Current date: 2026-09-07
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Created/updated limit: 2026-08-31 (7 days ago)
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Scoring abstracts
Number of records retrieved: 684
Keyword score statistics
score 7 -- 2 abstracts
score 6 -- 2 abstracts
score 5 -- 2 abstracts
score 4 -- 1 abstracts
score 3 -- 2 abstracts
score 2 -- 17 abstracts
in total -- 26 abstracts
Articles that appeared on 2026-09-07
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[abstract 1 / 26] Wow! (score: 7)
- Title: Radiation GRMHD Models of Accretion onto Stellar-Mass Black Holes: III. Near-Eddington AccretionAuthors: Lizhong Zhang, James M. Stone, Shane W. Davis, Yan-Fei Jiang, Patrick D. Mullen, Christopher J. White,Comments: 29 pages, 24 figures, 3 tables, accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We present a comprehensive analysis of four near-Eddington BLACK HOLE accretion models from GRMHD simulations with full radiation transport. This study investigates the dynamical effects of MAGNETic field topology and BLACK HOLE spin using two representative choices of each. Two stable near-Eddington solutions emerge in these models: a thin thermal disk embedded within a MAGNETic envelope when sufficient net vertical MAGNETic flux is present (e.g., vertical field $\gtrsim 5\times10^5$ G at $20r_g$), and a MAGNETically elevated disk when the net vertical flux is weak or absent. One model initialized without net vertical flux evolves into the thin disk solution, as strong, anisotropic radiation feedback at high accretion rates promotes the accumulation of vertical MAGNETic flux in the inner disk. In the thin thermal disk, accretion is driven primarily by mean-field Maxwell stress and proceeds largely within the MAGNETic envelope, while heat dissipation is spatially decoupled and concentrated near the midplane. However, in the MAGNETically elevated disk, accretion occurs throughout the disk body and is comparably driven by mean-field and turbulent stresses; heat dissipation therefore occurs locally through turbulence. Radiation transport is diffusion-dominated, enabling efficient radiative cooling ($\sim$4-10%). An optically thin wind is launched from the disk surface by combined radiative and MAGNETic forces, with stronger winds found in models with larger vertical MAGNETic flux and higher spin. Both strong and weak JETs are produced: strong JETs are persistent, highly RELATIVISTIC, and MAGNETically driven, while weak JETs are intermittent, mildly RELATIVISTIC, and powered by a combination of MAGNETic and radiative forces.
[abstract 2 / 26] Wow! (score: 7) - Title: ElectroMAGNETic alignment and JET precession around supermassive BLACK HOLEs: Quasi-periodic oscillations in tidal disruption eventsAuthors: Pau Amaro-Seoane, Leif Lui, Alejandro Torres-Orjuela, Xian Chen,Comments: 7 pages, 3 figuresSubjects: astro-ph.HE gr-qcCreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We evaluate quasi-periodic oscillations and JET formation in tidal disruption events using the covariant formulation of electroMAGNETic angular-momentum transfer. General-RELATIVISTIC frame-dragging tears apart misaligned transient accretion flows, forming an isolated inner mini-disk. The accumulation of MAGNETic flux on the event horizon powers a RELATIVISTIC JET via the Blandford-Znajek mechanism. Because the MAGNETic field anchors to the precessing mini-disk, the JET axis rotates, generating geometric modulations in the observed X-ray and radio fluxes. To ensure physical consistency with the force-free MAGNETosphere required to launch a Blandford-Znajek JET, we model the electroMAGNETic back-reaction using a split-monopole MAGNETic field topology. By performing a small-spin expansion of the Noether current density over the event horizon, we derive a closed-form analytical reaction torque exerted by the electroMAGNETic field on the accretion plasma. We evaluate the resulting kinematics to show that the electroMAGNETic back-reaction induces a retrograde precession of the mini-disk, coupling with the prograde Lense-Thirring precession to dictate the global oscillation frequency. We formulate explicit predictions for observable transient signals and predict a monotonic attenuation of the peak-to-trough flux ratio as the mini-disk aligns, as well as a specific frequency drift signature characterized by an initial lengthening followed by an asymptotic shortening of the time interval between consecutive flares. We establish an analytical mechanism where MAGNETic flux depletion stalls alignment, predicting a constant residual modulation amplitude at late times. We formulate a methodology to extract the BLACK HOLE spin and the MAGNETic flux density directly from the temporal derivatives of this predicted frequency drift, operating independently of spectral continuum fitting.
[abstract 3 / 26] Yes (score: 6) - Title: Preferential accretion onto eccentric and unequal binary BLACK HOLEsAuthors: Stanislav DeLaurentiis, Zoltán Haiman, Magdalena Siwek,Comments:Subjects: astro-ph.HECreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
Supermassive binary BLACK HOLEs (SMBBHs) are expected to be surrounded by circumbinary disks (CBDs) which affect the binary through gravitational forces and accretion. It has been reported that the binary can experience ``preferential accretion'' where one BLACK HOLE (BH) out-accretes the other for hundreds of orbits, but this asymmetry has yet to be fully described or understood. In this work, we utilize a suite of 80 SMBBH hydrodynamical simulations with varying mass ratios ($q_b$) and eccentricity ($e_b$) in order to robustly delineate the behavior of preferential accretion, determine its relationship to the structure of the CBD, and study its observational consequences. We characterize the accretion-rate ratio $λ(t) \equiv \dot{M}_2(t)/\dot{M}_1(t)$ and the mass-ratio rate of change $\dot{q}_b \equiv d/dt(M_2/M_1)$ across the suite. We confirm that the secondary tends to out-accrete the primary ($λ\geq 1$), and find this preference to be strongest for low-$e_b$, low-$q_b$ binaries and increasingly time-variable toward high $e_b$. We also find that (i) the time-variability of $λ$ tracks the precession of the CBD, (ii) there can be sub- and super-Eddington accretion in a single binary, and (iii) the gas-driven approach toward equal mass becomes particularly slow for highly eccentric, high $q_b$ binaries, suggesting that some binaries may not reach $q_b=1$ within the $30\,\mathrm{Myr}$ lifetime of a QUASAR and therefore allowing LISA to constrain the accretion history of SMBBHs. Our findings also suggest that periodically flickering JETs are a potential observable signature of many binaries.
