{"total":14,"items":[{"citing_arxiv_id":"2606.30865","ref_index":106,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Scalarization and descalarization in hyperbolic encounters of black holes","primary_cat":"gr-qc","submitted_at":"2026-06-29T19:54:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Numerical relativity in the decoupling limit reveals dynamical scalarization and spin-induced (de)scalarization during hyperbolic black hole encounters for both signs of the coupling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27431","ref_index":44,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Critical collapse of vacuum spacetimes: Nakamura wave initial data","primary_cat":"gr-qc","submitted_at":"2026-06-25T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations with Nakamura wave initial data confirm approximately discretely self-similar threshold solutions in vacuum gravitational wave collapse, but without exact self-similarity or a unique critical solution, consistent with prior studies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21549","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Binary Black Hole Coalescence and the Dynamics of Scalar Hair in Einstein-Maxwell-Scalar Theory","primary_cat":"gr-qc","submitted_at":"2026-06-19T15:45:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Numerical simulations of binary black hole coalescence in EMS theory show dynamic triggering of scalar hair depending on coupling strength and remnant charge.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12542","ref_index":69,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Implementation of multi-grid Poisson solver in numerical relativity and its application to gravitational collapse of massive star","primary_cat":"astro-ph.HE","submitted_at":"2026-06-10T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A grid-based multi-grid Poisson solver is implemented in numerical relativity, tested on puncture black holes and neutron stars, and used in a neutrino-radiation hydrodynamics simulation of 9 solar mass star collapse up to core bounce with high conservation accuracy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11299","ref_index":151,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A magnetar formation in binary neutron star merger","primary_cat":"astro-ph.HE","submitted_at":"2026-06-09T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"W. Terry, E. G. Zweibel, M. J. Pueschel, and R. Fan, Nature (London)649, 848 (2026). [148] D. R. Lorimer, Living Rev. Rel.11, 8 (2008), arXiv:0811.0762 [astro-ph]. [149] K. Kiuchi, L. E. Held, Y. Sekiguchi, and M. Shibata, Phys. Rev. D106, 124041 (2022), arXiv:2205.04487 [astro-ph.HE]. [150] M. Shibata and N. Takashi, Phys. Rev. D52, 5428 (1995). [151] T. W. Baumgarte and S. L. Shapiro, Phys. Rev. D59, 024007 (1998), arXiv:gr-qc/9810065. [152] J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, and J. van Meter, Phys. Rev. Lett.96, 111102 (2006), arXiv:gr-qc/0511103. [153] M. Campanelli, C. O. Lousto, P. Marronetti, and Y. Zlochower, Phys. Rev. Lett.96, 111101 (2006), arXiv:gr-qc/0511048. [154] D."},{"citing_arxiv_id":"2605.20320","ref_index":94,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The third wheel: ringdown and lensing of triple systems","primary_cat":"gr-qc","submitted_at":"2026-05-19T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Numerical relativity simulations of triple black hole systems reveal redshift effects and gravitational lensing in ringdown signals from head-on mergers, with no additional black hole formation from amplified waves.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"a fifth-order Kreiss-Oliger dissipation operator with co- efficientϵ diss = 0.2and Sommerfeld radiative boundary conditions [92]. Gravitational radiation is extracted at selected points in the domain via the computation of the Newman- Penrose scalarΨ 4, following the implementation de- scribed in [89]. Local properties of BHs are computed using theQuasiLocalMeasuresthorn [94], while their apparent horizons are located with theAHFinderDi- rectthorn [95]. Sinceweconsidernon-spinningBHsinitiallyatrest, we adopt Brill-Lindquist-type initial data [96, 97]. The nor- malization is chosen so that the total mass of the space- timeMequals the sum of the individual BH massesm i as measured by the apparent horizon finder. The simulation domain is a three-dimensional Carte-"},{"citing_arxiv_id":"2604.25582","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Lessons from binary dynamics of inspiralling equal-mass boson-star mergers","primary_cat":"gr-qc","submitted_at":"2026-04-28T12:50:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Numerical simulations of equal-mass boson-star mergers reveal larger waveform deviations from black-hole binaries in late inspiral and merger, plus odd multipole excitations for certain scalar-field phases, with some signals degenerate until IMR consistency tests are applied.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA, Living Rev. Rel.19, 1 (2016), arXiv:1304.0670 [gr-qc]. [47] J. E. Thompson, C. Hoy, E. Fauchon-Jones, and M. Han- nam, Use and interpretation of signal-model indistin- guishability measures for gravitational-wave astronomy, Phys. Rev. D112, 064011 (2025), arXiv:2506.10530 [gr- qc]. [48] S. T. McWilliams, B. J. Kelly, and J. G. Baker, Observing mergers of non-spinning black-hole binaries, Phys. Rev. D82, 024014 (2010), arXiv:1004.0961 [gr-qc]. [49] M. P¨ urrer and C.-J. Haster, Gravitational waveform ac- curacy requirements for future ground-based detectors, Phys. Rev. Res.2, 023151 (2020), arXiv:1912.10055 [gr- qc]. [50] M. A. Scheel et al."},{"citing_arxiv_id":"2604.15240","ref_index":127,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Boson star-black hole binaries: initial data and head-on collisions","primary_cat":"gr-qc","submitted_at":"2026-04-16T17:15:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A one-body conformal-factor correction stabilizes boson star-black hole initial data, enabling gravitational-wave analysis that shows higher multipoles can discriminate mixed mergers from pure black-hole binaries.