{"total":23,"items":[{"citing_arxiv_id":"2606.26259","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cepheids with giant companions III. Evolutionary modeling of nine binary double Cepheids from the Milky Way and Magellanic Clouds","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T18:02:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Extended q-PED modeling provides first mass estimates for SMC Cepheids and new period-mass-radius and mass-luminosity relations while indicating binary interactions in several systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25517","ref_index":60,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveiling the nature of barium stars. I. Asteroseismic masses and the evolutionary link between Ba dwarfs and giants","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T07:50:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23551","ref_index":278,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observing a 542-day transiting giant with large TTVs: The 2025 transit of HIP 41378 f and new constraints on the outer system","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T16:25:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New 2025 transit timing of HIP 41378 f shows a 7-hour early arrival consistent with TTVs; N-body modeling with TRADES refines ephemerides for planets d, e, and f.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.22619","ref_index":145,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Comparative Study of Two Luminous Red Novae I. Progenitor Modeling and Dust Formation","primary_cat":"astro-ph.SR","submitted_at":"2026-06-21T18:01:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21824","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors","primary_cat":"astro-ph.HE","submitted_at":"2026-06-20T01:25:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19575","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The fate of Earth during the Sun's giant phases: New constraints from ab initio tidal modelling and AGB mass loss","primary_cat":"astro-ph.EP","submitted_at":"2026-06-17T20:28:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Updated ab initio tidal models predict Earth survives the Sun's giant phases, but outcomes depend strongly on AGB mass-loss rates, with L2 Pup observations as proxy indicating survival while low rates lead to engulfment.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13567","ref_index":207,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors","primary_cat":"astro-ph.SR","submitted_at":"2026-06-11T16:56:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"1D models show convective boundary mixing dominates the asteroseismic imprint of accretion in massive stars, robust to semiconvection changes but drastically altered without it, with thermal relaxation as key.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12242","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Shaping the horizontal branch: The role of envelope mass in the evolution of stripped core-helium-burning stars","primary_cat":"astro-ph.SR","submitted_at":"2026-06-10T15:45:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MESA models show residual hydrogen envelope mass sets effective temperature on the horizontal branch, with maximum values of 0.05-0.30 solar masses to avoid later thermally pulsing AGB evolution, plus explanations for blue hook stars and puffed-up pre-HB configurations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12034","ref_index":91,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Oscillations of red giant stars with magnetic damping in the core. II. Mixed mode visibilities on the red-giant branch","primary_cat":"astro-ph.SR","submitted_at":"2026-06-10T12:57:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Synthetic spectra show that observational biases cause dipole mode visibilities to be overestimated by up to 20 percent on the red-giant branch, while partial energy preservation under magnetic damping can produce both present and absent mixed-mode signatures.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07787","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Extending asteroseismic magnetometry across the diverse landscape of magnetic structures","primary_cat":"astro-ph.SR","submitted_at":"2026-06-05T18:59:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Extends magnetogravity polarization formalism to arbitrary magnetic field geometries, revealing avoided crossings and mode conversion below a local field threshold.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07230","ref_index":117,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Study of photometric and spectral variability of the roAp star HD~210684","primary_cat":"astro-ph.SR","submitted_at":"2026-06-05T12:53:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Observational analysis of HD210684 yields rotational period 5.02188 d, magnetic obliquity 77°, and main-sequence age ~1.45 Gyr from photometry, LSD magnetic measurements, and MESA/GYRE modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02732","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Precision constraints on stellar physics from main sequence detached eclipsing binaries","primary_cat":"astro-ph.SR","submitted_at":"2026-06-01T18:00:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bayesian framework with active-learning surrogate for MESA models constrains ages and α_MLT from 38 main-sequence DEBs, recovering some α_MLT values below the solar calibration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02726","ref_index":230,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Accretion of Primordial Black Holes in Stellar Interiors","primary_cat":"astro-ph.HE","submitted_at":"2026-06-01T18:00:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Self-consistent spherical accretion simulations show cooling-enhanced growth of PBHs with radiative efficiency ~10^{-2} in the bremsstrahlung regime, yielding a critical seed mass of ~10^{-16} M_sun to consume a solar-mass star in a Hubble time.