[abstract 4 / 26] Yes (score: 6) - Title: The October 2022 flare in OJ 287 and the mass of its primary BLACK HOLEAuthors: Mauri J. Valtonen, Staszek Zola, Manpreet Singh, Andrei V. Berdyugin, Kari Nilsson, A. Gopakumar, Alok C. Gupta, Tapio Pursimo, Alexandr E. Volvach, Marek Drozdz, Waldemar Ogloza, Rene Hudec, Martin Jel\'ınek, Jan Štrobl, Michal Zejmo, Stefano Ciprini, Daniel E. Reichart, Vladimir V. Kouprianov, Alberto Sadun, Markus Mugrauer, Katsura Matsumoto, Ryo Imazawa, Makoto Uemura, Lankeswar Dey,Comments: 21 pages, 10 figures, 1 tableSubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
The bright BLAZAR OJ~287 has demonstrated a sequence of flares, which are well explained by a quasi-Keplerian orbit model. The flares are associated with the impact of the secondary on the accretion disk of the primary. The orbit must precess in order to produce the correct sequence of flares, and from the precession rate we calculate the mass of the primary. This precession rate gives the mass of the primary $M_{BH} = (18.35\pm0.05) \times 10^9 M_{\odot}$. Two kinds of flares have been identified: direct flares from the impacts, and tidal flares arising from an increased accretion flow into the JET. The precession rate and the primary BLACK HOLE mass may be independently determined from both sets of flares; the tidal flare of October 2022 was recommended for an intense campaign for this reason. This paper describes these observations over a wide spectral range. We show that the October 2022 flare fits the expectations for a tidal flare and thus supports the earlier determination of the mass of the binary BLACK HOLE system in OJ 287. The mass of the primary may also be deduced from secondary indicators such as the correlation with the hydrogen line strength and the BLACK HOLE mass. These studies require that the mass is above $M_{BH} \sim 10^{10} M_{\odot}$, but do not specify the value more exactly.
[abstract 5 / 26] Yes (score: 5) - Title: Super-Eddington Accretion and Early-Stage Feedback in Ton S180Authors: Pierpaolo Condò, Giacomo Venturi, Eleonora Parlanti, Marco Berton, Enrico Congiu, Alessia Tortosa, Stefano Carniani, Francesco Tombesi, Tommaso Zana, Claudio Ricci, Ezequiel Treister, Luis C. Ho, Enrico Piconcelli, Miguel Coloma Puga, Emilia Järvelä, Luca Crepaldi, Amelia Vietri, Benedetta Dalla Barba,Comments: 15 pages (main text), 8 figures. Accepted for publication in A&A (1 September 2026)Subjects: astro-ph.GA astro-ph.HECreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
Narrow-line Seyfert 1 (NLSy1) galaxies are key laboratories for studying rapid supermassive BLACK HOLE (SMBH) growth and ACTIVE GALACTIC NUCLEus (AGN) feedback at high accretion rates. We investigate the nearby NLSy1 Ton S180 with VLT-MUSE optical integral field spectroscopy to connect its nuclear accretion properties with the spatially resolved ionized gas and host-galaxy kinematics. We modeled the unresolved nuclear spectrum and applied a custom point spread function subtraction to recover the host-galaxy emission on kiloparsec scales. The nuclear spectrum requires a complex permitted-line decomposition and a blueshifted [O III] outflow component. Single-epoch estimators and the stellar velocity dispersion imply BLACK HOLE masses in the range $\log(M_{\rm BH}/M_\odot) = 6.5 - 7.7$. Combined with the observed luminosity, this implies a dimensionless mass accretion rate of $\dot{M} / \dot{M}_{\rm Edd} = 4.1 - 980$, confirming the extreme accretion regime. The host galaxy shows a circumnuclear ring, an inner elongated structure consistent with a bar, and rotation-dominated gas and stellar kinematics. Simple inflow models do not significantly better reproduce the observed velocity field. We detect a resolved ionized outflow extending about 2 kpc west of the nucleus, with mildly blueshifted velocities (with a maximum of $v_{\rm max} \sim 340$ km s$^{-1}$). Its mass outflow rate is only $\sim 4.2 \times 10^{-4}\,M_\odot\,\mathrm{yr}^{-1}$, whereas the unresolved nuclear outflow reaches $v_{\rm max} \sim 1140$ km s$^{-1}$ and $\dot{M}_{\rm out} > 1.5\,M_\odot\,\mathrm{yr}^{-1}$. This contrast may reflect either weak ionized coupling from nuclear to galactic scales or different episodes of AGN activity over time. These results show that Ton S180 is undergoing rapid SMBH growth, while the observed ionized outflow remains confined to the inner few kiloparsecs and is weak on host-galaxy scales.
