Current date: 2026-10-23
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Datestamp limit: 2026-10-23 (0 days ago)
Created/updated limit: 2026-10-16 (7 days ago)
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Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
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Scoring abstracts
Number of records retrieved: 771
Keyword score statistics
score 8 -- 1 abstracts
score 6 -- 3 abstracts
score 5 -- 3 abstracts
score 4 -- 10 abstracts
score 3 -- 6 abstracts
score 2 -- 22 abstracts
in total -- 45 abstracts
Articles that appeared on 2026-10-23
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[abstract 1 / 45] Wow! (score: 8)
- Title: Prompt Jet Launching and Delayed Thermal Disk in Tidal Disruption Event for Prolonged Activity GRB 220706AAuthors: Yuri Sato, Rin Oikawa,Comments: 9 pages, 1 figureSubjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
GRB 220706A exhibits X-ray flaring activity extending to ~51 days after the trigger, along with a luminous optical thermal component emerging on a timescale of ~10^6 s. Such prolonged central-engine activity could be powered by a collapsar fed by an extended stellar envelope. However, a RELATIVISTIC JET may struggle to break out of the extended envelope. These challenges motivate a tidal disruption event (TDE), although explaining both the early RELATIVISTIC JET and the luminous late optical thermal emission within one TDE framework remains difficult. We investigate a TDE scenario in which shocks between stellar debris streams drive the early inflow of some debris, potentially carrying preexisting fossil MAGNETic flux toward the BLACK HOLE (BH) and powering an initial RELATIVISTIC JET via the Blandford-Znajek mechanism. The remaining debris circularizes into an accretion disk, whose thermal emission accounts for the late optical thermal component. For GRB 220706A, the optical timescale, luminosity, and color temperature are consistent with disruption of a blue supergiant (M_*~50M_{sun}, R_*~20~R_{sun}) by a BH of mass M_{BH}~10^5 M_{sun}, assuming that the accretion disk forms on a timescale comparable to the orbital period of the most tightly bound stellar debris. A MAGNETic field strength of ~10^5 G is required near the BH before disruption to power a JET capable of producing the inferred gamma-ray luminosity. Continued fallback may sustain central-engine activity beyond the observed X-ray flaring episode, making future X-ray monitoring a test of this scenario.
[abstract 2 / 45] Yes (score: 6) - Title: The BLACK HOLE-galaxy correlations of the 12 micron local AGN sample: a NUSTAR perspectiveAuthors: M. Gliozzi, L. Spinoglio, J. A. Fernandez-Ontiveros, M. A. Malkan, J. K. Williams, M. Young. A. D. Oxley, S. Satyapal,Comments: 12 pages, 9 figures (+ Appendix), accepted for publication in Astronomy and AstrophysicsSubjects: astro-ph.GA astro-ph.CO astro-ph.HECreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
The M-sigma correlation of inactive galaxies plays a crucial role in estimating the BLACK HOLE mass (MBH) in ACTIVE GALACTIC NUCLEi (AGN): 1) it is used to calibrate the reverberation mapping (RM) method; 2) the RM is the basis of the single epoch method, the most-used technique to determine MBH of broad-line AGN; and 3) in narrow-line AGN, MBH is often directly inferred from the M-sigma correlation. The main goal of this work is to test whether the M-sigma relation calibrated from inactive galaxies can be reliably applied to a local AGN population spanning Seyfert 1, Seyfert 2, and hidden broad-line region galaxies (HBLRs), and whether the resulting AGN relation has sufficient predictive power to be used as an indirect MBH estimator. To investigate this hypothesis, we used the 12 micron AGN sample, a local representative and largely unbiased sample. Since a substantial fraction of this sample has good-quality NUSTAR data, we estimated their MBH with the X-ray scaling method, which works for any AGN accreting at moderate or high level. We find that the M-sigma correlation of the 12 micron AGN sample is different from the one obtained with inactive galaxies and has a substantial scatter. Therefore, its predictive power for MBH estimates is fairly limited. We also find that the MBH-Mgal correlation based on the 12 micron AGN sample is consistent with the analogous correlation obtained from a large sample of nearby type 1 AGN and inconsistent with that of inactive galaxies. Finally, we find suggestive evidence that Seyfert 1 and HBLRs have similar and systematically higher Eddington ratios than Seyfert 2 galaxies.
[abstract 3 / 45] Yes (score: 6) - Title: Chandra and Multiwavelength Study of Pevatron Candiate HESS J1702-420AAuthors: Hui Yang, Yichao Lin, Jeremy Hare, Seth Gagnon, Oleg Kargaltsev,Comments: 13 pages, 6 figures; submitted to A&A; Comments welcomeSubjects: astro-ph.HECreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
Aims: HESS J1702-420A is a promising Galactic PeVatron candidate whose physical nature remains unknown. Previous XMM-Newton observations revealed hard, apparently extended X-ray emission from XMMU J170147.3-421407, offset from the center of the TeV source, suggesting a possible pulsar wind nebula (PWN) association. We aim to resolve its X-ray morphology, investigate compact-object candidates in the field, and assess their possible association with HESS J1702-420A. Methods: We obtained three new ACIS-I observations from the Chandra X-ray observatory (CXO) with a total exposure of 50.4 ks. We performed imaging, source detection, spectral and variability analyses, and multiwavelength (MW) machine-learning (ML) source classification. Neutron star (NS) candidates were further investigated using deep near-infrared and radio imaging. Results: The Chandra observations resolve XMMU J170147.3-421407 into a faint point-like source, Src11 (CXO J170144.5-421415), and asymmetric diffuse emission comprising eastern and western lobes. The X-ray spectral, variability, and MW properties of Src11 and the diffuse emission are consistent with those commonly observed in pulsar/PWN systems, further supported by the ML classifications. However, the asymmetric diffuse morphology is unlike a typical bow-shock/tail or JET/torus PWN, and the $\sim7'$ offset from HESS J1702-420A makes a firm physical association difficult to establish. A possible shell-like radio structure north-west of Src11 may indicate a more complex PWN/SNR environment. Other NS candidates are less consistent with a pulsar/PWN interpretation, making Src11 the most compelling candidate in the field.
[abstract 4 / 45] Yes (score: 6) - Title: Analysis of a coronal hole JET in the chromosphere and the transition region with IRIS data and SDO observationsAuthors: M. Koletti, C. Gontikakis, S. Patsourakos, K. Tsinganos,Comments: accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.SRCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Coronal JETs are transient phenomena that occur throughout the solar atmosphere, often triggered by the activation of mini-filaments. Jets are an important field of study, as they are believed to contribute to the mass supply of the solar wind. We study a small-scale solar JET occurring in a low-latitude coronal hole, focusing on traces of the JET eruption to the lower atmosphere, utilizing chromospheric and transition region diagnostics. We also investigate the possible mechanisms and dynamic conditions leading to its onset. We analyze ultraviolet spectra from the Interface Region Imaging Spectrograph to investigate chromospheric dynamics and their connection to the transition region, using diagnostics of the Mg II k 2796.35 Å and Si IV 1393.75 Å lines, together with non-LTE inversions. We complement this analysis with multiwavelength imaging and MAGNETograms from the Solar Dynamics Observatory, as well as MAGNETic field modeling. The analysis of Mg II k and Si IV parameters reveals a coupling between chromospheric and transition region plasma dynamics. Profiles on the JET spire present deeper central reversals, larger peak separations and higher transition region Doppler velocities. The JET initiation is associated with a mini-filament-like structure, preceded by dynamic variations in the photospheric MAGNETic field. We find single-peaked Mg II k profiles at one of its footpoints, possibly indicating plasma drainage. The presence of a null point and a quasi-separatrix layer suggests that RECONNECTion can play a role in the mini-filament-like structure destabilization and JET eruption. This study suggests that the signature and possibly the origin of coronal JETs can be traced down to the chromosphere. The detailed analysis of the Mg II k profiles at the JET spire and the mini-filament-like structure may provide valuable observational constraints for future MHD simulations.
[abstract 5 / 45] Yes (score: 5) - Title: Investigating the Gamma-Ray Emission from Explosive Dispersal Outflows with FERMI-LATAuthors: Paarmita Pandey, Stephen C. Lenker, Laura A. Lopez, Anna L. Rosen, Tim Linden, Todd A. Thompson, Stella S. R. Offner, Katie Auchettl, Christopher M. Hirata,Comments: Accepted for publication in ApJ, 14 pages, 7 figuresSubjects: astro-ph.HECreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
We present the first systematic study of explosive dispersal outflows (EDOs) as potential sources of high-energy emission in the Milky Way. EDOs are energetic outflows produced during dynamical interactions in young, massive star-forming regions, and their physical conditions make them promising environments for cosmic-ray acceleration. Using 16 years of $0.2$--$500$ GeV FERMI-LAT observations, we study the gamma-ray properties of seven EDOs. Three EDOs, DR21, G34.26$+$0.15, and G5.89$-$0.39 show spatially coincident GeV emission, while the remaining systems yield non-detections. Among the sample, DR21 stands out as the brightest candidate, with a detection significance $\geq 40σ$. Its spectrum is well described by a power law with an exponential cutoff, and the integrated luminosity in the $0.1$--$500$ GeV band is $L_γ\simeq 2\times10^{35}\ \mathrm{erg\ s^{-1}}$. When compared with the outflow's estimated kinetic energy, the inferred cosmic-ray acceleration efficiency is $\leq 15\%$, consistent with values for shocks in dense molecular environments. The energetics and morphology support an association between the DR21 molecular outflow and the observed gamma rays. Our results demonstrate that EDOs span a wide range of gamma-ray luminosities and efficiencies, suggesting they may contribute to the Galactic COSMIC RAY budget. This motivates searches for additional EDOs and improved multiwavelength characterization of their environments.
