectroscopy of CD-27 2812","primary_cat":"astro-ph.SR","submitted_at":"2026-04-15T08:59:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Model-independent masses and radii plus effective temperatures are derived for the F9 V primary (M1=1.36 Msun, R1=1.72 Rsun, Teff=6197 K) and M-dwarf secondary (M2=0.56 Msun, R2=0.53 Rsun, Teff=3770 K) in CD-27 2812.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.12705","ref_index":45,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Self-Lensing Signals in Binary Systems Containing White Dwarfs with Neutron star or Stellar-mass Black hole Companions","primary_cat":"astro-ph.SR","submitted_at":"2026-04-14T13:18:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Self-lensing signals occur with probabilities of roughly 10^{-3} in WD+NS systems and 10^{-2} in WD+BH systems; TESS could detect at least one if 8% of white dwarfs have NS companions and 3% have BH companions, while Roman cannot.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09834","ref_index":113,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Observational and Dynamical Constraints on an Unseen Outer Perturber in the GJ 436 Hot Neptune System","primary_cat":"astro-ph.EP","submitted_at":"2026-04-10T19:08:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Archival RV and astrometric data plus three-body simulations constrain an unseen outer perturber in the GJ 436 system to sub-Jovian masses at a_c ≳ 6.8 AU, supporting Kozai-Lidov migration as the source of the hot Neptune's polar eccentric orbit.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09152","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Machine Learning as a Transformative Tool for (Exo-)Planetary Science","primary_cat":"astro-ph.EP","submitted_at":"2026-04-10T09:39:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper reviews ML applications for sequence modeling, pattern recognition, and generative Bayesian analysis to tackle heterogeneous data challenges in (exo)planetary science.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Bailey, arXiv e-prints arXiv:1302.3675 (2013). DOI 10.48550/arXiv.1302.3675 [4] P.H. Abelson, Science197(4308), 1039 (1977). DOI 10.1126/science.197.4308.1039 [5] C.E. Kohlhase, P.A. Penzo, Space Science Reviews21(2), 77 (1977). DOI 10.1007/BF00200846 [6] W.J. Borucki, D. Koch, G. Basri, et al., Science327(5968), 977 (2010). DOI 10.1126/science.1185402 [7] G.R. Ricker, J.N. Winn, R. Vanderspek, et al., Journal of Astronom- ical Telescopes, Instruments, and Systems1, 014003 (2015). DOI 10.1117/1.JATIS.1.1.014003 [8] S.J. Bolton, J. Lunine, D. Stevenson, et al., Space Science Reviews213(1-4), 5 (2017). DOI 10.1007/s11214-017-0429-6 [9] J.P. Gardner, J.C. Mather, M. Clampin, et al., Space Science Reviews123(4),"},{"citing_arxiv_id":"2604.09011","ref_index":170,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The formation of planetary systems: physics, populations, and architectures","primary_cat":"astro-ph.EP","submitted_at":"2026-04-10T06:23:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The Bern Model has incorporated MHD disk evolution, pebble accretion, and improved interiors, yielding quantitative matches to exoplanet mass functions, radius distributions, and system architectures.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A more detailed explanation of the results and limitations can be found in [98]. 3.6 Emerging planetary system architectures The study and classification of planetary system architectures are essential for a better understanding of the formation and evolution of planetary systems, including our own Solar System. The Corot [168], Kepler [169], and now TESS [170] missions have revolutionized the study of planetary systems by detecting thousands of multi- planet systems. This increase in the detection of such systems has expanded the focus beyond just the diversity of exoplanets to also include the diversity of planetary systems. By studying exoplanet diversity, we can test and refine planetary formation models, just as studying the diversity of planetary systems allows us to improve our"},{"citing_arxiv_id":"2604.07976","ref_index":68,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The puzzling story of flare inactive ultra fast rotating M dwarfs -- III. Investigating X-ray Activity","primary_cat":"astro-ph.SR","submitted_at":"2026-04-09T08:43:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"X-ray data show ultra-fast rotating M dwarfs have saturated or enhanced coronal emission, ruling out supersaturation as the cause of their unexpectedly low flaring activity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}