[abstract 6 / 26] Yes (score: 5) - Title: The angular structure of the GW170817 JET from prompt emission aloneAuthors: R. Moradi, R. Ruffini,Comments: 11 pages, 4 figures, including Supplemental MaterialSubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We determine the angular structure of the GW170817 JET by the prompt emission alone, without afterglow fitting, circumburst density or microphysical parameters. We assume that GRB 090510 and GW170817 have outflows of the same kind, observed respectively on-axis and at the interferometric viewing angle of $20^\circ$. We support this assumption with independent gravitational-wave data showing compatible binary masses and radiated energies. We show that for an observer whose beaming cone is filled with outflow, the point-source Doppler scalings do not apply: $E_{\rm iso}=4πε(θ_v)$, with $ε$ the energy radiated per unit solid angle along the line of sight, while the peak energy follows $E_{\rm p,i}\proptoΓ(θ_v)$. We obtain $n={\rm d}\lnε/{\rm d}\lnΓ= 3.76\pm0.29$ from the ratio of the two bursts, with no free parameter and no assumed angle. This excludes four structures in common use at $4.7σ$ to $13σ$; three remain above $4σ$ across the full reported range of the peak energy of the GW170817 JET. Two prompt spectra fix no angular scale; supplying it with the core Lorentz factor of GRB 090510 and the viewing angle gives $ε\proptoθ^{-7.4}$ outside a core of $2^\circ$--$5^\circ$, in agreement with the width inferred from $367$ short bursts, the outflow remaining RELATIVISTIC at $Γ=33$ on the line of sight. The exponent exceeds what the Lorentz boost of a uniform comoving flow can produce, so the structure is intrinsic to the outflow and not a consequence of the boost. The same structure fixes the emission radius, which contributes $0.41$~s of the $1.74$~s delay between the gravitational-wave signal and the gamma-rays, the remainder being the launch and breakout of the JET, with no free parameters. We conclude that the faintness lies in the structure of the GW170817 JET, not in the de-beaming of a bright core.
[abstract 7 / 26] 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. Accepted for publication in A&ASubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
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 8 / 26] (score: 3) - Title: Leveling of MHD turbulence imbalance in shear flowsAuthors: M. Kavtaradze, G. Mamatsashvili, G. Chagelishvili, E. Uchava,Comments: 12 pages, 6 figures, accepted for publication in Physical Review ESubjects: physics.space-ph astro-ph.SR physics.flu-dyn physics.plasm-phCreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
We investigate MAGNETohydrodynamic (MHD) turbulence in plane shear flows with a streamwise background MAGNETic field in the super-Alfvénic regime, i.e., when the flow velocity is larger than the local Alfvén speed. In this regime, turbulence is energetically supplied by large-scale shear of the flow via transient, or non-modal amplification of Alfvén waves, which are the building blocks of MHD turbulence, and streamwise-uniform, mostly nonMAGNETic modes. We show that shear reduces turbulence imbalance, driving the system toward a balanced state -- the energies of counter-propagating Alfvén waves become essentially equal, even for an initially perfectly imbalanced Alfvénic turbulence. This balancing occurs due to the shear-induced linear non-modal dynamics of Alfvén waves -- their non-modal growth, resulting in over-reflection, and coupling between counter-propagating wave branches. Because of its linear origin, this process of balancing of MHD turbulence by shear is fundamentally different from the nonlinear processes operating in standard MHD turbulence in the absence of a mean shear flow. It can have direct implications for understanding the balanced/imbalanced nature of MHD turbulence in shear regions of the solar wind.
[abstract 9 / 26] (score: 3) - Title: Nonstationary Stochastic Timing Signatures in the Prompt Gamma-Ray Light Curve of GRB 170817AAuthors: Lin Xie, Dahai Yan,Comments: 29 pages, 5 figures, 4 tables. Submitted to Journal of High Energy AstrophysicsSubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We investigate time-dependent stochastic structure in the weak prompt gamma-ray emission of GRB 170817A using change-point and deep-kernel Gaussian-process (GP) models. The analysis is based on the 10-300 keV FERMI/GBM light curve with 0.10 s time resolution. Two change-point configurations identify similar covariance transitions at 0.269 and 0.237 s after the gravitational-wave merger, with 10-90% transition widths of 0.441 and 0.393 s, respectively. At the representative gate-defined boundary of t_tr = 0.27 s, all four fixed-split assignments yield positive evidence gains over the full-exposure stationary Matern-3/2 reference. The largest gain is Delta ln Z_split = 5.72 +/- 0.16 for the Matern-3/2 to Matern-3/2 assignment, while the gate-matched damped random walk (DRW) to Matern-3/2 assignment gives Delta ln Z_split = 5.50 +/- 0.16. The fixed-split comparison therefore supports segment-specific covariance evolution without requiring a change of covariance family. The deep-kernel models recover localized time-deformation features peaking at 1.65 and 1.75 s after the merger for DRW and Matern-3/2 base kernels, respectively. Their offsets from the adopted gamma-ray onset at 1.74 s are -0.09 and +0.01 s, both within the 0.10 s sampling resolution. The full-band timing features remain stable when the bin width is changed from 0.10 to 0.12 s, whereas energy subdivision produces larger shifts in gate locations than in warp peaks. Residual diagnostics show that the models reproduce the dominant temporal structure, although localized residual dependence remains. We interpret the gate-defined covariance transition and the localized time-deformation feature as model-dependent phenomenological timing diagnostics. Further simulation calibration and count-level modelling are needed to assess the statistical robustness and physical origin of the recovered nonstationary structure.