[abstract 6 / 45] Yes (score: 5) - Title: The deepest X-ray view of a kiloparsec scale JET at z=6.1Authors: Fabio A. Meanti, Luca Ighina, Alberto Moretti, Kyra Bettwy, Alessandro Caccianiga, Thomas Connor, Fabrizio Tavecchio, Silvia Belladitta, Emmanuel K. Bempong-Manful, Cristiana Spingola,Comments: Accepted for publication in Astronomy & Astrophysics (A&A) on 13 October 2026Subjects: astro-ph.HE astro-ph.GA hep-thCreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
The mechanism responsible for the high-energy emission observed in kiloparsec-scale JETs across cosmic time remains poorly understood. The RELATIVISTIC JET associated with the z=6.1 AGN PSO J030947.49+271757.31 is the highest-redshift large-scale JET currently resolved in X-rays, providing a unique opportunity to study these structures. We present new Chandra observations, combined with archival data, for a total exposure of 360 ks. The increased exposure allowed us to resolve the extended X-ray emission into two distinct, slightly resolved components and perform spatially resolved spectral analyses. The extended emission has a photon index of Gamma = 2.25 (+0.45, -0.44), steeper than that of the core (Gamma = 1.86 +/- 0.09), and an extended-to-core luminosity ratio of 18%. Simulations using the Chandra image as input show that an AXIS-like mission could increase the detected photon statistics by a factor of approximately 17. We resolve the kiloparsec-scale JET into two main components and constrain its spectral properties. This is the most distant and one of the most X-ray-luminous large-scale JETs currently known. Future X-ray missions with arcsecond-scale angular resolution could enable more detailed studies of such systems and reveal a population of fainter high-redshift JETs beyond Chandra's reach.
[abstract 7 / 45] Yes (score: 5) - Title: Nuclear Millimeter Continuum Emission in Radio-Quiet Active Galactic Nuclei: an ALMA Spectral and Variability StudyAuthors: Sophie M. Venselaar, Claudio Ricci, Yoshiyuki Inoue, Chin-Shin Chang, Akihiro Doi, Noemi Barnier, Taiki Kawamuro, Susanne Aalto, Momoka Hamamoto, Elena Shablovinskaya, Ezequiel Treister,Comments: Accepted for publication in The Astrophysical Journal (ApJ)Subjects: astro-ph.HE astro-ph.GACreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
Unresolved millimeter (mm) emission is observed in radio-quiet (RQ) Active Galactic Nuclei (AGN), but its physical origin remains debated. Self-absorbed SYNCHROTRON emission from the compact X-ray corona is one of the leading candidates. Previous support for this coronal SYNCHROTRON origin has mainly been based on variability and spectral indices in a few RQ AGN, with a lack of (quasi-)simultaneous broadband data for larger samples. We present Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of nine nearby ($z \sim 0.008-0.064$) RQ AGN, obtained quasi-simultaneously at 100, 145, and 233 GHz. Based on power-law fits to the spectral energy distributions, we measure millimeter spectral indices ranging from $-0.05^{+0.09}_{-0.09}$ to $0.88^{+0.12}_{-0.11}$. Furthermore, across two 100 GHz observing epochs per source, separated by $4-11$ days, we detect flux density variability of $30-56$% (>$3σ$ significance level) in three out of nine sources. Spectral slopes alone are insufficient to constrain the origin of the millimeter emission; however, the observed short-timescale variability and inferred brightness temperature values are consistent with a non-thermal emission mechanism arising from a compact emitting region with a size of $R_{\rm mm}< 10^3 - 10^4 R_{\rm g}$, such as the corona or a compact JET. Furthermore, we find a clear correlation between the 100/233 GHz and X-ray flux in our sample, and establish a new linear correlation between 145 GHz and X-ray emission.
[abstract 8 / 45] Yes (score: 4) - Title: Exploring the connection between Fast Radio Bursts and binary neutron star mergersAuthors: Barbara Patricelli, Maria Grazia Bernardini, Cecilia Sgalletta, Michela Mapelli,Comments: 5 pages. Published in A&A (2026), Volume number 714, Article Number A254Subjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Fast Radio Bursts (FRBs) are highly energetic radio sources whose duration is of the order of milliseconds. The physical origin of these sources is still unknown. Many models suggest MAGNETars as possible progenitors of FRBs, and this is supported by the association between FRBs and the Galactic MAGNETar SGR 1935+2154; other proposed progenitors include binary neutron star (BNS) mergers, that are themselves linked to MAGNETar formation. In this work we investigate the possible connection between FRBs and BNS mergers, including MAGNETars that might be produced in such events, by comparing the detection rates inferred from synthetic BNS and associated FRB populations with the rates observed by CHIME. We produce a synthetic catalog of BNS mergers by combining recent theoretically predicted BNS merger rate as a function of redshift and the neutron star mass distribution inferred from measurements of Galactic BNSs. Using this catalog we predict the number of BNS systems ending as MAGNETars (stable or supramassive neutron star) or BLACK HOLEs (formed promptly or after the collapse of a hypermassive neutron star) for different equations of state. We then simulate for each BNS (and therefore for each MAGNETar remnant) an associated FRB and estimate how many of them can be potentially detected by CHIME. We find that the rate of BNS mergers and the rate of MAGNETars produced after BNS represents a non-negligible fraction of the FRBs detected by CHIME, both repeating and non-repeating. Although additional formation channels need to be considered to account for the entire population of FRBs, the existence of a fraction of FRBs that might genuinely be associated to BNS mergers has profound implications in the context of multi- messenger astronomy, supporting the systematic searches of coincident detections of FRBs and GWs from a BNS merger with current and future facilities.
[abstract 9 / 45] Yes (score: 4) - Title: First Results of Calculation of the Dayside Magnetopause Reconnection Rate with TRACERSAuthors: D. E. da Silva, L. J. Chen, B. Burkholder, C. J. Martin, B. Michotte de Welle, I. DesJardin, S. A. Fuselier, K. J. Trattner, S. M. Petrinec, G. Cucho-Padin, D. Sur, N. Y. Buzulukova, J. Bonnell, J. S. Halekas, D. Miles, S. Henderson, J. Dorelli,Comments: Under revision for Journal of Geophysical Research: Space PhysicsSubjects: physics.space-ph physics.geo-ph physics.plasm-phCreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
Quantifying the rate of RECONNECTion remains a key challenge in the study of geoMAGNETic storms. In this study, we present the first results from the new Tandem Reconnection and Cusp Electrodynamics Reconnaissance Satellites (TRACERS) mission to calculate the RECONNECTion rate from dispersed ion populations measured in the cusp, using previously developed methodology. We study ion dispersion events in two storms. During the first storm, which occurred on September 30, 2025, 21 dispersion events were identified in TRACERS 2 ion data as a combined result of geospace dynamics and the spacecraft cusp encounters. Throughout this time when ion dispersion was detected by TRACERS , the RECONNECTion rate is calculated and is shown to track reasonably well with another measure of geoMAGNETic activity, the Cross Polar Cap Potential (CPCP) as obtained by the Super Dual Auroral Radar Network (SuperDARN). The dispersions are correlated with the smoothed CPCP, and a correlation of $r^2=0.62$ was found using the dispersions from the onset and main phase of the storm. The correlation disappears when including dispersions from the recovery period. The distribution of RECONNECTion rates throughout this storm lies generally between 0.1 - 1.5 mV/m, slightly lower than previous RECONNECTion rates calculated with DMSP, but consistent with in-situ observations made with Polar. In this work, we also apply a previously developed automatic identification algorithm for ion-energy cusp dispersion to TRACERS, with the intent that it may serve as a tool for future statistical analysis as the data volume becomes too large to manually review.
[abstract 10 / 45] Yes (score: 4) - Title: Rest-frame Ultraviolet Variability of Quasars in the Cosmic Himalayas OverdensityAuthors: Jiaqi Lin, Zhenya Zheng, Bin Ma, Yongming Liang, Lin Long,Comments:Subjects: astro-ph.GACreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Some high-redshift overdensities show an enhanced incidence of AGNs, suggesting that large-scale environment may influence supermassive BLACK HOLE fuelling and triggering. Whether environment also affects AGN variability remains unclear.Using the Cosmic Himalayas (CH), an extreme concentration of 11 type 1 QUASARs at z=2.16-2.20, we investigate possible offsets in rest-frame ultraviolet variability relative to QUASARs with comparable redshifts, BLACK HOLE masses, and Eddington ratios.We construct a parent sample of 1,138 Stripe 82 QUASARs at 2.11<=z<=2.25 and combine photometry from the SDSS, the PS1, and the ZTF to build observer-frame g- and r-band light curves spanning up to 27~yr. We compare DRW parameters and ensemble structure functions (SFs) with control pseudo-samples matched in BLACK HOLE mass and Eddington ratio, and use injection--recovery simulations to forecast the detectability of a CH-like offset.The CH QUASARs show a tendency toward shorter DRW damping timescales (median offsets of -0.32 and -0.13 dex in g and r) and slightly higher asymptotic amplitudes. None of the four DRW comparisons is statistically significant, including the largest offset in the g-band damping timescale (p=0.16). Ensemble SFs generally exceed matched-control medians, although 18 of 19 lag bins per band remain within the 95% pointwise envelopes. Assuming a true uniform -0.32 dex g-band timescale offset, injection--recovery simulations predict an 80% probability of nominal 3sigma detection with approximately 60 QUASARs of comparable variability scatter and data quality.If confirmed, the tentative variability offsets may suggest that large-scale environment influences accretion-flow variability beyond its potential role in QUASAR triggering. Larger samples with higher-precision light curves, such as those expected from the LSST, are required to test this possibility.
[abstract 11 / 45] Yes (score: 4) - Title: EP J062132.0+623837: A Multi-wavelength Study of a Changing-look Active Galactic Nucleus Discovered by Einstein ProbeAuthors: Lin-Na Xu, Ning Jiang, Tinggui Wang, Shifeng Huang, Yibo Wang, Zhenfeng Sheng, Mingxin Wu, Jiazheng Zhu, Huaqing Cheng, Chichuan Jin, Jun-Jie Jin, Dongyue Li, Yuan Liu, Jianwei Lyu, Jian-Guo Wang, Yun-Fei Xu, Yongquan Xue, Zhen Zhang,Comments: 16 pages, 9 figures, 2 tables. Accepted for publication in ApJSubjects: astro-ph.GA astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
EP J062132.0+623837 is a new X-ray source identified in 14-day binned survey data from the Wide-field X-ray Telescope aboard the Einstein Probe (EP). Subsequent X-ray observations with the Follow-up X-ray Telescope (FXT) on board EP localized the source to the central region of the galaxy 2MASX J06213207+6238390 at $z=0.084$. Here, we present a comprehensive analysis of the multi-wavelength data for this object. During the FXT and SWIFT/XRT follow-up, the source remained X-ray active, with observed luminosities of $(3-9)\times10^{43}$ erg s$^{-1}$, and its X-ray spectra were well described by power-law models with photon indices of $Γ\sim1.5$. The optical spectrum of the host galaxy clearly reveals a broad-line ACTIVE GALACTIC NUCLEus (AGN) exhibiting significantly enhanced broad Balmer emission lines compared to an archival spectrum obtained four years earlier, thereby marking a changing-look transition from Type 1.8 to Type 1.5. Furthermore, long-term optical and mid-infrared light curves indicate that the nucleus underwent dramatic brightening around 2010 and has since shown substantial variability. Given the spatial coincidence and multi-wavelength behavior, we identify EP J062132.0+623837 as a changing-look AGN, initially detected by EP and subsequently confirmed to exhibit large-amplitude variability across multiple bands. This case study demonstrates the great potential of wide-field time-domain X-ray surveys for discovering changing-look AGNs, paving a new avenue for their systematic identification as a powerful complement to ongoing optical surveys.