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"zolla, \"Constraint damping of the conformal and co- variant formulation of the Z4 system in simulations of binary neutron stars,\" Phys. Rev. D88, 064049 (2013), arXiv:1307.7391 [gr-qc]. [126] Robin Croft, \"Local continuity of angular momen- tum and noether charge for matter in general rel- ativity,\" Class. Quant. Grav.40, 105007 (2023), arXiv:2203.13845 [gr-qc]. [127] Tamara Evstafyeva, Roxana Rosca-Mead, Ulrich Sper- hake, and Bernd Brugmann, \"Boson stars in massless and massive scalar-tensor gravity,\" Phys. Rev. D108, 104064 (2023), arXiv:2310.05200 [gr-qc]. 20 [128] Tamara Evstafyeva, Ulrich Sperhake, Isobel M. Romero-Shaw, and Michalis Agathos, \"Gravitational- Wave Data Analysis with High-Precision Numerical"},{"citing_arxiv_id":"2604.06312","ref_index":78,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Black Hole-Boson Star Binaries: Gravitational Wave Signals and Tidal Disruption","primary_cat":"gr-qc","submitted_at":"2026-04-07T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical simulations of black hole-boson star binaries show that scalar self-interactions can suppress tidal disruption while radiative efficiency depends on the chosen potential.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"ness designed to predominantly capture the distribution of scalar matter in the bulk rather than at larger radii, Cmax ..= max r>0 m(r) r ,(10) wheremis the aspect mass enclosed within a radiusr. C. Computational Framework The BS-BH mergers presented in this work have been simulated usinggrchombo[76, 77], an open-source code capable of evolving the the Baumgarte-Shapiro-Shibata- Nakamura (BSSN) [78, 79] and conformal covariant Z4 (CCZ4) [80] formulations of numerical relativity with full adaptive mesh refinement (AMR). In this work, we ex- clusively use the CCZ4 formulation due to its constraint- damping properties; cf. Refs. [27, 74], in which dynami- cal evolutions of isolated, stationary BSs are seen to ex- hibit long-lasting linear growth in the Hamiltonian con-"},{"citing_arxiv_id":"2604.00978","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nonlinear Lattice Framework for Inflation: Bridging stochastic inflation and the $\\delta{N}$ formalism","primary_cat":"gr-qc","submitted_at":"2026-04-01T14:48:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"A shear-free lattice method bridges stochastic inflation and δN formalism by enabling fully nonlinear calculations of curvature perturbations in single-field models with ultra-slow-roll phases.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"contributions of the spatial curvature to thelocalFriedmann constraint, or (c) the correct volume weighting needed to construct uniform-density hypersurfaces forδN and related - 2 - observables. Moreover, although in the typical inflationary models that are conducive to parametric resonance, the influence of local gravity on the small-scale phenomena characteristic of such an epoch is found to be small [49, 50], in models with aUSR epoch or an upward turn in the potential [51] driving inflation, the influence of inhomogeneous geometry cannot be assumed to remain subdominant. In parallel with these developments, fully relativistic simulations of inflationary dynam- ics and preheating have become increasingly feasible. Using Baumgarte-Shapiro-Shibata-"},{"citing_arxiv_id":"2602.01830","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hyperbolicity analysis of the linearised 3+1 formulation in the Teleparallel Equivalent of General Relativity","primary_cat":"gr-qc","submitted_at":"2026-02-02T09:05:15+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The linearized 3+1 TEGR system has imaginary eigenvalues in its principal symbol but becomes strongly hyperbolic after gauge fixing isolated problematic sectors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.00307","ref_index":99,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Spin-up and mass-gain in hyperbolic encounters of spinning black holes","primary_cat":"gr-qc","submitted_at":"2025-10-31T23:11:47+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":"2508.21216","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Persistence of post-Newtonian amplitude structure in binary black hole mergers","primary_cat":"gr-qc","submitted_at":"2025-08-28T21:11:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fits to numerical relativity data indicate that leading-order post-Newtonian dependence on mass ratio persists in several modes of binary black hole mergers through the merger, while low-degree polynomials capture deviations in higher modes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1202.5809","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dynamical Boson Stars","primary_cat":"gr-qc","submitted_at":"2012-02-27T00:47:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Boson stars are particle-like solutions in general relativity that model dark matter, black hole mimickers, and binary systems.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2016 for a review on numerical methods to find stationary gravitational solutions). Equation (38) is linear and homogeneous in α and one is therefore able to rescale the field consistent with Eq. (44). We can get rid of the constants in the equations by re-scaling the variables in the following manner ˜φ0≡ √ 4π Gφ0 , ˜r≡ m r , ˜t≡ ω t , ˜α≡ (m/ω)α . (45) Notice that the form of the metric in Eq. (33) resembles Schwarzschild allowing the association a2≡ (1− 2 M/r)−1, where M is the ADM mass of 14 Steven L. Liebling, Carlos Palenzuela the spacetime. This allows us to define a more general mass aspect function M(r, t) = r 2 ( 1− 1 a2(r, t) ) , (46) which measures the total mass contained in a coordinate sphere of radius r at"}],"limit":50,"offset":0}