[abstract 10 / 26] (score: 2) - Title: ODIN: Confirmation and 3D Reconstruction of Six Massive Protoclusters at Cosmic NoonAuthors: Ashley Ortiz, Vandana Ramakrishnan, Kyoung-Soo Lee, Arjun Dey, Yucheng Guo, Ethan Pinarski, Anand Raichoor, Francisco Valdes, J. Aguilar, Steven Ahlen, Maria Celeste Artale, Davide Bianchi, August Bliese, David Brooks, Rebecca Canning, Maria Cerdosino, Todd Claybaugh, Andrei Cuceu, Axel de la Macorra, Peter Doel, Jaime Forero, Eric Gawiser, Enrique Gaztanaga, Satya Gontcho, Caryl Gronwall, Lucia Guaita, Gaston Gutierrez, Hiram K. Herrera-Alcantar, Ho Seong Hwang, Woong-Seob Jeong, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Ankit Kumar, Ofer Lahav, Martin Landriau, Jaehyun Lee, Seong-Kook Lee, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, Byeongha Moon, John Moustakas, Adam Myers, Seshadri Nadathur, Nathalie Palanque-Delabrouille, Changbom Park, Will Percival, Ignasi Perez-Rafols, Francisco Prada, Eshwar Puvvada, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, Hyunmi Song, David Sprayberry, Gregory Tarle, Paulina Troncoso, Ana Sofia Uzsoy, Benjamin Weaver, Yujin Yang, Rongpu Zhou, Hu Zou,Comments:Subjects: astro-ph.GACreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
Protoclusters represent sites of accelerated galaxy formation and extreme astrophysical activity characteristic of dense environments. Identifying massive protoclusters and mapping their spatial structures are therefore crucial first steps in understanding how the large-scale environment influences galaxy evolution. We combine wide-field Ly$α$ imaging from the ODIN survey with extensive DESI and ancillary spectroscopy across the extended COSMOS and XMM-LSS fields ($\approx$14 deg$^2$) to search for massive protoclusters. We confirm six systems at $z\approx 2.4$ and $z\approx 3.1$, reconstruct their three-dimensional structures, estimate descendant halo masses, and, for one structure at $z\approx 3.12$, demonstrate that overlapping narrowband filters ($NB497$ and $N501$) provide accurate redshift tomography for emission-line galaxies. One protocluster at $z\approx 2.45$ overlaps with one of the LATIS tomographic fields, enabling direct comparison between galaxy and H {\sc i} overdensities traced by Ly$α$ forest absorption. Another at $z\approx 3.12$ hosts a massive quiescent galaxy ($M_{\ast} \approx 1.2 \times 10^{11}M_\odot$), indicating early quenching in a dense environment. By comparing Ly$α$ emission properties across environments, we find that protocluster galaxies exhibit higher median line fluxes and a deficit of faint emitters relative to the field. The effect is strongest when both 2D and 3D density information are combined, indicating that galaxies in the densest protocluster cores are most affected by environmental processes. This effect is stronger at $z\approx3.1$ than at $z\approx2.4$, suggesting possible redshift evolution.
[abstract 11 / 26] (score: 2) - Title: Energetic particles, Shafranov shift and finite $β$ effects on TAE, KBM and ITG instabilities in global electroMAGNETic gyrokinetic simulationsAuthors: B. Rofman, G. Di Giannatale, A. Mishchenko, E. Lanti, A. Bottino, T. Hayward-Schneider, J. N. Sama, A. Biancalani, B. F. McMillan, S. Brunner, L. Villard,Comments:Subjects: physics.plasm-phCreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
Burning plasma is computationally challenging to simulate due to the multi-scale interactions between energetic particles (EPs), Alfven eigenmodes, and microinstabilities that drive turbulence. Many studies circumvent this difficulty by focusing on a single instability and making the corresponding simplifying assumptions. However, these approximations do not necessarily preserve the global instability spectrum, leading to conflicting results and inconsistencies. In this work, we identify the minimal set of assumptions needed to model a burning plasma self-consistently with the modes and species in the system. Using the global gyrokinetic code ORB5, to systematically evaluate the impact of commonly adopted assumptions on the plasma response. We find it is essential to include Shafranov shift and finite $β$ effects from all MAGNETically confined species. Otherwise, unphysical electroMAGNETic modes like internal kinks and kinetic ballooning modes (KBMs) appear to dominate the instability spectrum. The EP contribution to the Shafranov shift is particularly important, stabilizing both the toroidal ion temperature gradient (ITG) and toroidal Alfven eigenmode (TAE) at the longer wavelengths (low toroidal mode numbers). For TAEs, these effects significantly reduce the linear growth rate, which saturates instead of proportionally increasing with EP fraction. In the nonlinear regime ITG-driven heat and particle fluxes are unaffected by the Shafranov shift in self-consistent MAGNETic equilibria. While the the nonlinear saturation level of the TAE remains unchanged across all cases, unlike for the ITG case Shafranov shift does reduce the TAE-driven EP fluxes.
[abstract 12 / 26] (score: 2) - Title: Dependences of radio pulsar parameters on the kick velocityAuthors: Anton D. Lazarev, Sergei B. Popov,Comments: 12 pages, 12 figures. Published to the Open Journal of Astrophysics. Abstract abridgedSubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
According to several studies, analysis of observational data and theoretical modeling favor a bimodal distribution of the natal velocity kick of neutron stars. We analyze this proposal by using available data on radio pulsars. For $\sim200$ normal isolated radio pulsars with well-measured spin and kinematic parameters, we determine if they belong to the low- or high-velocity mode of such a distribution by applying the parametrization proposed by Igoshev (2020). Our results demonstrate that about $23\%$ belong to the low-velocity mode. We then analyze the differences in the properties of the two sets of pulsars belonging to the two modes. For some parameters (characteristic ages and distances), we see a clear difference between the two modes. However, for these quantities, it can be attributed to selection bias. For those parameters that are not subject to strong selection, such as pulse width, we do not observe any difference. Interestingly, we detect a notable difference in the MAGNETic field distribution between the two modes. Lower-field pulsars ($B\lesssim 10^{12}$~G) are overabundant among objects from the low-velocity mode. Among pulsars with low fields ($\lesssim 10^{11}$~G), we do not identify any objects from the high-velocity mode of the kick distribution. The origin of this discrepancy is not clear, and we discuss several possibilities. Our analysis demonstrates that, most probably, this feature can be explained by selection effects. Thus, we conclude that there is no robust bimodality in physical parameters of radio pulsars that can be related to the proposed bimodality of the kick velocity. This can be considered as an indirect argument against the hypothetical bimodality in the NS kick distribution. (abridged)
[abstract 13 / 26] (score: 2) - Title: Complex Lags from Simple PhysicsAuthors: Benjamin Ricketts, Gregoire Marcel,Comments: 17 pages, 25 figures, accepted to A&ASubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
X-ray timing information produced through Fourier analysis from the variable emission of BLACK HOLE X-ray binaries has been used for several decades to provide key insights into the physical setup of these systems not measurable with spectroscopy. In particular, quasi-periodic oscillations within these systems have been of particular interest and remain the source of great debate on how they come about. We investigate the timing products of simple toy models of QPO variability to provide more intuition when thinking about signals produced by these sources. We simulate simple physical setups and show how phase lags and coherence of the signals change in these different setups. We first focus on properties of QPO like signals under a single driving signal assumption. We then investigate the case of multiple oscillations in a signal. Finally, we investigate how timing products change when QPOs are produced by time dependent modulation of periodic signals. Many simple physical setups with common driving signals are able to reproduce complex non-linear phase lags that resemble those present in the data. The changes in physical setup aligns with experience in the data, such as differing power spectra but fall short of reproducing the data as expected. Multiple incoherent processes present in the signal struggle to reproduce behaviour present in the data. Coherence seems to be a more useful tool for differentiating between setups. Fourier analysis with complicated data like that produced by X-ray binaries can lead one to be tempted to invoke exotic lag mechanisms without the appropriate framing. This paper attempts to help provide tools and intuition as to how different phenomena in signals (particularly relating to QPOs) can result in non-linear phase lags with explicit structure.