[abstract 12 / 45] Yes (score: 4) - Title: Search for Ultra-Relativistic Magnetic Monopoles with LHAASO-KM2AAuthors: Zhen Cao, F. Aharonian, Y. X. Bai, Y. W. Bao, D. Bastieri, X. J. Bi, Y. J. Bi, W. Bian, J. Blunier, A. V. Butkevich, C. M. Cai, W. Y. Cao, Zhe Cao, J. Chang, J. F. Chang, E. S. Chen, G. H. Chen, H. K. Chen, L. F. Chen, Liang Chen, Long Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, X. B. Chen, X. J. Chen, X. P. Chen, Y. Chen, N. Cheng, Q. Y. Cheng, Y. D. Cheng, M. Y. Cui, S. W. Cui, X. H. Cui, Y. D. Cui, B. Z. Dai, H. L. Dai, L. X. Dai, Z. G. Dai, Danzengluobu, Y. X. Diao, A. J. Dong, K. K. Duan, X. D. Duan, J. H. Fan, Y. Z. Fan, J. Fang, J. H. Fang, K. Fang, C. F. Feng, H. Feng, L. Feng, S. H. Feng, X. T. Feng, Y. Feng, Y. L. Feng, S. Gabici, B. Gao, Q. Gao, W. Gao, C. Ge, M. M. Ge, T. T. Ge, L. S. Geng, G. Giacinti, G. H. Gong, Q. B. Gou, M. H. Gu, W. M. Gu, F. L. Guo, J. Guo, K. J. Guo, X. L. Guo, Y. Q. Guo, Y. Y. Guo, R. P. Han, O. A. Hannuksela, M. Hasan, H. H. He, H. N. He, J. Y. He, X. Y. He, Y. He, S. Hernández-Cadena, C. Hou, X. Hou, H. B. Hu, S. C. Hu, C. Huang, D. H. Huang, F. Huang, J. J. Huang, X. L. Huang, X. T. Huang, X. Y. Huang, Y. Huang, Z. J. Huang, Z. Q. Huang, A. Inventar, X. L. Ji, H. Y. Jia, K. Jia, H. B. Jiang, K. Jiang, X. W. Jiang, Z. J. Jiang, M. Jin, S. Kaci, M. M. Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, W. H. Lei, Cheng Li, Cong Li, D. Li, F. Li, H. B. Li, H. C. Li, Jian Li, Jie Li, K. Li, L. Li, R. L. Li, T. Y. Li, W. L. Li, X. R. Li, X. Y. Li, Y. Li, Zhe Li, Zhuo Li, E. W. Liang, Y. F. Liang, S. J. Lin, B. Liu, C. Liu, D. Liu, D. B. Liu, H. Liu, J. Liu, J. F. Liu, J. L. Liu, J. R. Liu, M. Y. Liu, Q. Liu, R. Y. Liu, S. M. Liu, T. Liu, W. Liu, Y. Liu, Y. Liu, Y. N. Liu, Y. Q. Lou, Q. Luo, Y. Luo, H. K. Lv, B. Q. Ma, L. L. Ma, X. H. Ma, I. O. Maliy, J. R. Mao, Z. Min, W. Mitthumsiri, Y. Mizuno, G. B. Mou, A. Neronov, C. -Y. Ng, K. C. Y. Ng, M. Y. Ni, L. Nie, L. J. Ou, Z. W. Ou, P. Pattarakijwanich, Z. Y. Pei, D. Y. Peng, J. C. Qi, M. Y. Qi, J. J. Qin, H. Qu, A. Raza, C. Y. Ren, M. Q. Ruan, D. Ruffolo, A. Sáiz, D. Savchenko, D. Semikoz, L. Shao, O. Shchegolev, Y. Z. Shen, X. D. Sheng, F. W. Shu, H. C. Song, Yu. V. Stenkin, Y. Su, C. Y. Sun, D. X. Sun, H. Sun, J. X. Sun, M. Sun, Q. N. Sun, X. N. Sun, Z. B. Sun, N. H. Tabasam, J. Takata, P. H. T. Tam, H. B. Tan, Q. W. Tang, R. Tang, Z. B. Tang, W. W. Tian, C. N. Tong, L. H. Wan, C. Wang, D. H. Wang, G. W. Wang, H. G. Wang, J. C. Wang, J. F. Wang, J. S. Wang, K. Wang, Kai Wang, Kai Wang, L. P. Wang, L. Y. Wang, W. Wang, X. G. Wang, X. J. Wang, X. Y. Wang, Y. Wang, Y. D. Wang, Z. H. Wang, Z. X. Wang, Zheng Wang, D. M. Wei, J. J. Wei, Y. J. Wei, T. Wen, S. S. Weng, C. Y. Wu, H. R. Wu, Q. W. Wu, S. Wu, X. F. Wu, Y. S. Wu, S. Q. Xi, J. Xia, G. M. Xiang, D. X. Xiao, G. Xiao, Y. F. Xiao, B. H. Xie, F. Xie, Y. L. Xin, H. D. Xing, Y. Xing, D. R. Xiong, B. N. Xu, C. Y. Xu, D. L. Xu, R. X. Xu, S. S. Xu, L. Xue, D. H. Yan, T. Yan, C. Yang, C. Y. Yang, F. F. Yang, L. L. Yang, M. J. Yang, R. Z. Yang, W. X. Yang, Z. H. Yang, Z. G. Yao, X. A. Ye, L. Q. Yin, N. Yin, X. H. You, Z. Y. You, Y. H. Yu, Q. Yuan, H. Yue, H. D. Zeng, T. X. Zeng, W. Zeng, X. T. Zeng, M. Zha, B. Zhang, B. B. Zhang, B. T. Zhang, C. Zhang, H. Zhang, H. M. Zhang, H. Y. Zhang, J. L. Zhang, J. Y. Zhang, L. Y. Zhang, Li Zhang, P. F. Zhang, R. Zhang, R. Y. Zhang, S. R. Zhang, S. S. Zhang, S. Y. Zhang, W. Zhang, X. Zhang, X. L. Zhang, X. P. Zhang, Yi Zhang, Yong Zhang, Z. P. Zhang, Z. H. Zhang, J. Zhao, L. Zhao, L. Z. Zhao, S. P. Zhao, X. H. Zhao, F. Zheng, T. C. Zheng, B. Zhou, H. Zhou, J. N. Zhou, L. Zhou, M. Zhou, P. Zhou, R. Zhou, X. X. Zhou, X. X. Zhou, B. Y. Zhu, C. G. Zhu, F. R. Zhu, H. Zhu, K. J. Zhu, Y. F. Zhu, Z. F. Zhu, Y. C. Zou, X. Zuo,Comments: 10 pages, 5 figures, plus Supplemental Material (1 page, 2 figures)Subjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Ultra-RELATIVISTIC MAGNETic monopoles traversing the atmosphere are expected to initiate extensive air showers characterized by a muon deficit and a compact lateral profile. Using 1438.81 live days of data from the LHAASO-KM2A array, we present a search for these cosmic particles within the Lorentz factor range of $10^5$ to $10^7$. A machine-learning classifier utilizing lateral shower shape observables from the electroMAGNETic detectors is deployed to separate the signal from the hadronic background. No statistical excess above the background expectation is observed, and upper limits at the 90\% confidence level are established on the isotropic monopole flux. The resulting upper limit is $2.6 \times 10^{-16}\,\mathrm{cm}^{-2}\,\mathrm{s}^{-1}\,\mathrm{sr}^{-1}$ at $γ= 10^5$ and reaches $8.8 \times 10^{-19}\,\mathrm{cm}^{-2}\,\mathrm{s}^{-1}\,\mathrm{sr}^{-1}$ at $γ= 10^7$, which improves upon the astrophysical Parker bound by over three orders of magnitude. This work establishes constraints on the monopole flux within a previously unconstrained velocity window.
[abstract 13 / 45] Yes (score: 4) - Title: Breaking the symmetry: X-ray POLARIZATION from a spreading layer on a tilted weakly MAGNETized neutron starAuthors: Anna Bobrikova, Alexandra Veledina, Juri Poutanen, Vladislav Loktev,Comments: 11 pages, 6 figs, submitted to A&ASubjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
When modeling the emission from an X-ray binary system, we often assume that the rotational axis of the compact object is aligned with that of the binary system. While often considered irrelevant for spectroscopic observations, the orientation of the binary system is crucial for polarimetric properties. With the recent advent of X-ray polarimetric observations enabled by the Imaging X-ray Polarimetry Explorer (IXPE), indications of a possible misalignment of the neutron star rotational axis with respect to the binary axis have been reported. Following these indications, we present an analytical model for the polarimetric properties of emission arising from a spreading layer on an inclined weakly MAGNETized neutron star (WMNS). We discuss the expected polarimetric properties and study the impact of geometrical parameters of the system on the POLARIZATION of WMNS emission. We compare our results with those for aligned systems. Finally, we discuss applications of the model to recent and upcoming X-ray polarimetric observations with IXPE and mention the suggestions for further development of the model.
