{"total":15,"items":[{"citing_arxiv_id":"2606.23576","ref_index":86,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Corotating Interaction Regions (CIRs): evolution over a solar lifetime","primary_cat":"astro-ph.SR","submitted_at":"2026-06-22T16:42:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"CIRs form closer to young fast-rotating solar-mass stars, migrate outward as rotation slows, and produced 10^3 to 10^7 times more energetic particles than today during the Hadean period.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18355","ref_index":127,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Revisiting the Exo-Mercury Candidate GJ 367 b with ESPRESSO and a Self-Consistent Tidal Distortion Model","primary_cat":"astro-ph.EP","submitted_at":"2026-06-16T18:03:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Revised mass of 0.503 M_Earth and radius of 0.736 R_Earth for GJ 367 b give a density of 6.9 g cm^{-3} and an iron fraction of 50-70% via new tidal and composition modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12732","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"X-ray Emission and Stellar Ages of Sun-Like Stars","primary_cat":"astro-ph.SR","submitted_at":"2026-06-10T22:43:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Observational analysis of 85 FGK stars yields X-ray luminosity and temperature relations with age, confirming t^{-1.5} decay in soft band while noting increased scatter in harder band at older ages.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11292","ref_index":92,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Revealing the Origin of Desert Dwellers via Stellar Obliquities","primary_cat":"astro-ph.EP","submitted_at":"2026-06-09T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Roche lobe overflow during gas giant destruction aligns stellar spins with orbits within tens of degrees regardless of starting conditions, offering an observable to differentiate this mechanism from high-eccentricity migration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09485","ref_index":132,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Quantifying isochrone-based age uncertainties for rapidly rotating A-type stars","primary_cat":"astro-ph.SR","submitted_at":"2026-06-08T13:40:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A population-synthesis framework shows rotation and unresolved companions bias isochrone ages by a factor of at least 2 near the ZAMS and by 31% for older A stars, adding ~0.1 solar mass and ~180 Myr random uncertainties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04927","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stellar Activity Cycles Grow Longer and Weaker Before Disappearing","primary_cat":"physics.gen-ph","submitted_at":"2026-06-03T14:21:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New California Legacy Survey data confirms stellar activity cycles grow longer and weaker before disappearing, resolving the Sun's apparent outlier status in evolutionary trends.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23018","ref_index":127,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Gaia Exoplanet Orbits, Demographics, and Evolution Survey (GEODES): Characteristics of Three Long-Period Companions Accelerating their Host Stars","primary_cat":"astro-ph.EP","submitted_at":"2026-05-21T20:41:14+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Three accelerating stars yield one stellar companion at 166 AU, one 45 Jupiter-mass object at ~18 AU, and one 9.5 Jupiter-mass object at 6.4 AU that is 65% likely to be a planet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22618","ref_index":192,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"HWO Target Stars and Systems: Activity and Rotation Catalog (ARC) of Potential Target Stars for the Habitable Worlds Observatory","primary_cat":"astro-ph.SR","submitted_at":"2026-05-21T15:30:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Collates archival stellar activity and rotation data for potential HWO targets, finding measurements for at least 70% of high-interest systems but activity cycles for fewer than 20%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20660","ref_index":110,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Formation of extremely low-mass white dwarf binaries undergoing enhanced angular momentum loss","primary_cat":"astro-ph.SR","submitted_at":"2026-05-20T03:26:46+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"and the center of massx cm = 1/(1 +q) of the system, is described by the separationx L2 −x cm. A. Picco et al. (2024) calculated a numerical solution for (x L2 −x cm)2, which is (xL2 −x cm)2(q)≃1 + 5X n=1 an ×    q−(n−n0) q≥1 q(n−n0) q <1, (8) wheren 0 = 0.658,a 1 = 1.544,a 2 =−3.118,a 3 = 4.387, a4 =−3.567,a 5 = 1.190. For the AML induced by MB, we adopt the standard Skumanich prescription (A. Skumanich 1972; S. Rap- paport et al. 1983) withγ MB = 3. It is worth noting that the effectiveness of MB depends on the mass of the donor's convective envelope. Following P. Podsiadlowski et al. (2002), for convective envelopes with fractional massesq conv <0.02, we reduce the MB efficiency by a factore 1−0.02/qconv. GW radiation plays a crucial role in short-period bi-"},{"citing_arxiv_id":"2605.12647","ref_index":114,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The HAges Catalog: Stellar Ages for High Priority HWO Target Stars","primary_cat":"astro-ph.SR","submitted_at":"2026-05-12T18:44:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The HAges catalog compiles published asteroseismic and gyrochronological ages for 659 HWO target stars, finding that only ~5% have asteroseismic ages and ~20% have gyrochronal ages.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"sured rotation period to its age through a process known as magnetic braking. Cool stars with convective en- velopes generate magnetic fields that couple to their ion- ized stellar winds. Magnetized winds carry away angular momentum along magnetic field lines, causing a star's rotation to steadily slow over billions of years in a pre- dictable manner (A. Skumanich 1972). Obtaining precise ages through either asteroseismol- ogy or gyrochronology is possible for the predominantly FGK-type dwarfs in the top tiers of the TSS25 list. For asteroseismology, statistical precisions of<20% in age are common for well-characterized solar-like oscillators, with uncertainties of≲10% possible for the best charac- terized stars (e."},{"citing_arxiv_id":"2605.04591","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spectroscopic Disentangling Revealed the Tertiary Component in the Multiple System EM Boo","primary_cat":"astro-ph.SR","submitted_at":"2026-05-06T07:41:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Tertiary in EM Boo is A-F type with Teff=7000K; system distance ~300 pc indicates Gaia DR3 underestimates true distance due to multiplicity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.07976","ref_index":72,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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},{"citing_arxiv_id":"2603.05586","ref_index":82,"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":"2601.11943","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Dynamo Confinement Scenario for the Solar Tachocline and its Implications for Spin-down in the Radiative Spreading Regime","primary_cat":"astro-ph.SR","submitted_at":"2026-01-17T07:33:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dynamo-generated magnetic fields confine the tachocline against radiative spreading in global simulations, with stronger stable stratification producing longer cycles, deeper penetration via skin effect, and better confinement plus interior spin-down transmission.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.10569","ref_index":25,"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}