[abstract 14 / 26] (score: 2) - Title: Energy deposited by BLACK HOLEs in the hot X-ray gas of elliptical galaxies, groups and clustersAuthors: A. Cattaneo, S. Ettori,Comments: 13 pages (+4 pages of Appendix); accepted for publication in A&ASubjects: astro-ph.CO astro-ph.GACreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
Galaxy groups show entropy excesses $ΔS$ with respect to theoretical expectations from models and simulations with purely gravitational heating. We determine the heat $Q_{\rm heat}\simeq TΔS$ deposited by non-gravitational sources into the hot gas of elliptical galaxies, groups and clusters, and to compare it with the energy output of their central BLACK HOLEs (BHs). We adopt a simple model for the hot gas with only one free parameter: the core entropy. We calibrate the core entropy on the observed relation between X-ray luminosity and halo mass, and we use it to determine the entropy $S$ of the hot gas. We determine $ΔS=S-S_0$ by taking the difference between $S$ and the entropy $S_0$ found in cosmological adiabatic simulations for haloes of the same mass. The temperature $T$ of the hot gas during the heating phase is determined from semi-analytic/semi-empirical modelling by assuming that heat absorption traces the accretion histories of supermassive BHs. Our findings suggest that supermassive BHs thermalise 1 to $3\%$ of their energy output in the surrounding gas. Our results suggest two regimes: (i) in elliptical galaxies and groups, ACTIVE GALACTIC NUCLEi (AGN) heat the gas much more rapidly than it can cool, generating the observed entropy excesses and quenching STAR FORMATION when the accumulated heat is large enough to unbind the gas reservoir in the host halo; (ii) in galaxy clusters (at $M_{200}>10^{14}{\rm\,M}_\odot$), heating and cooling are in self-regulated equilibrium.
[abstract 15 / 26] (score: 2) - Title: Strong Constraints on Line Signals from Dark Matter Annihilation in a Nearby SubhaloAuthors: Asier Salces Pérez, Thong T. Q. Nguyen, Pedro De la Torre Luque, Tim Linden,Comments: 10 pages, 9 figuresSubjects: hep-ph astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We present a dedicated search for monochromatic gamma-ray emission from a recently proposed nearby DARK MATTER subhalo candidate. Using nearly 15 years of FERMI-LAT Pass 8 data, we perform a sliding-window search for gamma-ray lines between 10 and 300 GeV. We do not find any statistically significant evidence for a line signal. The largest excess occurs at $E_γ\simeq 28 \, {\rm GeV}$ with a local significance of $2.5σ$. We therefore derive 95% confidence level upper limits on the annihilation cross section for $χχ\rightarrow γγ$. Under the assumed NFW subhalo model, the resulting constraints are stronger than existing Galactic Center line limits over much of the explored mass range. We further translate these line constraints into bounds on well-motivated WIMP models, such as Higgs-portal and Wino DARK MATTER scenarios, restricting previously open parameter regions consistent with thermal freeze-out as well as models associated with DARK MATTER interpretations of the Galactic Center Excess.
[abstract 16 / 26] (score: 2) - Title: A SWIFT X-ray view of the SMS4 sample - III: Deeper insight into previously undetected sourcesAuthors: Alessandro Maselli, William R. Forman, Christine Jones, Ralph P. Kraft, Matteo Perri,Comments: 14 pages, 3 figures, 8 tables; accepted for publication in the Astrophysical Journal Supplement SeriesSubjects: astro-ph.HECreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
We update the X-ray information given in Maselli et al. (2024) for five bright radio sources in the SMS4 catalog, thanks to additional observations with the X-Ray Telescope (XRT) on board the Neil Gehrels SWIFT Observatory (hereafter SWIFT) carried out through February 2026. X-ray emission from MRC B1754-597, previously based only on data from the eROSITA-DE DR1 catalogs, is now detected also by SWIFT, which yields a more precise positional uncertainty. Thanks to ~7 ks of additional exposure with SWIFT we are now able to detect MRC B1817-391, a source for which no X-ray counterpart is found in eROSITA-DE DR1. Another source that is not detected in the eROSITA-DE DR1 catalogs, and that was not observed by SWIFT earlier than 2025, is MRC B1827-360: with a ~6 ks X-ray observation, the source is detected. Finally, based on ~8 ks of additional exposure, we detect X-ray emission for MRC B2032-350, a source that lies out of the DR1 footprint. In contrast, additional exposure (~2 ks) just gives an upper limit on the X-ray emission of MRC B1814-519. The analysis of the extent and the hardness ratio of the four detected X-ray sources suggests the presence of soft, diffuse X-ray emission as expected from galaxy group cores or hot galaxy coronae. Using the positional uncertainty of the X-ray detections to constrain the search for counterparts at lower energies, we provide a new infrared/optical counterpart for MRC B1817-391 and confirm the counterparts previously reported in the literature for the three remaining sources.