[abstract 14 / 45] Yes (score: 4) - Title: Charmed baryon-to-meson ratios inside JETs as a discriminator of hadronization mechanisms: from color RECONNECTion in p+p to coalescence in Pb+PbAuthors: Zi-Xuan Xu, Wei Dai, Ben-Wei Zhang, Enke Wang,Comments: 14 pages, 12 figuresSubjects: hep-ph hep-thCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Jets separate the products of hard scatterings from the underlying event and thus help to clarify the origin of the enhanced baryon-to-meson ratios observed from small to large collision systems. We investigate the charmed baryon-to-meson ratio $Λ_c^+/D^0$ within JETs in p+p and Pb+Pb collisions at $\sqrt{s_{NN}}=5.02$~TeV to discriminate between candidate hadronization mechanisms. In p+p collisions, simulated with PYTHIA8 using color RECONNECTion (CR-BLC Mode 2) as a representative beyond-leading-color scenario, the in-JET ratio is enhanced at low-to-intermediate $p_T$ relative to the inclusive one---opposite to the light-flavor $Λ/K^0_S$ case---because the color-RECONNECTion-induced excess of the ratio remains correlated with the JET and survives the JET requirement, while the fragmentation baseline shows no such enhancement. In Pb+Pb collisions, described by the SHELL model with a coalescence plus fragmentation hybrid hadronization, the in-JET ratio is instead suppressed moderately at intermediate $p_T$, because coalescence hadrons assembled from soft thermal partons carry no correlation with the JET direction and are preferentially discarded by the JET selection. The sign of the in-JET modification thus discriminates between the two mechanisms. Both mechanisms shift charmed hadrons toward small values of the parallel JET momentum fraction $z^{ch}_{||}$, with a stronger effect on $Λ_c^+$, so that the $z^{ch}_{||}$ spectrum probes non-fragmentation hadronization independently of parton energy loss. The radial profile of the in-JET ratio rises with the distance from the JET axis in both systems, with the lowest-$p_T$ interval displaced farthest for color RECONNECTion and the intermediate-$p_T$ interval for coalescence. These results provide the baseline and predictions needed for future JET-tagged charmed-hadron measurements in both collision systems.
[abstract 15 / 45] Yes (score: 4) - Title: Spectral Properties of X-Ray Flares in Gamma-Ray BurstsAuthors: Xiongwei Bi, Zejun Jiang, Jirong Mao,Comments: Accepted for publication in The Astrophysical Journal (ApJ)Subjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
We conducted a systematic spectral analysis of the X-ray flares of GAMMA-RAY BURSTs (GRBs) observed by SWIFT/X-ray Telescope from 2005 April to 2015 March. The sample includes 521 flares from 206 GRBs. The GRBs cover the three subtypes: X-ray flashes (XRFs), X-ray-rich GRBs (XRRs), and classical GRBs (C-GRBs). We used a simple power-law model to fit the spectra during the flares, as well as to fit the preflare and postflare afterglow emissions, and obtained the parameters such as photon index and intrinsic hydrogen column density ($N_{\rm H}$). By comparing the spectral characteristics of flares, prompt emission, and afterglow emission, and analyzing the temporal evolution of the X-ray flare spectra, we obtained the following main conclusions. (1) The spectrum during the flare phase is significantly harder than that of the preflare and postflare phases, while there is no obvious difference in the spectrum between the preflare and postflare phases. (2) The intrinsic $N_{\rm H}$ shows no significant change between the preflare and flare phases, but significantly decreases after the flare. (3) The overall X-ray flare spectra are softer than those of the prompt emission. (4) For GRBs with multiple flares, the photon index softens with increasing flare peak time. (5) The X-ray flare spectra in XRFs are softer than those in C-GRBs. These results support the origin of X-ray flares being from the internal shock radiation driven by the late activity of the GRB central engine.
[abstract 16 / 45] Yes (score: 4) - Title: A Generalized Framework for Rapid Polarization Response Generation in Wide Field-of-View Compton PolarimetersAuthors: Mohamed Gamal Zaid, Merlin Kole, Mark McConnell, Fabio Muleri, Hancheng Li,Comments: 34 pages, 18 figures, Accepted for publication in ApJSubjects: astro-ph.IM astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Polarimetry is the most direct probe of the unsettled radiation mechanism and MAGNETic field structure of GAMMA-RAY BURST (GRB) prompt emission at the energies where it peaks, tens of keV to about 1 MeV. Compton polarimeters use the azimuthal scattering angle distribution (ASAD), a 180 degree modulation on axis. GRB measurements have largely relied on the on-axis modulation factor $μ_{100}$. For a wide field-of-view planar polarimeter, GRBs arrive off axis, where the Klein-Nishina projection adds harmonics to the ASAD. Muleri (2014) described this projection and evaluated it in a low-energy expansion for X-rays. We evaluate it numerically without approximation over the whole prompt-emission energy band for any incidence and POLARIZATION angles, quantify the off-axis harmonics a single modulation factor cannot capture, and verify the model against GEANT4 simulations of an ideal polarimeter. We also include the effect of the detection threshold on the ASAD. With POLAR as the case study, we present two modes that build the full POLARIZATION response with at least 95 percent fewer Monte Carlo simulations. Mode 1 takes only the unpolarized simulation per energy and recovers the POLARIZATION measured with POLAR's full GEANT4 responses for all but the brightest GRBs, where it underestimates the POLARIZATION degree. Mode 2 adds two polarized simulations per energy at distinct angles and reproduces the simulated ASADs to their statistical noise and the POLARIZATION of every GRB tested. Both modes are released as open-source software for any planar Compton polarimeter.
[abstract 17 / 45] Yes (score: 4) - Title: Charged fluid tori with an approximate MAGNETic self-field around MAGNETized Schwarzschild BLACK HOLEs: A semi-analytic approachAuthors: Abylaikhan Tlemissov, Jiri Kovar,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
We study toroidal structures formed by a charged, non-self-gravitating perfect fluid orbiting a Schwarzschild BLACK HOLE immersed in a poloidal MAGNETic field. To obtain analytic and semi-analytic solutions, we assume a cold, rest-mass-dominated fluid with uniform specific charge and zero conductivity, so the current is purely convective. This regime is formally opposite to the ideal GRMHD limit. The total MAGNETic field comprises a prescribed asymptotically uniform external component and an approximate self-field associated with the azimuthal current in the torus. We represent the latter by a regularized dipole approximation to the field of an effective circular current loop. Neglecting the self-field, the method of characteristics yields a general implicit solution of the integrability condition for a function parametrizing the specific-angular-momentum profile. A separately obtained cylindrically dependent class recovers a solution from our earlier work. For the radially dependent class, we integrate the Euler equations, obtain the enthalpy potential, and derive local conditions for equatorially centered tori. We then examine the field-free limit, both MAGNETic components separately, and their superposition. The external field supports closed tori within analytically derived parameter bounds, whereas no such equilibrium is found for the isolated approximate self-field within the numerically explored domain. In a representative combined-field sequence, the radial extent varies nonmonotonically with relative self-field strength: it increases for weak self-fields and decreases as the self-field becomes comparable to the external field. The results show how an approximate MAGNETic self-field modifies the morphology and domain of existence of charged-fluid tori.
[abstract 18 / 45] (score: 3) - Title: Search for high-energy neutrinos from Einstein Probe detected Fast X-ray Transients using 14 years of IceCube muon track dataAuthors: Sri Devaki Meduri, Shantanu Desai,Comments: 11 pages, 1 figureSubjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
We perform a time-integrated search for high energy neutrinos from 27 fast X-ray transients (FXTs) detected by Einstein Probe, using 14 years of publicly available IceCube muon-track data. We employ the unbinned maximum likelihood method which is used for IceCube point source searches. We do not find any statistically significant excess from any of the FXTs. The largest TS value is obtained for EP240801a (TS=4.77), corresponding to a local $p$-value of 0.04, which is not significant. We therefore calculate 90\% confidence level upper limit on the differential muon neutrino flux. The most stringent upper limit is obtained for EP241021a, with $E^2 Φ(E)=2.1\times 10^{-10}$ (GeV cm$^{-2}$ s$^{-1}$), for a $E^{-2}$ spectrum at a pivot energy of 100 TeV.
[abstract 19 / 45] (score: 3) - Title: Lomb-Scargle Recovery of Periodic Binary Signals across Black Hole Mass and CadenceAuthors: Karan Akbari, Sayantan Bhattacharya,Comments: 26 pages, 7 figures, 5 tablesSubjects: astro-ph.GA astro-ph.HE astro-ph.IMCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Searches for periodic supermassive BLACK HOLE binaries in QUASAR light curves rely on recovery fractions, the share of injected signals detected, which forecasts use as detection efficiencies. Lin, Charisi, & Haiman (2026) measured them for the Lomb-Scargle periodogram on damped-random-walk light curves matched to 12,400 bright, high-mass Palomar Transient Factory (PTF) QUASARs with Sloan Digital Sky Survey Data Release 7 (DR7) masses. To test them over four decades of mass, we inject their sinusoidal and sawtooth signals into light curves of mergers in the TNG100-1 cosmological simulation, with magnitudes drawn from DR7 QUASARs of similar mass (extrapolated at low mass). We apply their threshold in each frequency bin, set by $10^5$ noise-only light curves per binary, on observed PTF cadences, one Stripe 82 cadence and an LSST-like cadence (Legacy Survey of Space and Time). At fixed absolute magnitude $M_i=-23$, sinusoid recovery falls toward high mass, and with DR7 magnitudes it climbs above about $10^8\,M_\odot$, so the magnitude assignment sets the sign of the trend. Above $10^8\,M_\odot$, where their sample lies, PTF sinusoid recovery is 39.8 against their 44.7 per cent. At LSST-like cadence sinusoid recovery is 76.9 per cent, about three times their 22.6 per cent, for reasons mostly unidentified. Denser sampling of the same PTF baselines did not lower recovery in any test. Even at LSST-like cadence we miss most sawtooth signals above $10^8\,M_\odot$. We tabulate recovery per 0.5-dex mass bin and cadence, with low-mass values likely too high for a deeper survey.
[abstract 20 / 45] (score: 3) - Title: Quasinormal modes of Type I perturbations of dilaton-Euler-Heisenberg BLACK HOLEsAuthors: Yu-Xuan Wang, De-Cheng Zou, Yun Soo Myung, Sheng-Yuan Li, Ming Zhang,Comments: 26 pages, 13 figuresSubjects: gr-qcCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
We study the type I quasinormal modes (QNMs) of MAGNETically charged dilaton--Euler--Heisenberg (dEH) BLACK HOLEs, where axial gravitational and polar electroMAGNETic perturbations are coupled. Direct integration and Chebyshev pseudospectral methods give consistent QNM frequencies for the fundamental branches continued from Schwarzschild at $\ell=1,2,3$. Varying $α$ at fixed $ζ=α-β$ changes the spectrum on the same background. The damping response depends on charge and multipole and can have opposite signs for the two coupled branches. For $ζ<0$, dipole damping decreases with charge toward horizon merger. For $ζ>0$, the Type I charge range extends beyond the complementary POLARIZATION's local angular-gradient bound. All tracked modes remain damped in the nonextremal ranges, supporting the stability of these branches.
