{"total":22,"items":[{"citing_arxiv_id":"2605.22174","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark photon -- Assisted Primordial Magnetogenesis","primary_cat":"astro-ph.CO","submitted_at":"2026-05-21T08:44:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Coupling dark photons to standard photons enables adequate primordial magnetogenesis without strong-coupling or backreaction issues.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21092","ref_index":105,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Audible Axion Magnetogenesis: Linking Intergalactic Magnetic Fields and Gravitational Waves","primary_cat":"hep-ph","submitted_at":"2026-05-20T12:24:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Axion-like particles in the trapped misalignment mechanism produce observable gravitational waves while generating intergalactic magnetic fields that exceed blazar lower bounds in the parameter space promising for gravitational wave detection.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Brandenburg, K. Enqvist, and P. Olesen, Phys. Lett. B 392, 395 (1997), arXiv:hep-ph/9608422. [102] P. Olesen, Phys. Lett. B 398, 321 (1997), arXiv:astro- ph/9610154. [103] R. Banerjee and K. Jedamzik, Phys. Rev. D 70, 123003 (2004), arXiv:astro-ph/0410032. [104] S. Candelaresi and A. Brandenburg, Phys. Rev. E 84, 016406 (2011), arXiv:1103.3518 [astro-ph.SR]. [105] R. Durrer and A. Neronov, Astron. Astrophys. Rev. 21, 62 (2013), arXiv:1303.7121 [astro-ph.CO]. [106] A. Brandenburg and T. Kahniashvili, Phys. Rev. Lett. 118, 055102 (2017), arXiv:1607.01360 [physics.flu-dyn]. [107] A. Brandenburg, T. Kahniashvili, S. Mandal, A. Roper Pol, A. G. Tevzadze, and T. Vachas- pati, Phys. Rev. D 96, 123528 (2017), arXiv:1711."},{"citing_arxiv_id":"2605.20332","ref_index":117,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological History of Flavour Deconstruction Models: Constraints from Monopole Production","primary_cat":"hep-ph","submitted_at":"2026-05-19T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Flavour deconstruction models with semi-simple gauge groups generically produce light monopoles that require low-scale reheating after inflation to satisfy cosmological and astrophysical bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14044","ref_index":31,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Magnetic Origin of Primordial Black Holes: Ultralight PBHs and Secondary GWs","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T19:06:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Most studies of inflationary magnetogenesis have primarily focused on magnetic fields at large scales, where their amplitudes are strongly constrained by CMB B-mode polarization measurements [31-33, 38, 39] and recent blazar observations [40-42]. Combining these observations suggests that the present-day magnetic field strength on scales of∼1 Mpc lies within the range∼10 −9-10−19 Gauss [31, 32, 43]. In contrast, the evolution of magnetic fields at small scales is considerably more complicated, as nonlinear plasma effects become important and depend sensitively on the microscopic properties of the surrounding medium. Conse- quently, inflationary magnetic fields at small scales remain comparatively weakly constrained. While most previous"},{"citing_arxiv_id":"2605.13605","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DEFROST: Detecting Excess in Faraday Rotation thrOugh Sophisticated analysis Techniques","primary_cat":"astro-ph.IM","submitted_at":"2026-05-13T14:40:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DEFROST algorithm disentangles Galactic and extragalactic Faraday rotation in RM catalogs, recovering extragalactic parameters within 5 sigma for sources at absolute Galactic latitude above 45 degrees.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"However, from a theoretical point of view, we note that we can expect a non-zero mean as, for example, in case of primordial magnetic fields, generated during either phase transitions or inflation, see Durrer & Neronov (2013) for a review. In general, the extragalactic Faraday rotation variance in Eq. 9 can be expressed as a function of a vector of parameters Θ, ⟨ϕ2 eg,i⟩=σ 2 eg,i(Θ). (10) 2 We define the length scale as Λl0 := Z dl′ 0 ⟨B(l0)B(l′ 0)⟩ ⟨B(l0)2⟩ . Article number, page 3 of 14 A&A proofs:manuscript no. aa58520-25 Θis anN-dimensional vector, whereNis the number of param- eters used to represent the extragalactic Faraday depth variance and its elements are the parameters we wish to infer. Following Vacca et al. (2016), we assume that the extragalactic Faraday"},{"citing_arxiv_id":"2605.13016","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting constraints on primordial vector modes and implications for sourced magnetic fields and observed $EB$ power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T05:11:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Updated constraints on neutrino-sustained primordial vector modes imply magnetic fields too weak to seed observations and cannot reproduce the EB power spectrum while satisfying parity-even limits.