[abstract 17 / 26] (score: 2) - Title: AGN-DB: A Unified Multi-Wavelength Database of Active Galactic NucleiAuthors: Alessandro Peca, Nico Cappelluti, C. Megan Urry, Zhongtian Hu, Jerry R. Bonnell, Jack McKeown, Giulia Cerini, Xulei Sun, Fabio Pacucci, Tracey Jane Turner, Peter G. Boorman, Aritra Ghosh, Connor Auge, Rebeka L. Böttger, Adi Foord, Massimiliano Galeazzi, Jeyhan S. Kartaltepe, Iver Warburton Kilmarrin, Allison Kirkpatrick, Michael J. Koss, Stephanie LaMassa, Md Mahmudunnobe, Stefano Marchesi, Lea Marcotulli, Isaac Moskowitz, Priyamvada Natarajan, Mitsunori Ogihara, Meredith Powell, David Sanders, Dominic Sicilian, Chuan Tian, Ezequiel Treister,Comments: Submitted to ApJ. Comments and inputs from the community are very welcome!Subjects: astro-ph.GA astro-ph.HECreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
We present the Active Galactic Nuclei Database (AGN-DB), a comprehensive, multi-wavelength catalog compiled from more than 100 publicly available AGN catalogs and samples released by the end of 2025, spanning radio to $γ$-ray wavelengths. The database contains approximately 8.1 million unique sources, approximately 7.8 million of which remain after flagging stellar contaminants, and approximately 6.8 million of these are classified as AGN. Source cross-matching across catalogs is performed using Lyra, a Bayesian likelihood-ratio framework that jointly considers positional uncertainties, source densities, and photometric information to compute posterior match probabilities. The resulting catalog provides astrometric coordinates, redshifts, photometry, and classifications for each unique source. All multi-catalog provenance is preserved. For every property, we store the full array of values and originating catalog identifiers, enabling multi-epoch and multi-survey analyses. In this paper, we describe the AGN-DB pipeline, including the cross-matching methodology, and present the statistical properties of the v1.0 catalog. AGN-DB is designed to enable population studies, spectral energy distribution modeling, AGN classification, and variability analyses at an unprecedented scale. Its pipeline is designed to facilitate the integration of new catalogs, allowing AGN-DB to be updated regularly, with releases planned at least annually.
[abstract 18 / 26] (score: 2) - Title: Waveform models for the gravitational-wave memory effect: III. Phenomenological frequency-domain model for nonspinning binariesAuthors: Arwa Elhashash, David A. Nichols,Comments:Subjects: gr-qc astro-ph.HECreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
We present a phenomenological frequency-domain model for the gravitational-wave (GW) memory signal from nonspinning binary-black-hole mergers on quasicircular orbits. We develop separate amplitude and phase models for the dominant $(l,m)=(2,0)$ spherical-harmonic mode of the GW memory signal. The amplitude and phase models are built from superpositions of elementary and transcendental functions, which can be evaluated efficiently. Both portions of the model are calibrated against a numerical-relativity surrogate model over mass ratios from one to eight. Their accuracy is assessed by computing their mismatch with the numerical-relativity models using the Advanced LIGO sensitivity curve from the fourth observing run. The mismatches are of the order $10^{-4}\unicode{x2013}10^{-3}$ over the parameter space of total mass covered by LIGO. The resulting frequency-domain model is a more computationally efficient waveform model for the GW memory signal than a related time-domain model earlier produced by the authors. An open-access implementation of both the time-domain and frequency-domain models is provided in the Python package GWMemoryModel, which can be used for relevant analyses of nonspinning binary BLACK HOLEs.
[abstract 19 / 26] (score: 2) - Title: Screened Scalar Hair and the Weak-Lensing Separation of Black Holes from Neutron Stars in Quadratic $f(R)$ GravityAuthors: Yashmitha Kumaran, Ilídio Lopes,Comments: 9 pages, 4 figuresSubjects: gr-qcCreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
Quadratic $f(R)$ gravity carries a massive scalar degree of freedom, the scalaron, whose finite range $λ$ screens its influence on the geometry outside a compact object. We show that this screening severs the exterior of a BLACK HOLE from that of a neutron star of the same mass. The correction to the Schwarzschild metric is Yukawa-suppressed, falling as $e^{-r/λ}$ instead of polynomially in the coupling, and is thus invisible to any expansion in powers of that coupling; also, the exterior is intrinsically isotropic, so that inverting the temporal potential alone, as in single-potential solutions, fails to solve ]field equations. Applying the Gauss-Bonnet theorem to this geometry, we find the leading deflection angle to be exactly the general-RELATIVISTIC $4GM/b$, the scalaron contributions cancelling identically in the combination that bends light. The first correction carries the unfamiliar signature $λ^{-1/2}b^{-3/2}e^{-b/λ}$, screened beyond the scalaron range and confirmed against direct quadrature to around 20% at $b=4λ$, improving to 7% at $b=12λ$. What survives is not a difference of degree but of kind. The three ingredients that deliver it, non-analyticity in the coupling, the intrinsically isotropic gauge and the pressure-weighted scalar charge, are here obtained within a single, self-consistent derivation for the first time. A static BLACK HOLE carries no scalar hair, and lenses precisely as GR requires; a neutron star acquires a scalar charge weighted by the pressure supporting it against collapse, and does not. Weak lensing hence closes as a discriminant of the theory, whilst the horizon, as against a material surface, remains one in principle. The observational advantage lies not in bending angles at large $b$ but in the strong-field imaging of the photon sphere, and in the stellar interior, where the scalar charge is fixed by EoS.