[abstract 21 / 45] (score: 3) - Title: FRB 20210601A: Extreme Temporal Clustering in a Repeating Fast Radio Burst Source as Evidence for a Hidden Class of Episodic RepeatersAuthors: Ryan Mckinven, Amanda M. Cook, Alice P. Curtin, B. M. Gaensler, Jason W. T. Hessels, Naman Jain, Lordrick Kahinga, Victoria M. Kaspi, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Fengqiu Adam Dong, Maxwell Fine, Emmanuel Fonseca, Afrokk Khan, Bikash Kharel, Calvin Leung, Robert Main, Kiyoshi W. Masui, Kyle McGregor, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Aaron B. Pearlman, Ziggy Pleunis, Mawson W. Sammons, Paul Scholz, Kaitlyn Shin, Seth R. Siegel, Kendrick Smith, Ingrid Stairs,Comments:Subjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Population studies of fast radio burst (FRB) repetition typically model sources using a single distribution of steady, time-averaged burst rates, yet individual sources show significant departures from this assumption. Here we present FRB 20210601A, a source discovered by the Canadian Hydrogen Intensity Mapping Experiment FRB project (CHIME/FRB) that represents the most extreme such departure yet identified. The source produced at least nine bursts within a single 106.5 s interval -- the highest instantaneous burst rate yet reported from a repeating FRB source at $\gtrsim 2$ Jy ms fluences -- yet remained otherwise undetected despite $\sim 320$ hr of exposure spanning 7 yr. The active interval occurred while the source was in a side-lobe of the CHIME/FRB digitized beams, implying an instantaneous burst rate $\gtrsim2.3\times$ higher ($\gtrsim$ 21 bursts) at main-lobe sensitivity. The source's intense, brief burst storm flanked by apparent quiescence despite substantial exposure is unique among the CHIME/FRB repeater sample, although its burst morphology, excess dispersion measure ($\rm{DM_{excess}} \sim 360$ pc cm$^{-3}$), Faraday rotation measure ($|\rm{RM_{excess}}| \sim 150-170$ rad m$^{-2}$), and temporal scattering ($τ\lesssim 0.37$ ms at 600 MHz) are otherwise typical. Modeling a population of episodically active repeaters (i.e., short burst storms separated by long recurrence times) and accounting for declination-dependent exposure, we forecast $\sim1-4$ additional source discoveries similar to FRB 20210601A over the next decade of CHIME/FRB operations, corresponding to a CHIME/FRB-detectable population of $9^{+200}_{-8}$ sources (68% credible interval). These results demonstrate that highly episodic repeaters could constitute a selection-biased but detectable component of the FRB population, possibly reflecting distinct MAGNETospheric states or triggering mechanisms.
[abstract 22 / 45] (score: 3) - Title: Synthetic 2D MAGNETic turbulence with controlled island structuringAuthors: Yari De Paep, Daniela Maci, Rony Keppens,Comments: 16 pages, 9 figures, accepted for Journal of Plasma PhysicsSubjects: physics.plasm-ph astro-ph.HE astro-ph.SRCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Magnetic turbulence remains up to this day not fully understood, despite its important role in the behavior of plasmas. A recurring ingredient in plasma turbulence is the spontaneous formation and evolution of plasmoids. These represent MAGNETic islands on current sheets in two-dimensional turbulent MAGNETic fields that are consistently found in high-resolution direct numerical simulations (DNSs) using a MAGNETohydrodynamic description. However, such simulations require considerable amounts of computational power. Synthetic turbulence models provide an alternative, cheap approach to the generation of fully-developed turbulent fields. In this work, we first present an extension of our open-source, general synthetic turbulence BxC toolkit that is specifically tailored to generate 2D turbulent MAGNETic fields. We then use a novel physically motivated, but purely geometric construction that generates current sheet island chains, which results in fields that visually match the ones obtained through DNSs. We show how this construction affects the MAGNETic field lines and find a correlation with the formation of MAGNETic O-points and X-points. The MAGNETic flux and size of the islands in the field are found to match well with theoretical scaling laws. Lastly, we show BxC's capabilities by generating a 2D $N\times N$ turbulent MAGNETic field of resolution $N = 100000$, going beyond the state-of-the-art reached by simulations, on a single CPU with modest computational resources. Our construction maintains direct control over the inertial range, and allows to make morphological changes to the plasmoids and fields, demonstrating plasmoid appearance, disappearance and merging.
[abstract 23 / 45] (score: 3) - Title: A Catalog of Spectral Properties for DESI DR1 QuasarsAuthors: Qiaoya Wu, Yue Shen,Comments: 17 pages, 10 figures, and 2 tables. Preprint version; comments and feedback are welcomeSubjects: astro-ph.GACreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
The Dark Energy Spectroscopic Instrument (DESI) is carrying out a five-year spectroscopic survey designed to map the large-scale structure of the Universe and obtain spectra for millions of galaxies and QUASARs over a wide redshift range. We present a value-added catalog of spectral properties for 1,717,774 unique QUASARs (1,774,723 spectra) in the DESI Data Release 1. We perform a uniform spectral decomposition of the QUASAR continuum, host galaxy emission (at $z<1$), and \FeII\ emission, and measure the line properties of major broad and narrow emission lines from Ly$α$ to H$α$ covered by DESI spectra. We also provide single-epoch BLACK HOLE mass estimates (from H$β$, \MgII, and \CIV), bolometric luminosities, and Eddington ratios for these QUASARs. We provide systemic redshifts that account for the intrinsic velocity shifts of individual lines; they agree with the DESI pipeline redshifts to within 500~km s$^{-1}$ for 88.6\% of the sample, and are most useful at $z>1$ where the pipeline redshift is heavily constrained by blueshifted high-ionization lines. We also provide local fits to several optical coronal lines, including \NeV~$\lambda3426$, [\ion{Fe}{7}]~$\lambda5722$, [\ion{Fe}{7}]~$\lambda6088$, and [\ion{Fe}{11}]~$\lambda7893$. We show that several emission-line ratios, including those involving coronal lines, vary systematically with Eddington ratio. The catalog is intended as a community resource for studies of QUASAR demographics, BLACK HOLE accretion, emission-line physics, and the connection between the broad-, coronal-, and narrow-line regions.
[abstract 24 / 45] (score: 2) - Title: Tandem JETs in crossflow: a one-parameter dilution law for the trajectory and the velocity decayAuthors: Xunchen Liu,Comments: 52 pages, 16 figuresSubjects: physics.flu-dynCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
The front JET of a tandem pair in crossflow is not passive. This paper treats the mean-flow phenomenology and its scaling; the mechanism is left to the companion paper. In 40\ kHz time-resolved PIV measurements covering nine spacing--velocity-ratio conditions ($L=2d$, $3d$, $4d$; $r\approx3$, $5$, $7$) and a single-JET baseline, the front-JET $rd$-normalized trajectory lies below the single-JET reference in every condition (near-field segment up to 40\% shorter), while the shielded rear JET rises above the reference in eight of the nine and penetrates $1.4$--$2.0$ times deeper than the front JET. The mean pressure and reverse-flow statistics are inconsistent with the two classical explanations: the inter-JET region is pressurized rather than sub-atmospheric, the lateral pressure difference across the front JET is weakened rather than enhanced (within reconstruction uncertainty), and the reverse-flow region does not follow the ordering of the modification. In natural coordinates the centerline decay re-scales onto the single-JET law at the effective velocity ratio (seven of nine within 18\%), so bending and decay are two readouts of one dilution, which whole-trajectory matching condenses into the one-parameter law $r_{\mathrm{eff}}/r=r/(r+c)$, $c=3.31$, with the velocity ratio as the primary control and the spacing entering through the near-field capacity ($c_h=2.50$--$3.30$). The law has one fitted constant and needs only the single-JET reference family; leave-one-condition-out predictions reproduce each held-out condition within 15\%, so the procedure is portable to any tandem array in which the gap recirculation closes.
[abstract 25 / 45] (score: 2) - Title: Geodesic torsion of the MAGNETic field line and other predictors of coil non-planarity in QI stellaratorsAuthors: Andrea Pavone, Sehyun Kwak, Felix Warmer,Comments:Subjects: physics.plasm-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Stellarator MAGNETic fields are often realized with non-planar modular coils with their out-of-plane bending being one of the main engineering challenges. We ask whether the non planarity of the fialment can be predicted from the equilibrium alone. We look at a dataset of coils for stellarator equilibira and find that the geodesic torsion of the MAGNETic field line is a strong and robust predictor in a wide range of coil feasibility requirements. We compare the performance of the geodesic torsion against other equilibrium and surface geometry properties and find it to be a superior predictorv hardly replaceable by other quantities we considered in this dataset. The ranking it induces also reproduces the ordering of four published configurations --- precise QA, precise QI at nfp 2 and 3, and W7-X. Our conclusions suggest that geodesic torsion of the MAGNETic field line may be considered as a cheap and robust candidate for a stage-one non-planarity proxy.
[abstract 26 / 45] (score: 2) - Title: CMB Bounds on Primordial Black Holes via Radiation CaptureAuthors: Marzieh Farhang, S. M. S. Movahed,Comments: 6 pages, 4 figuresSubjects: astro-ph.COCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
We explore the capture of neutrinos and photons in the cosmic neutrino and photon background by primordial BLACK HOLEs (PBHs). We model this phenomenon as a gravitational interaction that effectively modifies the continuity equations for radiation and PBH densities and the cosmic expansion history. We find that the observability of this modified cosmic history is highly sensitive to PBH mass, and only extraordinarily massive PBHs would leave observable trace on the temperature and E-mode POLARIZATION of the cosmic microwave background (CMB). Specifically, Planck data restrict PBH abundance to $f_{\rm pbh}\lesssim 10^{-1}$ for PBH masses above $10^{15} M_\odot$, getting considerably tighter for higher masses. We expect substantial improvement as high-resolution measurements of larger CMB multipoles become available. A future cosmic-variance-limited experiment, with $\ell_{\rm max}=7000$, would set $f_{\rm pbh}\lesssim 10^{-1}-8\times 10^{-5}$ (for the fiducial $Λ$CDM cosmology) across $10^{13}-10^{18}M_\odot$. These constraints would be comparable to the current limits at the high-mass end of the spectrum [Carr et al, 2026]. The gravitational interaction of PBHS with the cosmic background radiation and its imprints on CMB would thus provide an independent complementary probe of extraordinarily massive PBH abundance.