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ditions and can leave characteristic imprints in cosmic microwave background (CMB) temperature and polar- ization anisotropies. They may be sourced, for example, by primordial magnetic fields through their anisotropic stress, or more generally in scenarios that involve addi- tional vector degrees of freedom and nontrivial gauge field dynamics in the early universe (see e.g., Ref. [1] for re- views). Perturbations in the neutrino sector can also play a crucial role. Once neutrinos begin to free-stream, their anisotropic stress permits regular primordial vector solu- tions that can survive and leave observable imprints [2, 3]. In this paper, we focus on those vector modes sourced by neutrino sector initial conditions, which are well moti-"},{"citing_arxiv_id":"2605.06795","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Plasma heating during the chiral plasma instability","primary_cat":"hep-ph","submitted_at":"2026-05-07T18:00:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"During chiral plasma instability, excess energy from chiral asymmetry heats the plasma with δT ~ μ5²/T instead of fully building the helical magnetic field.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Pedrini, New applications of the chiral anomaly,hep-th/0002195. - 32 - [19] S.A. Voloshin, Testing the Chiral Magnetic Effect with Central U+U collisions, Phys. Rev. Lett.105(2010) 172301 [1006.1020]. [20]CMScollaboration, Observation of charge-dependent azimuthal correlations in p-pb collisions and its implication for the search for the chiral magnetic effect, Phys. Rev. Lett.118(2017) 122301 [1610.00263]. [21]CMScollaboration, Constraints on the chiral magnetic effect using charge-dependent azimuthal correlations in pPb and pbpb collisions at the cern large hadron collider, Phys. Rev. C97(2018) 044912 [1708.01602]. [22]ALICEcollaboration, Constraining the magnitude of the chiral magnetic effect with event shape engineering in pb-pb collisions at √sNN = 2."},{"citing_arxiv_id":"2605.05323","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Primordial Magnetic Fields at Cosmic Dawn: 21-cm Forecasts with HERA and SKA","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T18:00:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Primordial magnetic fields enhance low-mass halo abundance at Cosmic Dawn, advancing Lyman-alpha coupling, X-ray heating and reionization and imprinting detectable signatures on global and fluctuating 21-cm signals observable by HERA and SKA.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"field power spectrum to the induced matter perturba- tions and their redshift evolution. Primordial magnetic fields (PMFs) can modify the growth of cosmic struc- ture by sourcing additional density fluctuations on small scales [35, 37, 39, 52]. We model a stochastic, homoge- neous, and isotropic PMF with comoving rms strength σB,0 (smoothed on 1 Mpc scales) and a power-law spec- tral indexn B [23, 24]. The indexn B sets the scale de- pendence of magnetic fluctuations, withn B → −3 corre- sponding to a scale-invariant spectrum on large scales. Although PMFs are statistically homogeneous and isotropic, their impact on structure formation is con- fined to a limited range of spatial scales. Prior to re- combination, magnetic fields are tightly coupled to the"},{"citing_arxiv_id":"2604.24835","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"JWST Constraints on Primordial Magnetic Fields","primary_cat":"astro-ph.CO","submitted_at":"2026-04-27T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"JWST UV luminosity function calibration of reionization history bounds primordial magnetic fields to √<B²> < 0.27 nG (n_B=-2) and < 0.18 nG (n_B=2) at 95% CL by ruling out double reionization at z≈24.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"law initial primordial magnetic field (PMF) spectrum, P lin B ∝k nB, and focus on the casesn B =−2 andn B = 2 for which there are templates fitted to magnetohydrody- namic (MHD) simulations. These choices correspond to representative red and blue spectra, capturing inflation- ary and causal (e.g. phase transition) magnetogenesis scenarios, respectively [54]. We parametrize the ampli- tude of the spectrum in terms of the smoothed magnetic field at 1 Mpc scale, B2 1 Mpc ≡ Z d3k (2π)3 P lin B (k)e −(k/Mpc−1)2 .