[abstract 20 / 26] (score: 2) - Title: Exact solution of the Klein-Gordon equation in a Kiselev BLACK HOLE backgroundAuthors: Matheus. D. de Oliveira, Alexandre G. M. Schmidt,Comments: The manuscript has 20 pages and 2 figuresSubjects: gr-qcCreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
In this work, we investigate exactly the dynamics of a RELATIVISTIC spinless particle influenced by a static and uncharged BLACK HOLE surrounded by a quintessence-like anisotropic fluid or Kiselev BLACK HOLE. Considering two quintessence-like models as examples, we calculate the radial wave function and determine, in both cases, the quasispectrum of energy, as well as the Hawking radiation and temperature. We find that the stronger the influence of quintessence-like anisotropic fluid, the smaller the radiation observed outside the event horizon. Furthermore, the temperatures obtained in both cases are directly influenced by the quintessence-like anisotropic fluid, and we recover the values obtained in other contexts, such as those derived using the surface gravity. Finally, in the absence of quintessence, we recover in both cases the Hawking temperature $T_{H} = 1/(8πk_{B} M)$ corresponding to the Schwarzschild BLACK HOLE.
[abstract 21 / 26] (score: 2) - Title: Assessing the effect of error field penetration during plasma current ramp-up in the DIII-D tokamakAuthors: C. F. B. Zimmermann, E. M. Bursch, C. Paz-Soldan, J. M. Hanson, N. Leuthold, N. C. Logan, A. O. Nelson,Comments:Subjects: physics.plasm-phCreated: 2026-09-03; Updated: 2026-09-07; Datestamp: 2026-09-07
This work provides evidence that established error field penetration threshold scalings remain applicable during plasma current ramp-up. In dedicated DIII-D experiments with imposed $n=1$ perturbations during extended $I_p$ ramps, an apparent empirical threshold is found between $2$ and $3$~kA of applied 3D coil current, above which MHD modes are seeded. The imposed perturbation couples to the rational surfaces present during the ramp, seeding near the $q=4$ surface and penetrating as an $m/n=3/1$ mode by the end of the perturbation phase. To interpret these observations, multi-machine penetration threshold scalings are combined with equilibrium-based overlap metrics from the GPEC code, including the in-situ error fields of the device. This modeling reproduces the observed onset in the amplitude scan and classifies mode seeding across a database of 12 ramp-up discharges spanning a range of plasma currents and densities. Across this database, the seeding appears to be controlled primarily by the applied 3D coil current rather than by the plasma current or its ramp rate. Accounting for the in-situ error fields is found to be important for reliable prediction. These results are consistent with the robustness of scaling-based penetration metrics when coupled to detailed 3D field modeling under transient ramp-up conditions, and suggest the importance of accounting for in-situ error fields when assessing additional externally induced perturbations. This work is motivated by future tokamaks in which transient, non-axisymmetric error fields can arise during startup, for example from runaway electron mitigation coils.
[abstract 22 / 26] (score: 2) - Title: Evidence of Orbital Evolution of Gigahertz-Peaked Spectra in Binary Millisecond PulsarAuthors: Rahul Sharan, Bhaswati Bhattacharyya,Comments: Accepted in The Astrophysical Journal (ApJ)Subjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We present the first systematic investigation of the continuous orbital evolution of the Gigahertz-Peaked Spectum turnover frequency ($ν_{peak}$) in the binary millisecond pulsar, PSR J2144$-$5237. Using approximately 50 hours of densely sampled observations spanning the $\sim10$-day orbit with the Parkes Ultra-Wideband Low frequency receiver, we obtained continuous frequency coverage from 704 MHz to 4 GHz, enabling robust measurements of the spectral evolution throughout the binary orbit. We detect a clear and systematic modulation of the turnover frequency with orbital phase for both the $1^{st}$ pulse and $2^{nd}$ pulse components, with both emission components exhibiting remarkably similar evolutionary trends despite originating from distinct emission regions within the pulsar MAGNETosphere. The correlated evolution of the two pulse components strongly suggests that the observed spectral variability is governed by propagation through the intra-binary environment. The large orbital modulation of turnover frequency can be explained by cyclotron resonance absorption in MAGNETized plasma associated with the companion, while alternative absorption mechanisms are unable to reproduce the observed behaviour. Modelling the orbital evolution of the turnover frequency within the cyclotron absorption framework, can constrain the electron density distribution in the pulsar wind, estimate the MAGNETic field strength of the companion, and place limits on the geometry of the absorbing plasma and the binary system. This study establish orbital evolution of the Gigahertz Peaked Spectum as a powerful new diagnostic of the MAGNETized intra-binary medium and provide a hitherto unexplored probe of pulsar wind-companion interactions in eclipsing millisecond pulsar binaries.
[abstract 23 / 26] (score: 2) - Title: Through a glass, darkly: a combined framework for estimating fast radio burst host galaxy and population properties in an era of uncertain host identificationAuthors: C. W. James, B. C. Andersen, L. Marnoch, J. L. Hoffmann, N. Loudas, J. X. Prochaska, S. D. Ryder, M. Woodland,Comments: 23 pages, 16 figures, 2 tables. Submitted to PASASubjects: astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
The identification of fast radio burst (FRB) host galaxies, and subsequently their redshifts ($z$), has allowed the FRB dispersion measure (DM) to be used to probe the cosmological distribution of ionised gas, and study the properties of the FRB population itself. However, current methods cannot account for FRBs with uncertain host galaxy associations, leading to underutilisation of data, and potential biases towards nearby, bright hosts. In this work, we develop a methodology which can. We do so by combining three ingredients - the zDM code, for modelling the Macquart relation; PATH, for statistical host galaxy identification; and a set of models able to describe the intrinsic FRB host galaxy distribution - into a single formalism. We prove the fidelity of our formalism by using a synthetic set of FRB observations, with simulated hosts sampled from galaxy catalogues, and show that it reproduces intrinsic host galaxy properties even for FRB localisation uncertainties of 30", where a traditional PATH analysis produces no confidant host associations. When applied to a sample of FRBs localised by the Australian Square Kilometre Array Pathfinder, we confirm previous results showing that FRBs prefer host galaxies fainter than that predicted by star-formation, consistent with an exponential surface density scaling as $0.41^{+0.13}_{-0.09}$ times the half-light radius. We encourage the application of this formalism to data-sets from other FRB-hunting instruments.