[abstract 27 / 45] (score: 2) - Title: No Strong Evidence for Plasma Lensing in FRB 20240114AAuthors: Jiarui Niu, Nan Xu, Xiaohui Liu, Songyu Shen, Junshuo Zhang, Tiancong Wang, Pawan Kumar, Yuanhong Qu, Dejiang Zhou, Weiwei Zhu, Bing Zhang, He Gao, Dongzi Li, Jinlin Han, Di Li, Xuelei Chen, Kejia Lee, Ye Li, Weiyang Wang, Qiuyang Fu, Jiawei Jin, Yanqing Cai, Caisong Liu, Shuo Cao, Ziwei Wu, Dengke Zhou, Longxuan Zhang, Wanjin Lu, Yi Feng, Chenhui Niu, Jiawei Luo, Rui Luo, Chunfeng Zhang, Shiqian Zhao, Chengwei Liang,Comments: 13 pages, 4 figures, accepted for publication in ApJLSubjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
FRB 20240114A is an extremely active repeating fast radio burst for which plasma lensing has been proposed to explain its burst-rate variations, spectral evolution, and apparently ``carbon-copy'' burst pairs. Using FAST data and publicly available Parkes observations, we test this interpretation with the predictions of a one-dimensional Gaussian plasma-lens model. Although the burst-rate enhancements may be fitted separately for Parkes and FAST, the corresponding magnification peaks and demagnification troughs between the two datasets are offset from each other, inconsistent with plasma lensing predictions. The enhancement peaks also do not show consistent periodicity, disfavoring a binary plasma lensing origin. The burst bandwidths are not systematically narrower during the proposed lensing interval than in other episodes. Most importantly, the burst energy distribution, which shows an intrinsic turnover peak at low energies, shows no significant shift of the turnover during the magnification interval, providing a model-independent test to the plasma-lensing interpretation. All these suggest that there is no strong evidence in favor of a plasma lensing interpretation to the source. Rather, all the burst property variations are consistent with being caused by the intrinsic variations of the FRB central engine.
[abstract 28 / 45] (score: 2) - Title: Decoupling candidate dual AGN from chance superpositions in the GOTHIC survey via a deep-learning frameworkAuthors: Bhavesh Mukheja, Snehanshu Saha, Anwesh Bhattacharya, Mousumi Das, Françoise Combes, Sudhanshu Barway,Comments: Submitted to MNRAS. Supplementary Material merged in the main textSubjects: astro-ph.GA cs.CV cs.LG math-ph math.MP physics.data-anCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Dual ACTIVE GALACTIC NUCLEi (DAGN) mark a critical phase in the evolution of merging galaxies and the pairing of supermassive BLACK HOLEs, yet they remain difficult to identify in large imaging surveys because of projection effects and limited spatial resolution. Compact foreground stars and unresolved substructure can mimic dual nuclei through chance superposition, complicating automated detection. We revisit the 46,061 galaxies flagged but rejected as DAGN candidates by the GOTHIC pipeline, primarily because the two nuclei fell within the SDSS fibre aperture or exceeded its separation threshold. We train a supervised deep-learning framework based on the YOLOv11 oriented-bounding-box architecture on annotated SDSS imaging to separate genuine dual nuclei from foreground stellar contaminants and other spurious alignments. The final model attains a validation precision of 0.919, recall of 0.905, and $F_1$ of 0.912, and yields 29,605 dual-nucleus candidates after removing star-dominated and blended detections. Structured visual inspection indicates that $54.5$--$62\%$ are consistent with genuine dual nuclei, implying $\sim(1.4$--$1.8)\times10^{4}$ plausible systems. Cross-calibrating the YOLO separation against the deterministic GOTHIC centroid measurement and restricting to the compact regime ($d \le 6.87''$) gives a conservative subset of $\sim 13{,}672$ candidates, reaching calibrated separations of $\sim 0.56''$. Spectroscopy of the most compact ($\le 1$~kpc) systems shows spectra dominated by stellar absorption, with no resolved double-peaked emission, so confirmation requires higher-resolution follow-up. The catalogue is a statistically refined list of candidates, not confirmed DAGN. Nonetheless, deep-learning detection substantially reduces contamination and expands the plausible DAGN census.
[abstract 29 / 45] (score: 2) - Title: Filament Formation via Collision-induced Magnetic Reconnection -- Kinematic FeaturesAuthors: Shuo Kong, Griselda Arroyo-Chávez, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, Duo Xu, Szu-Ting Chen,Comments: 18 pages, 8 figures, accepted by PASPSubjects: astro-ph.GA physics.plasm-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
The Collision-induced Magnetic Reconnection (CMR) mechanism has recently been proposed as a filament formation model that emphasizes the active role of MAGNETic fields. To enable better observational tests with data from modern telescopes, we provide more specific observable predictions for filaments formed via CMR. Two types of CMR kinematics are revealed in position-velocity (PV) diagrams. First, due to the nature of CMR, the midplane contains a {\it converging motion} close to the filament and two {\it diverging motions} farther from the filament. They exhibit a blueshift, redshift, blueshift, redshift (BRBR) velocity pattern along the line-of-sight when the collision midplane is inclined, giving rise to a special pattern in the PV-diagram. Second, the longitudinal PV-diagram along the filament spine exhibits a velocity oscillating pattern, which is currently attributed to the MAGNETic transport of gas clumps in the {\it converging motion}. The first type of pattern involves emission primarily outside the filament, which can be confused with the environment. The second type, however, mainly emerges from gas inside the filament, thus more robust for observational tests. Both the integral-shaped filament and the Stick filament in the Orion A cloud show the velocity oscillation in PV-diagrams, although the spatial oscillation frequency and their velocity spread differ.
[abstract 30 / 45] (score: 2) - Title: Energy-dependent trapping of backscattered helium during MAGNETron sputtering growth: A molecular dynamics studyAuthors: Pascal Brault, Anne-Lise Thomann, Alejandro Borroto,Comments:Subjects: physics.comp-ph physics.plasm-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Helium incorporation during MAGNETron sputtering can strongly affect thin film growth and lead to the formation of gas/solid nanocomposites and nanoporous structures. Here, molecular dynamics (MD) simulations are used to investigate the trapping mechanism of helium atoms (He) and the subsequent formation of He bubbles during the sputter deposition of aluminum (Al) and titanium (Ti) thin films. The simulations account for the kinetic energy distributions of sputtered metal atoms and backscattered gas species. Results indicate that He is efficiently incorporated into the growing films, leading to the formation of high-pressure, dense He bubbles, with a much higher He-to-metal atomic ratio in Ti ($\sim$ 60%) than in Al ($\sim$ 12%). More importantly, the simulations reveal a clear energy dependence of He trapping in Ti: background He atoms at thermal energies are essentially not incorporated, whereas efficient trapping starts at an incident energy of approximately 20 eV and increases up to a saturation regime near 100 eV. Simulated thermal desorption spectroscopy (TDS) further reveals distinct release mechanisms in the two investigated metals: He desorption from Al occurs at higher temperatures and is preceded by the removal of surface Al atoms, whereas He and Ti atom desorption starts continuously around 950 K, leading to a porous structure. Comparative simulations with argon (Ar) demonstrate negligible trapping even at comparable kinetic energy or momentum, showing that neither parameter alone accounts for the strong He incorporation observed in Ti. The above results are in very good agreement with what is reported in literature for low-kinetic energy He ion implantation in metal surfaces, suggesting similar insertion mechanisms. They clarify the atomistic conditions governing noble gas trapping during film growth and provide a basis for controlling He incorporation and porosity in films synthesized by MAGNETron sputtering.
[abstract 31 / 45] (score: 2) - Title: Pseudo-spectral methods in gravitational lensing: Spin precession in loop quantum BLACK HOLE spacetimesAuthors: Xiankai Pang, Xiao-Kan Guo,Comments: references added; 24 pages, 6 figures, 3 tables; comments welcomeSubjects: gr-qcCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Gravitational lensing is usually treated as an initial value problem: for a given impact parameter of an unbound orbit, one computes the resulting deflection angle. In this paper we advocate the inverse point of view. For a prescribed deflection angle, the orbit is selected by two boundary conditions at spatial infinity, so that the lensing problem becomes a well-defined two-point boundary value problem, with the impact parameter playing the role of a nonlinear eigenvalue. We show that pseudo-spectral methods based on Chebyshev collocation solve this boundary value problem accurately at modest computational cost, and that the parallel transport equations governing the spin precession of the particle reduce to a single linear system on the same grid. As a concrete application, we compute the spin precession of massive particles in backward scattering off two BLACK HOLE spacetimes from loop quantum gravity, the covariant effective metric and the self-dual loop quantum BLACK HOLE. We find that the quantum corrections are most pronounced for slowly moving particles, while in the ultra-RELATIVISTIC limit the universal spin flip is always recovered. The flip itself is universal, but the rate at which it is approached is not. The derivative of $\cosξ$ with respect to the particle speed at $v=1$ depends on the quantum parameters of both spacetimes. The framework is not restricted to the models studied here and applies to any static, spherically symmetric spacetime.
[abstract 32 / 45] (score: 2) - Title: Exploring PSR J0901-4046 as an ultra-slowly rotating neutron star versus a white dwarfAuthors: Banibrata Mukhopadhyay, Nirupam Roy, Zenia Zuraiq, Chandrachur Chakraborty, A R Rao,Comments: 13 pages including 5 figures (14 png files) and 2 tables; accepted for publication in The Astrophysical Journal (ApJ) -- see Paper II as the companion paper titled: "Exploring the origin of slow-rotating pulsars: Emission from STARS simulated white dwarfs" also accepted for publication in The Astrophysical Journal (ApJ)Subjects: astro-ph.HE astro-ph.SR gr-qcCreated: 2026-10-20; Updated: 2026-10-23; Datestamp: 2026-10-23
The source PSR J0901-4046 shows a very long rotational period, of $\approx 75.88$ s. In fact, its long period suggests that it could be a white dwarf. We examine the properties of the source and compare the outcomes under the hypotheses of the source being a highly MAGNETized white dwarf (B-WD) and neutron star. We find that assuming it to be a B-WD with a surface field $\sim 10^{10}$ G explains many properties, including its storage/rotational energy, explaining luminosity. On the contrary, the neutron star-based idea, particularly if examined under the conventional spin down mechanism, requires an unusually high surface MAGNETic field $\gtrsim 10^{14}$ G, even exceeding $10^{16}$ G, depending on the obliquity angle and emission mechanism. The source also sits very close to AR Sco, a white dwarf pulsar, in the period and period-derivative plane. We suggest that the source is a B-WD. Along with AR Sco, it being a B-WD constrains the death line model. B-WD hypothesis alleviates the necessity of an unusually high MAGNETic field hindering pair production for PSR J0901-4046 under the neutron star hypothesis. We argue that some rotation-powered pulsars with extreme properties may possibly be white dwarfs rather than neutron stars.