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02725","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Can current models predict the local black hole merger rate?","primary_cat":"astro-ph.HE","submitted_at":"2026-06-01T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Theoretical predictions for local BBH merger rates exceed observations by a factor >10 under conservative SFRD and metallicity assumptions, indicating need for revisions in stellar evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.30422","ref_index":64,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Millicharged Particle Constraints from Asymptotic Giant Branch Stars","primary_cat":"hep-ph","submitted_at":"2026-05-28T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New upper bounds on millicharged particles (masses 10-100 keV, charges down to 5e-13) from the AGB-to-HB star ratio in globular clusters, improving prior limits by up to two orders of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22911","ref_index":90,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mergers via failed common envelope as a route towards intermediate-mass stripped stars","primary_cat":"astro-ph.SR","submitted_at":"2026-05-21T18:00:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Failed common envelope mergers yield 6-14 solar mass stripped stars consistent with long-lived core He-burning objects that appear single or in wide binaries from hierarchical triples.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21062","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models","primary_cat":"astro-ph.SR","submitted_at":"2026-05-20T11:46:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The radial expansion of the star is described by the empirical relation log10 Rmax R⊙ =− 1 14 log10 Eheat 8×10 49 erg !2 +3.1,(4) which should be taken as an upper limit (Ogata et al. 2021). The duration of this inflated phaseτ infl can be estimated given the total injected energy,E heat, and the rate at which the star radiates this energy,L max, leading to the relation τinfl =α Eheat Lmax ,(5) withα∼0.18 an efficiency factor (Ogata et al. 2021). The lumi- nosityL max and radiusR max of the inflated companion are found to remain roughly constant for a timeτ infl after the onset of ECI (see Fig.3 in Ogata et al. 2021). The ECI-driven expansion oc- curs on a dynamical timescale (Hirai et al. 2025, although it may be longer, see Chen et al."},{"citing_arxiv_id":"2605.17005","ref_index":127,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Red novae, their progenitors, and remnants","primary_cat":"astro-ph.SR","submitted_at":"2026-05-16T14:06:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A synthesis of observational data on red novae as stellar merger events, including outburst properties, progenitor diversity, and long-term remnants.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23503","ref_index":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Hyperaccreting Neutron Stars inside Massive Envelopes: The Implausibility of Thorne-\\.Zytkow Objects","primary_cat":"astro-ph.HE","submitted_at":"2026-04-26T02:36:37+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":"common-envelope end states. E. Evolutions In this work, we dynamically evolve 2 stellar models with 4 different phases with the NS (total 8 models) in spherical symmetry. In addition, we explore multidimen- sional effects with some models with the 1.4 M ⊙ NS and 15 M⊙ stellar progenitor. Our models are evolved with theGmunucode, which solves GRMHD [52, 53] and Einstein field equations in the conformally flat approximation [54]. Energy- integrated two-moment neutrino transport [39, 40], and nuclear burning [36] modules are also activated in a fully coupled manner. We employ the IMEXCB3a time in- tegrator [55], the Harten-Lax-van Leer (HLL) Riemann solver [56], and a 3rd-order reconstruction piecewise"},{"citing_arxiv_id":"2604.21650","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Modeling of the magnetic stellar wind braking of the ssrAp 33 Lib (HD137949)","primary_cat":"astro-ph.SR","submitted_at":"2026-04-23T13:14:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Magnetic wind braking can slow ssrAp stars like 33 Lib to rotation periods of 80 years or more according to MESA evolution models that include magnetic field and wind changes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.02413","ref_index":86,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Black Hole Mass Gap as a New Probe of Millicharged Particles","primary_cat":"hep-ph","submitted_at":"2026-04-02T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Millicharged particles weaken pulsational pair-instability in massive stars, shifting the lower edge of the black hole mass gap upward and turning gravitational wave observations into a probe for particles with masses 35-200 keV and charges 10^{-10} to 10^{-9}.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"on minicharged particles in models with a hidden photon,JCAP02(2014) 029 [1311.2600]. [84] D. C. Moore, A. D. Rider and G. Gratta,Search for Millicharged Particles Using Optically Levitated Microspheres,Phys. Rev. Lett.113(2014) 251801 [1408.4396]. [85] N. Vinyoles and H. Vogel,Minicharged Particles from the Sun: A Cutting-Edge Bound,JCAP03(2016) 002 [1511.01122]. [86] J. H. Chang, R. Essig and S. D. McDermott, Supernova 1987A Constraints on Sub-GeV Dark Sectors, Millicharged Particles, the QCD Axion, and an Axion-like Particle,JHEP09(2018) 051 [1803.00993]. [87] G. Magill, R. Plestid, M. Pospelov and Y.-D. Tsai, Millicharged particles in neutrino experiments,Phys. Rev. Lett.122(2019) 071801 [1806.03310]. [88] X."},{"citing_arxiv_id":"2602.15119","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detection horizon for the neutrino burst from the stellar helium flash","primary_cat":"astro-ph.SR","submitted_at":"2026-02-16T19:00:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The helium flash produces a neutrino burst with a 1.7 MeV line detectable up to almost 3 pc in future facilities, but asteroseismology remains the practical probe for now.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.06741","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Diagnosing the Properties and Evolutionary Fates of Black Hole and Wolf-Rayet X-ray Binaries as Potential Gravitational Wave Sources for the LIGO-Virgo-KAGRA Network","primary_cat":"astro-ph.HE","submitted_at":"2025-10-08T07:54:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MESA binary evolution simulations with revised Bondi-Hoyle accretion efficiency and observational constraints yield lower BH mass upper limits for IC 10 X-1 and NGC 300 X-1 and predict Hubble-time BBH mergers for all three systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}