(1) PMFs generate post-recombination density perturba- tions via the Lorentz force that acts on baryons. This adds an additional small-scale contribution to the mat- ter power spectrum beyond the standard adiabatic CDM"},{"citing_arxiv_id":"2604.21237","ref_index":33,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Bianchi-I Cosmology with Radiation in Asymptotically Safe Gravity","primary_cat":"gr-qc","submitted_at":"2026-04-23T03:13:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"In asymptotically safe gravity, radiation-filled Bianchi-I cosmologies show quantum corrections that soften anisotropy, while magnetic fields lead to persistent Kasner anisotropy without Lambda but isotropic de Sitter decay with nonzero Lambda.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the nonvanishing components of the Ricci tensor and the Ricci scalar are obtained as R00 = −3 ˙H − 3X i=1 H2 i , R ii = a2 i \u0010 ˙Hi + 3HH i \u0011 , R = 6 ˙H + 9H2 + 3X i=1 H2 i , (1.6) where Hi are the directional Hubble parameters, and H represents their mean value, defined as Hi = ˙ai ai , H = 1 3 3X i=1 Hi. (1.7) Classical studies, including the exact vacuum solution by Kasner [33] and the Heckmann-Sch¨ ucking solution for dust [34], along with its generalizations [35, 36], have been instrumental in understanding cosmological singularities [37, 38] and the isotropization of the BI universe in the presence of matter [39, 40]. A considerable body of work has explored BI cosmologies from various perspectives [30, 41-53]. These analyses have been further extended to other"},{"citing_arxiv_id":"2604.20768","ref_index":134,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Primordial Magnetogenesis and Gravitational Waves from ALP-assisted Phase Transition","primary_cat":"hep-ph","submitted_at":"2026-04-22T16:57:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ALP-assisted first-order phase transitions can explain observed intergalactic magnetic fields and produce detectable gravitational waves, linking cosmology with particle physics searches.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"difference between the false and true vacua as α= 1 ρrad ( 1−T∂ ∂T ) [ F(0,T)−F(σn,T) ]⏐⏐⏐⏐ Tn .(2.12) In the supercooled regime, where vacuum energy dominates, this simplifies to α≃V0 ρrad(Tn) = (Tinf Tn )4 ,(2.13) withT inf = (30V0/(g∗π2))1/4 denoting the temperature at which vacuum domination sets in1. The inverse duration of the PT is characterised by the parameterβ[134]: β H =−dlog Γ dlogT ⏐⏐⏐⏐ T=Tn ≃−4 +Td(S3/T) dT ⏐⏐⏐⏐ T=Tn =−4 + A3 log2(M/Tn),(2.14) 1Here, we assume thatg ∗ remains approximately constant betweenT inf andT n. - 6 - This expression highlights that, in the presence of strong supercooling,β/Hcan approach O(1), thereby enhancing the power spectrum of the GW signal. Once the transition completes, the Universe reheats to a temperature"},{"citing_arxiv_id":"2604.17230","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Suppressed Magnetogenesis from Ultralight Dark Matter due to Finite Conductivity","primary_cat":"astro-ph.CO","submitted_at":"2026-04-19T03:27:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Finite conductivity of the plasma suppresses parametric resonance amplification of electromagnetic fields from ultralight pseudoscalar dark matter, making it impossible to generate magnetic fields of sufficient strength in cosmic voids for observationally viable couplings.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"the vector potential in each half cycle of the oscillating φ field. As the amplification continues with time, in a few cycles, the EM field energy density will be comparable to the φ field energy density, and the gauge field backre- action on the evolution of φ will be important. However studying the backreaction is not the aim of this letter (please see Ref. [14] for the backreaction effects). We choose our parameters similar to the parameters of Fig.2 of Ref. [14]. On comparing our results shown in figure 1 with Fig. 2 of [14], we can say that there is a good match between the two results. In the second case, we include the plasma conductiv- ity in the evolution of the EM field. The corresponding results are shown in figure 2, where the panel layout and"},{"citing_arxiv_id":"2604.01277","ref_index":115,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Lights, Camera, Axion: Tracing Axions from Supernovae in the Diffuse $\\gamma$-ray Sky","primary_cat":"hep-ph","submitted_at":"2026-04-01T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Axions produced in supernovae generate a diffuse gamma-ray signal through conversion in magnetic fields, yielding competitive constraints on the axion-photon coupling from COMPTEL, EGRET, and Fermi-LAT data plus forecasts for future MeV telescopes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"range of magnetic field configurations considered for host galaxies. C. Intergalactic magnetic field The magnetic fields in the large-scale structure, i.e., the intergalactic medium (IGM), are poorly constrained, as direct measurements are scarce and the allowed param- eter space remains wide. An overview of IGM magnetic field generation mechanisms and observational bounds are