[abstract 33 / 45] (score: 2) - Title: Charting the Galactic Underworld II: Strategies for Identifying BHs and NSs with LISAAuthors: Tom Wagg, Frank E. Prince, Katelyn Breivik, Kira Baasch, Jorie McDermott, Michael Zevin,Comments: 18 pages, 6 figures, submitted to AAS journals - comments welcome!Subjects: astro-ph.SR astro-ph.GA astro-ph.HECreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
Stellar-mass BLACK HOLEs (BHs) and neutron stars (NSs) observed by space-based gravitational-wave detectors offer constraints on binary stellar evolution that are complementary to those from ground- based detectors. The Laser Interferometer Space Antenna (LISA) is expected to detect hundreds of double compact objects (DCOs) containing a BH or NS, but distinguishing these sources from the far more numerous double white dwarfs (WDWDs) may prove challenging. We use adaptive importance sampling with COSMIC to synthesise large populations of BHBH, BHNS, NSNS, BHWD, and NSWD binaries. We combine these binaries with a Milky Way star-formation history and integrate their Galactic orbits with cogsworth, repeating our simulations for a grid of variations in uncertain (binary) stellar physics. We find that LISA detections are largely insensitive to the changes in Galactic position resulting from natal kicks. We then assess how well chirp mass, eccentricity, distance from the Galactic plane, and orbital frequency distinguish BH- and NS-hosting DCOs from WDWDs, accounting for LISA measurement uncertainties. Using chirp mass alone distinguishes only 50-60% of BHBHs and BHNSs, and ~40% of NSNSs, but combining this with orbital frequency recovers 90-100% of BHBHs and BHNSs and around ~50% of NSNSs, with eccentricity further improving the recovery of NSNSs to around 60-70%. Distance from the Galactic plane adds little discriminating power, though it can recover a handful of NSWDs that are missed otherwise. These methods will help identify a significantly larger number of BHs and NSs in LISA data that would be missed by a chirp mass cut alone.
[abstract 34 / 45] (score: 2) - Title: Plasma transport by carrier electrons: classical coefficients across ionization and MAGNETizationAuthors: C. A. Walsh,Comments:Subjects: physics.plasm-phCreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
The classical transport of MAGNETic field and electron energy in a plasma requires the use of coefficients that depend on plasma ionization $Z$ and MAGNETization $χ$. This paper explains these scalings through studying the electron velocities responsible for each transport process. Both electron-electron collisions and MAGNETization affect higher velocity electron populations preferentially, lowering the carrier velocities; transport carried by a high energy electron population is therefore more suppressed by both electron-electron collisions and MAGNETization than transport carried by lower velocities. Carrier Hall parameters $ψ=χf(Z)$ are defined for each coefficient such that MAGNETization can be described independent of ionization. An analytic idealized coefficient with a single rigid carrier velocity reproduces many of the characteristics of the coefficients, in particular thermal conductivity, but overestimates plasma MAGNETization due to MAGNETization itself lowering the carrier velocity. A single moving carrier model improves agreement, but cannot describe the smoothness of the Righi-Leduc coefficient, which originates from being an average over a range of carrier velocities. This is the first paper in a 3-part series; the subsequent papers will extend the carrier picture to non-local heat-flux (paper 2) and non-local MAGNETic field evolution (paper 3).
[abstract 35 / 45] (score: 2) - Title: The PAU Survey: Active galactic nucleus galaxies in galaxy pairsAuthors: F. Duplancic, M. Siudek, D. Navarro-Gironés, E. J. Gonzalez, F. Rodriguez, S. Alonso, I. V. Daza-Perilla, D. G. Lambas, E. Gaztañaga, A. L. O'Mill, M. Eriksen, J. Carretero, R. Casas, F. J. Castander, J. García-Bellido, H. Hildebrandt, M. Mezcua, R. Miquel, C. Padilla, P. Renard, E. Sánchez, S. Serrano, I. Sevilla-Noarbe, P. Tallada-Crespí,Comments: 16 pages, 18 figures, accepted by A&ASubjects: astro-ph.GA astro-ph.COCreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
Aims. Leveraging the high-precision photometric redshifts of the Physics of the Accelerating Universe Survey (PAUS), we aim to investigate the connection between ACTIVE GALACTIC NUCLEi (AGNs) and galaxy pairs up to redshifts of $\sim1.0$. Methods. We identified 16,824 galaxy pairs with projected separations of $r_p < 100$ kpc and radial-velocity differences of $ΔV < 3500$ km s$^{-1}$. AGNs were selected by cross-matching PAUS galaxies with multi-wavelength AGN catalogues, yielding 270 AGNs in pairs out of a parent sample of 8,880 AGNs in PAUS. We constructed control samples of isolated AGNs; non-AGNs in pairs; and isolated non-AGNs matched in redshift, absolute magnitude, and environment. Results. Active galactic nuclei in pairs show progressively redder rest-frame colours with increasing redshift, particularly at redshifts of $z\gtrsim 0.5$, whereas isolated AGNs and non-AGNs in pairs show no significant colour evolution and remain at $\mathrm{M_g-M_r}\sim0.65$. Pairs hosting AGNs are also preferentially morphologically disturbed interacting systems found at smaller projected separations and velocity offsets, consistent with more dynamically advanced interactions. Conclusions. These results provide evidence of a redshift-dependent link between galaxy interactions and AGN activity, suggesting that interactions play an increasingly important role in triggering nuclear activity at intermediate redshifts. This study highlights the unique capability of PAUS to probe AGN-galaxy interaction connections beyond the local Universe with unprecedented statistical power.
[abstract 36 / 45] (score: 2) - Title: Evolution of Jeans instability in nonthermal MAGNETized complex plasmasAuthors: Dipankar Ray, Pralay Kumar Karmakar, Bharati Kakad, Amar Kakad,Comments: 9 pages, 3 figures. Prepared for submissionSubjects: physics.plasm-ph astro-ph.HE astro-ph.SRCreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
The classical Jeans instability framework provides a conceptual foundation for understanding self-gravitational collapse and subsequent STAR FORMATION in interstellar environments. However, cosmic plasmas are inherently MAGNETized and frequently collisionless, exhibiting significant departures from local thermodynamic equilibrium. While linear theories predict initial instability thresholds, they fail to track the long-term nonlinear runaway dynamics. We present a fluid simulation investigating the nonlinear evolution of the Jeans instability in a MAGNETized tricomponent complex (dusty) plasma. The constituent nonthermal electrons and ions are governed by the $κ$-distribution law, while the heavier dust grains are treated in a fluid framework, coupled with a uniform ambient MAGNETic field. The numerical architecture utilizes a fourth-order finite difference method (FDM) for spatial gradients and a second-order leap-frog time-integration scheme. We systematically investigate the complex interplay among the self-gravitational attraction, nonthermal electrostatic screening, and MAGNETic pressure across a wide range of MAGNETic field strengths and degrees of nonthermality. It is found that enhanced nonthermality accelerates structural localization, while the MAGNETic field introduces a critical pressure barrier that suppresses the instability. In highly MAGNETized environments, thermal and nonthermal systems exhibit identical growth rate characteristics, indicating that MAGNETic pressure dominates the nonthermal thermostatistics in the strong MAGNETic regime. This study develops a comprehensive and numerically robust framework to understand early-stage STAR FORMATION and evolution processes in nonthermal astrophysical media.
[abstract 37 / 45] (score: 2) - Title: Predicting droplet landing in angle-controlled surface acoustic wave JETtingAuthors: Md Aminul, Sara Adibi, James Friend,Comments: 29 pages; 6 figuresSubjects: physics.flu-dynCreated: 2026-10-21; Updated: 2026-10-23; Datestamp: 2026-10-23
Nozzle-free droplet generation eliminates the need for a dispensing orifice, but useful printing also requires control over where droplets are deposited. Here we demonstrate predictable droplet deposition using a nozzle-free, angle-controlled surface acoustic wave JETting platform. Opposing focused interdigital transducers steer droplets from a pendant parent drop toward a collection substrate, with the ejection angle set by the time-integrated acoustic acceleration imbalance. The overall acceleration ratio identifies the operating window for single-droplet ejection and separates it from no-ejection, satellite-droplet, and multiple-droplet regimes. We then connect ejection angle to landing position through a geometric deposition model referenced to a balanced shot in each experiment. At a 5.2 mm parent-drop-to-substrate spacing, 80 steered shots across twenty experiments show strongly anisotropic relative placement scatter: 0.59 mm in the steering direction and 0.06 mm transverse to it. In tests conducted independently over several days, a model calibrated on six earlier collection dates predicted landing positions on two later dates with a root-mean-square error of 0.71 mm; bootstrap resampling placed the 95% confidence range for this error between 0.41 and 1.01 mm. The results establish a practical framework for predicting relative droplet landing in angle-controlled surface acoustic wave JETting and identify the limits imposed by steering angle, separation distance, and actuation regime from an orifice-free, clog-free droplet ejection method.
[abstract 38 / 45] (score: 2) - Title: Perturbations, eikonal limit and Hawking radiation of diverse external fields in a non-minimal charged BLACK HOLEAuthors: Yinan Jia, Zhen-Hao Yang, Xiao-Mei Kuang,Comments: 19 pages,10 figuresSubjects: gr-qcCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
We compare the quasinormal modes (QNMs), greybody factors, and Hawking emission of massless scalar, electroMAGNETic, and Dirac test fields propagating on a non-minimal Einstein--Yang--Mills BLACK HOLE. The QNMs are calculated using WKB and pseudospectral methods, while greybody factors are estimated with sixth-order WKB method. All computed modes are damped within the parameter range considered. Higher overtones generally exhibit stronger dependence on the non-minimal coupling $ξ$ than the fundamental mode, including non-monotonic behavior in the scalar and Dirac sectors. For large multipole numbers, all three fields follow a common leading eikonal description governed by the unstable circular null orbit. Increasing $ξ$ raises the orbital angular velocity and reduces the Lyapunov exponent, leading to higher oscillation frequencies and weaker damping rate. The greybody factors depend strongly on the multipole number, with weaker field dependent corrections from $ξ$. The partial-wave emission powers generally decrease with increasing $ξ$, while the lowest scalar mode shows mild non-monotonic behavior. This comparison reveals enhanced overtone sensitivity alongside comparatively small changes in transmission, whereas the Hawking emission reflects changes in both the greybody factors and the BLACK HOLE temperature.