[abstract 24 / 26] (score: 2) - Title: Can isolated binaries form unequal-mass binary black-hole mergers with a high-spin primary BLACK HOLE?Authors: Xiao-Tian Xu, Dong Lai, Bin Liu,Comments: submittedSubjects: astro-ph.SR astro-ph.GA astro-ph.HECreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
GWTC-5 has revealed a subpopulation of merging binary BLACK HOLEs (BBHs) with a high-spin primary BLACK HOLE (BH) and possibly unequal BH masses. GW241110 additionally exhibits a large spin-orbit misalignment, which suggests a hierarchical-merger origin. However, other formation scenarios are possible or even likely, especially for events without constraints on spin-orbit misalignment. As an alternative to hierarchical mergers, we investigate whether binary evolution can produce unequal-mass BBH mergers with a high-spin primary BH. Rather than performing comprehensive population-synthesis calculations, we examine the evolutionary pathways of forming merging BBHs and assess their uncertainties. We identify two possible pathways for producing unequal-mass BBHs with a high-spin primary. In initially wide binaries, mass-ratio reversal can make the tidally spun-up second-born BH both more massive and more rapidly rotating than the first-born BH; alternatively, in an initially close, unequal-mass binary, the primary star may evolve chemically homogeneously, while the secondary star evolves normally, producing a high-spin first-born BH that is more massive than its companion. Generally, large spin-orbit misalignment can be produced by large natal kicks or tertiary-induced nodal precession and/or Zeipel-Lidov-Kozai oscillations. We conclude that hierarchical mergers are not uniquely required to produce unequal-mass BBHs with a high-spin primary BH, although each isolated-binary pathway faces important theoretical constraints. Future detections of more merger events with primary BH spins around 0.7 would discriminate between binary evolution and hierarchical merger origin.
[abstract 25 / 26] (score: 2) - Title: PPN--spin degeneracies in mock S62-like stellar-orbit inferenceAuthors: Shant Khlghatyan,Comments: 21 pages, 15 figuresSubjects: astro-ph.GACreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We investigate the degeneracies between BLACK HOLE (BH) spin effects and parametrized post-Newtonian (PPN) parameters in the RELATIVISTIC orbital dynamics of S2-like and S62-like stars orbiting Sagittarius A$^{\ast}$. Using a 1PN+SO Hamiltonian framework and synthetic astrometric and radial velocity datasets, we perform Bayesian parameter inference. For current baseline observational precisions, the dominant RELATIVISTIC observable--the Schwarzschild periapsis advance--allows the recovery of the effective precession parameter $Υ$, while leaving the individual PPN parameters $γ$ and $β$ degenerate. Assuming microarcsecond-level astrometric precision, the spin-induced Lense-Thirring signal becomes partially detectable; fixing the PPN sector to General Relativity allows the BH spin magnitude to be constrained to an uncertainty of $\sim10^{-2}$. However, simultaneously varying PPN and spin parameters reveals a strong, approximately linear covariance between $Υ$ and the dimensionless spin parameter $χ$. To overcome this limitation, we demonstrate that joint multi-star inference can disentangle the degeneracy by combining a wider-orbit star, which constrains the dominant 1PN sector, with a compact RELATIVISTIC orbit that is sensitive to Lense-Thirring frame dragging.
[abstract 26 / 26] (score: 2) - Title: Energy Partitioning at the Termination ShockAuthors: Judit Szente, Bart van der Holst, Gabor Toth, Merav Opher,Comments:Subjects: astro-ph.SRCreated: 2026-09-04; Updated: 2026-09-07; Datestamp: 2026-09-07
We show new results of a global 3D MAGNETohydrodynamic (MHD) simulation of the Boston University outer heliosphere model where we used a newly developed approach that distributes the non-adiabatic shock heating among the cold protons, electrons, and pickup-ions (PUIs), while maintaining total energy conservation of all ions (cold protons and PUIs) and electrons. In our previous simulations ( E.S. Bair et al. 2025; B. van der Holst et al. 2026), all non-adiabatic shock heating was channeled to the cold protons, resulting in a too large temperature jump at the termination shock (TS) for the thermal solar wind. Using a new methodology we improved the simulation results with respect to the temperature jump observed at the TS by Voyager 2 (V2) spacecraft. Our simulations approached the observed jump conditions of a factor 10--20 in the cold solar wind temperature V2 measurements, and we obtain improvements in the simulation results relative to the data. Because we directly estimate in this way the distribution of non-adiabatic heating at the TS, we have the opportunity to study the physical process of heating cold plasma and PUIs in the TS. The results show that having almost 100\% non-adiabatic shock heating going towards PUIs at the TS reproduces the jump conditions observed along the V2 trajectory. This information is key to understanding the physical processes that shape the heliosphere. As shown by M. Opher et al. (2020), PUIs significantly change the shape of the heliosphere, for example, the presence of hot PUIs results in a deflated inner heliosheath. Our work provides the architecture of how energy partitioning at shocks in kinetic simulations (J. Giacalone et al. 2021) can be utilized in global MHD models.
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