provided in Refs. [115, 116]. Following the commonly adopted benchmark [110, 117-123], we assume an opti- mistic configuration with a field strength of 1 nG and a coherence length of 1 Mpc, which represents the maxi- mal conversion probability in the IGM. To encompass the uncertainty, we also consider a conservative scenario with the same coherence length but a smaller magnetic"},{"citing_arxiv_id":"2602.16575","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Chiral gravitational waves from multi-phase magnetogenesis","primary_cat":"astro-ph.CO","submitted_at":"2026-02-18T16:20:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-phase inflation with chiral vector interactions generates amplified primordial magnetic fields that induce a detectable circularly polarized gravitational-wave background.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.22592","ref_index":74,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Axion-Photon conversion via circular polarization imprints in the CMB $V$-mode observations","primary_cat":"astro-ph.CO","submitted_at":"2025-10-26T09:20:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Proposes that axion-photon conversion in pre-CMB helical magnetic fields imprints detectable V-mode polarization in the CMB, allowing CLASS 40 GHz observations to constrain ALP masses 10^{-10} to 10^{-8} eV and their photon coupling under optimistic nG field assumptions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.13752","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effects of primordial magnetic fields on 21 cm multifrequency angular power spectra","primary_cat":"astro-ph.CO","submitted_at":"2025-10-15T16:59:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The paper calculates multifrequency angular power spectra of the 21 cm line for models with primordial magnetic fields of strength 4 nG and spectral indices -2.9 and -2.5, then estimates signal-to-noise ratios for uGMRT, MeerKAT and SKA1-MID.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.08025","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the contribution of galaxies to the magnetic field in cosmic voids","primary_cat":"astro-ph.CO","submitted_at":"2025-10-09T10:02:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Superposition of static galactic magnetic dipoles is screened by intergalactic plasma and cannot account for lower bounds on magnetic fields in cosmic voids from blazar gamma-ray data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.23858","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting constraints on magnetogenesis from baryon asymmetry","primary_cat":"hep-ph","submitted_at":"2025-09-28T12:53:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Maximally helical primordial U(1)_Y magnetic fields can generate both intergalactic magnetic fields and baryon asymmetry; non-helical fields may work if Higgs dynamics compensate helicity loss to ≲10^{-9-10} precision during electroweak crossover.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.08011","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial black holes and magnetic fields in conformal neutrino mass models","primary_cat":"hep-ph","submitted_at":"2025-05-12T19:24:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Conformal U(1)' seesaw models produce PBHs contributing to dark matter and helical magnetic fields at seesaw scales of 10^4-10^11 GeV, with observable GW, microlensing, and Hawking signals at LISA, Roman, and future gamma-ray telescopes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.08141","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Testing cosmology and fundamental physics with the Cherenkov Telescope Array","primary_cat":"astro-ph.HE","submitted_at":"2019-07-18T16:23:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Sensitivity study forecasts that CTA can measure EBL absorption with high precision, detect IGMF signatures, and explore new parameter space for ALPs and LIV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.07392","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Introduction to multi-messenger astronomy","primary_cat":"astro-ph.HE","submitted_at":"2019-07-17T08:45:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"The paper supplies an introductory lecture-style summary of observational techniques, astronomical sources, and physical processes across the four main messengers in multi-messenger astronomy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04402","ref_index":114,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lectures on Reheating after Inflation","primary_cat":"astro-ph.CO","submitted_at":"2019-07-09T20:36:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture notes providing a generic introduction to reheating after inflation, covering its theoretical, phenomenological, and observational aspects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}