[abstract 39 / 45] (score: 2) - Title: Experimental evidence of forward energy transfer induced by core-edge coupling in multiscale tokamak turbulenceAuthors: F. Chen, Z. M. Shen, N. Sun, P. Li, Z. Y. Qiu, P. Liu, Z. Lin, H. T. Chen, J. S. Geng, Y. X. Li, P. J. Sun, E. Z. Li, X. M. Zhong, A. D. Liu, L. Zhang, J. Huang, Y. M. Duan, T. F. Zhou, H. L. Zhao, Q. Zang, Y. Q. Chu, S. X. Wang, H. Q. Liu, T. Zhang, Y. F. Jin, B. Lyu, C. B. Wu, Y. C. Hu, L. Ye, X. J. Wang, X. Z. Gong, Y. D. Li, J. G. Li,Comments:Subjects: physics.plasm-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Turbulence in MAGNETically confined plasmas is inherently quasi-two-dimensional and can exhibit both inverse and forward energy transfer across scales. Experimental evidence for cross-scale energy transfer in the hot plasma core has, however, remained scarce. Understanding such energy transfer is crucial because it governs turbulent transport, which directly impacts confinement quality of fusion plasmas. Here we report experimental evidence consistent with forward energy transfer associated with core-edge coupling in tokamak turbulence. We combined multichannel collective Thomson scattering (CTS) and radially localized Doppler backscattering (DBS) to resolve cross-scale fluctuation dynamics. The results reveal that a quasi-coherent mode (QCM) originating from the edge is also present in the core and resonantly couples with broadband turbulence, producing significant forward energy transfer and characteristic secondary instabilities. These combined measurements indicate that quasi-two-dimensional tokamak turbulence can support a net energy transfer from ion to electron scales through cross-scale wave-wave interactions, contrary to the inverse cascade paradigm of idealized two-dimensional turbulence. Such a plasma regime is attractive for fusion reactors, as it avoids large edge-localized modes (ELMs) that damage first-wall components and maintains high confinement quality even in the presence of high-Z impurities.
[abstract 40 / 45] (score: 2) - Title: Nonlinear Drift Waves and Electrostatic Density Cavities in Upper IonosphereAuthors: Hamid Saleem, Usman Saeed,Comments: 6 pages, 4 figures, 3 tablesSubjects: physics.plasm-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Nonlinear drift waves are investigated to explain the mechanism for the creation of one dimensional (1D) and two dimensional (2D) electrostatic density cavities in the presence of density gradient in direction perpendicular to the geoMAGNETic field. Ion motion along field lines has to be neglected for the formation of density depletion because nonlinear contribution of their parallel motion overcomes the effect of drift waves which create negative nonlinear potential. It is pointed out that a straightforward but appropriate model for drift waves can explain the generation of density cavities having widths in xy-plane if the external MAGNETic field is assumed to be along z-axis i.e. ${\bf B}_0 = B_0 \hat{z}$. The general nonlinear equation for drift waves takes the form of Zakharov-Kuznetson (ZK) equation when ion nonlinear vorticity term is ignored and it admits the solution in the form of 2D solitary wave. In 1D case, the ZK equation reduces to Korteweg de Vries (KdV) equation which admits solution in the form of 1D soliton. In both cases, the nonlinear potential becomes negative. The order of magnitude of the amplitude and width of density cavities is found to be in agreement with the satellite observations in upper ionosphere.
[abstract 41 / 45] (score: 2) - Title: On Spurious Mesh-Scale Oscillations Associated with Resonance-Cone Regimes in Wave-Plasma SimulationsAuthors: Hugo Bergerioux, Mario Merino,Comments: 33 pages, 18 figuresSubjects: physics.plasm-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Spurious mesh-scale oscillations can compromise frequency-domain finite-element simulations of electroMAGNETic wave propagation in MAGNETized cold plasmas. We investigate their origin and mitigation through a verification framework combining a mixed Nédélec-Lagrange solver, a waveport accommodating non-orthogonal modes in anisotropic media, and an analytical generalized Fresnel benchmark at a vacuum-plasma interface. Comparisons with this benchmark show that the observed oscillations occur in resonance-cone regimes and are absent from the analytical fields, confirming their numerical origin. Systematic tests assess the effects of approximation order, variational formulation, mesh geometry, and numerical collisionality. Plane-wave residual and Fourier spectral analyses suggest that local mesh variations induce spectral coupling to additional wavevector components, predominantly populating the dispersion branches in collisionless resonance-cone regimes where the reduced scalar equation loses ellipticity. Uniform rectangular grids recover the analytical wave structure, further supporting the role of mesh geometry and symmetry. However, strict symmetry requirements limit the applicability of this approach, motivating numerical regularization. In resonance-cone regimes, introducing sufficient numerical collisionality suppresses the mesh-scale oscillations, yielding smooth electric-field solutions and reducing the error relative to the analytical benchmark. For one resonance-cone benchmark configuration, the error-minimizing damping decreases with mesh refinement according to an empirical $Z_{\mathrm n}\propto h^{1.48}$ scaling, sustaining error reduction consistent with second-order convergence and avoiding the accuracy limit imposed by fixed collisionality. ...
[abstract 42 / 45] (score: 2) - Title: In Search of the Gravitational Wave of Fast X-Ray Transient in the Second Part of the LIGO-Virgo-KAGRA Fourth Observing RunAuthors: Po-Ya Wang, Albert K. H. Kong, Surojit Saha,Comments: Accepted for publication in PASP; 17 pages, 2 figures, 9 tablesSubjects: astro-ph.HECreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Fast X-ray Transients (FXTs) are brief, intense X-ray flashes unassociated with persistent X-ray sources or known stellar objects, typically lasting from seconds to hours. With the launch of the Einstein Probe in January 2024, the study of FXTs has entered a new phase. Its large field of view significantly increases the discovery rate, enabling more robust statistics. The leading discoveries have revealed a fraction of GAMMA-RAY BURSTs, while the rest remain unexplained. We propose a methodology to search for possible relations between gravitational waves (GWs) and FXTs, as it may serve as a discrepancy among proposed theoretical models. To achieve this, we intend to utilize X-Pipeline, an unmodeled search algorithm, to identify excess coherent signals in LIGO-Virgo-KAGRA (LVK) O4b observations. Out of 64 FXTs events, we obtained 19 FXTs for constructing robust searches. Given the absence of any detectable GW signals, we subsequently calculated upper limits and estimated exclusion distances for each source. In order to enrich the sample base and statistical analysis, this methodology could henceforth be conducted through future GW searches, including KAGRA in the O4c and O5 observations.
[abstract 43 / 45] (score: 2) - Title: Science-driven design and performance evaluation of a Silicon Laue Component lens for hard X-ray polarimetryAuthors: L. Abalo, N. M. Barrière, M. W. Beijersbergen,Comments: 6 pages. 2 figures. Submitted to Astronomy & AstrophysicsSubjects: astro-ph.IMCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Focusing hard X-rays above 80 keV is challenging for grazing-incidence optics. Laue lenses offer an alternative based on crystal diffraction. We assess a lens based on Silicon Laue Components (SiLCs), consisting of stacked silicon plates, for polarimetry of accreting stellar-mass BLACK HOLEs and strongly MAGNETized neutron stars in the 80-200 keV band. We derive effective-area requirements from the minimum detectable POLARIZATION at 99% confidence (MDP99) for an XL-Calibur-inspired polarimeter observing a 100-mCrab source for 100 ks. We evaluate an 18-m-focal-length lens combining Si(220) and Si(111) reflections, with a 63 arcsec diffraction bandpass and a 90% optical filling factor, using on-axis ray tracing of a perfectly aligned lens with uniform crystal curvatures. An MDP99 of 5% requires mean effective areas of approximately 260, 400, and 740 cm^2 in the 80-100, 100-130, and 130-200 keV bands, respectively. The lens spans radii of 356-1453 mm and continuously covers 80-200 keV. Its effective area reaches approximately 375 cm^2 near the low-energy boundary and falls to approximately 200 cm^2 at 180 keV. The focal-plane diameters enclosing 50% and 90% of the focused signal are 5.4 mm (62 arcsec) and 9.8 mm (112 arcsec). Mean effective areas of approximately 320, 250, and 220 cm^2 give reference MDP99 values of approximately 4.5%, 6.4%, and 9.5% in the three bands. The design reaches few-percent polarimetric sensitivity below 100 keV but does not maintain a 5% MDP99 across 80-200 keV under the adopted detector assumptions. It remains relevant for more strongly polarized hard components and provides a reference for end-to-end optimization of the optics, detector response, and background.
[abstract 44 / 45] (score: 2) - Title: Tandem JETs in crossflow: the enclosed-recirculation momentum exchange and the unsteady shear-layer dynamicsAuthors: Xunchen Liu,Comments:Subjects: physics.flu-dynCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Twin tandem JETs in crossflow are examined by 40\ kHz time-resolved particle image velocimetry (PIV) over nine spacing--velocity-ratio conditions ($L=2d$--$4d$, $r\approx3$--7; 68 twin cases, 11 single-JET records). The front JET is diluted: its trajectory lies below the single-JET reference, with a near-field segment up to 40\% shorter, and its velocity ratio falls to an effective value $r_{\mathrm{eff}}
[abstract 45 / 45] (score: 2) - Title: Coherent SYNCHROTRON radiation extraction from a bent beam pipeAuthors: Igor Zagorodnov, Dmitry Bazyl, Gennady Stupakov,Comments: 21 pages, 9 figuresSubjects: physics.acc-phCreated: 2026-10-22; Updated: 2026-10-23; Datestamp: 2026-10-23
Coherent SYNCHROTRON radiation generated in a bending MAGNET can propagate far downstream and heat the beam pipe. We investigate a beam-free side outlet that diverts part of this radiation into a separate guide. We use a paraxial equation to calculate radiation generation in the bend and its division between the two guides. Modal and finite-difference solutions are used in the bend, and quadratic finite elements on a changing transverse mesh in the branching region. We check the paraxial approximation against full-wave solutions at selected frequencies. Separately, we calculate radiation attenuation in a conducting pipe without an outlet using complex modes that satisfy impedance boundary conditions. For this example, independently damped perfectly conducting modes underestimate the high-frequency transmitted power. For a $70\times25$ mm rectangular chamber with a $30^\circ$ bend of radius 2.2 m and Gaussian bunches of rms length $10\,μ$m, the selected outlet diverts about 53\% of the total outgoing radiation power into the beam-free channel.
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