{"total":12,"items":[{"citing_arxiv_id":"2605.12324","ref_index":107,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An Ultra-Short Period Super-Earth and a Sub-Neptune Orbiting the K dwarf TOI-4311","primary_cat":"astro-ph.EP","submitted_at":"2026-05-12T16:07:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TOI-4311 hosts a 0.99-day super-Earth (1.38 R_earth, 4.5 M_earth) and 15-day sub-Neptune (2.47 R_earth), plus a candidate 38-day planet, with the dense inner planet potentially challenging formation theories given the host's galactic population.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08051","ref_index":33,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Inferring Asteroseismic Parameters from Short Observations Using Deep Learning: Application to TESS and K2 Red Giants","primary_cat":"astro-ph.SR","submitted_at":"2026-05-08T17:41:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Deep learning infers Δν and ν_max from one-month TESS and K2 observations of red giants with reliable results for ~50% of Kepler/K2 samples and ~23% of TESS stars, plus ΔΠ1 for ~200 K2 young red giants that match known patterns.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05468","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A single power law for the TRAPPIST-1 flare distribution across four orders of magnitude in energy","primary_cat":"astro-ph.SR","submitted_at":"2026-05-06T21:48:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"TRAPPIST-1 flares follow a single power law N(≥E_TESS) ∝ E_TESS^{-0.753} from 10^{29} to 10^{33} erg after sensitivity corrections and bandpass conversion.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"linear high-energy tail of the cumulative FFD, selecting flares withE (K2) TESS ≥E min, whereE min = 3.6×10 30 erg (see Appendix D for the choice ofE min), and compute the cumulative flare rate asν (K2)(> E TESS) =N(> ETESS)/∆T (K2) obs . We model the cumulative FFD of the combined JWST and K2 datasets with a single power law, ν(E > E TESS) =A \u0012 E E0 \u0013−β ,(14) whereβis the cumulative power-law slope andAis the normalization defined as the cumulative flare rate at the 6 28 29 30 31 32 33 log ETESS [erg] 3 2 1 0 1 2 log N( E) [per day] Sun TPRAPPIST-1 analogs Howard+2025 JWST Berardo+2025 HST Seli+2021 TRAPPIST-1 analogs this work K2 this work JWST corrected JWST, this work corrected JWST + K2 fit: = 1 = 0."},{"citing_arxiv_id":"2604.26398","ref_index":15,"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":"2604.17382","ref_index":52,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2604.07437","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"ASTRAFier: A Novel and Scalable Transformer-based Stellar Variability Classifier","primary_cat":"astro-ph.IM","submitted_at":"2026-04-08T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ASTRAFier is a Transformer-BiLSTM-CNN model that classifies stellar variability from light curves, reporting 94.26% accuracy on Kepler data and 88.22% on TESS, then applied to 2.8 million TESS curves to release a catalog.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.06602","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"UMI: GPU-Accelerated Asymmetric Robust Estimator for Photometric Detrending in Exoplanet Transit Searches","primary_cat":"astro-ph.IM","submitted_at":"2026-04-08T02:37:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"UMI is an asymmetric version of the Tukey bisquare estimator with upper-RMS scaling that improves transit signal recovery while running much faster on GPUs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.05305","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Scientific Validation of the SPARC4 Pipeline: Multi-band Imaging, Polarimetry, and Photometric Time Series for Improved Characterization of Transiting Exoplanets","primary_cat":"astro-ph.EP","submitted_at":"2026-04-07T01:20:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The SPARC4 pipeline delivers 0.02% photometric and ~0.02% polarimetric precision on transiting exoplanet observations and refines planetary parameters through joint modeling with TESS or K2 data.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"1±1.6 0.27(8) 0.15(13) only TESS data 58438.20150(35) 2.1751844(5) 3.83±0.05 0.08573(29) 87.4±1.30.27(30) 0.09(6)TESS+SP ARC4 58438.20151(23) FIXED 3.67±0.15 0.0870(11) 82.8±2.3 0.02(7) 0.42(19) 0.7±0.1 SPARC4 g band 58438.20137(12) FIXED 3.825±0.021 0.08481(26) 89.0±1.2 0.07(4) 0.55(9) 1.1±0.1 SPARC4 r band 58438.20145(15) FIXED 3.870±0.010 0.08517(24) 89.9±0.8 0.35(2) 0.004(21) 1.1±0.1 SPARC4 i band 58438.20168(23) FIXED 3.890±0.018 0.08651(35) 89.6±1.3 0.20(6) 0.04(10) 1.1±0.1 SPARC4 z band HATS-23 57072.8527(7) 2.1605160(50) 6.1 0.4 −0.3 0.159(20) 81.0 +0.9 −0.6 0.3728 0.3215 Bento et al. (2017) 58654.3462(11) 2.1605122(21) 8.7±1.8 0.099(16) 86.3±2.9 0.8(4) 0.4(4) only TESS data 58654.3463(11) 2."},{"citing_arxiv_id":"2603.18143","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"TESS light curves of two new magnetic cataclysmic variables: an asynchronous polar at the period minimum, and an eclipsing system with a large spin-to-orbit ratio","primary_cat":"astro-ph.SR","submitted_at":"2026-03-18T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Two new short-period asynchronous magnetic cataclysmic variables were found, one candidate at the period minimum with spin-to-orbit ratio 0.9879 and an eclipsing system with ratio 0.867, supporting magnetic synchronization predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.05586","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The TESS All-Sky Rotation Survey: Periods for 1,046,317 Stars Within 500 pc","primary_cat":"astro-ph.SR","submitted_at":"2026-03-05T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The TESS All-Sky Rotation Survey provides periods for 1,046,317 stars within 500 pc, with an estimated 93% being true rotation periods, and includes a method to correct half-period aliases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2401.14703","ref_index":75,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc","primary_cat":"astro-ph.SR","submitted_at":"2024-01-26T08:23:57+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reports 23.5% ±2.0% stellar multiplicity rate and 28.8% ±2.1% companion rate for M dwarfs in a 15 pc volume-limited sample from speckle imaging plus literature, with separation peaks at 198 au for planet hosts vs 5.57 au otherwise.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(60) Luyten (1997); (61) Luyten (1998); (62) Malo et al. (2014); (63) Mart' ın et al. (2000); (64) McCarthy & Henry (1987); (65) McCarthy et al. (1988); (66) McCarthy et al. (1991); (67) Montagnier et al. (2006); (68) Osvalds & Osvalds (1959);(69) Reid & Gizis (1997); (70) Reiners & Basri (2010); (71) Reuyl (1941); (72) Richichi et al. (1996); (73) Riedel et al. (2010); (74) Rossiter (1955); (75) Skrutskie et al. (2006); (76) Sperauskas et al. (2019); (77) Struve (1837); (78) Tokovinin et al. (2010); (79) Tomkin & Pettersen (1986); (80) van Biesbroeck (1961); (81) van Biesbroeck (1974); (82) van den Bos (1937); (83) van den Bos (1950); (84) van den Bos (1951); (85) Vrijmoet et al. (2022); (86) Vyssotsky (1927); (87) Ward-Duong et al. (2015); (88) Wendell (1913); (89) Wilson (1954); (90) Winters et al."},{"citing_arxiv_id":"1906.10569","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Influence of magnetic activity on the determination of stellar parameters through asteroseismology","primary_cat":"astro-ph.SR","submitted_at":"2019-06-25T14:37:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Magnetic activity induces frequency shifts that bias asteroseismic age estimates by up to 10% and helium abundance by up to 3% in solar-like stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}