mm-jets in the multi-messenger era

Karri I. I. Koljonen; Thomas D. Russell; Britton Jeter; Lauren Rhodes; Alexandra J. Tetarenko; María Díaz Trigo; Talvikki Hovatta; Pau Bosch-Cabot; Mamta Pandey-Pommier; Alessio Marino; Jakob van den Eijnden; Dieu D. Nguyen; Melania Del Santo; Thomas Maccarone; Anna Y. Q. Ho; Maria C. Baglio; Sera Markoff; the ALMA2040 Transient; Time-Domain Astronomy working group

arXiv · 2610.20741

mm-jets in the multi-messenger era

Karri I. I. Koljonen·Thomas D. Russell·Britton Jeter·Lauren Rhodes·Alexandra J. Tetarenko·María Díaz Trigo·Talvikki Hovatta·Pau Bosch-Cabot·Mamta Pandey-Pommier·Alessio Marino·Jakob van den Eijnden·Dieu D. Nguyen·Melania Del Santo·Thomas Maccarone·Anna Y. Q. Ho·Maria C. Baglio·Sera Markoff·the ALMA2040 Transient·Time-Domain Astronomy working group

View original source ↗Read source document ↗Export metadata ↓

Abstract

Jets and outflows operate across the full cosmic mass scale from young stellar objects (YSOs) and X-ray binaries (XRBs) to active galactic nuclei (AGN), gamma-ray bursts (GRBs), and tidal disruption events (TDEs), shaping many time-domain and multi-messenger transients. Key questions concern on how jets are launched, accelerated and collimated; where and how they dissipate energy and accelerate particles; and how they couple to their environments to set electromagnetic counterpart diversity and feedback. Millimeter and sub-millimeter observations uniquely address these questions by tracking the evolving synchrotron turnover for robust calorimetry and Lorentz-factor constraints, providing full-Stokes polarization and Faraday diagnostics close to the jet base, and enabling high-resolution imaging from Galactic ejecta to event-horizon-scale AGN jet bases via global Very Long Baseline Interferometry (VLBI). We describe the jet and outflow science enabled by ALMA2040, a next-generation mm/sub-mm interferometer combining an order-of-magnitude sensitivity gain with rapid-response observing, simultaneous multi-band coverage, full-Stokes polarimetry, and integration with global VLBI networks. These capabilities will enable statistically controlled, trigger-driven samples spanning XRB outbursts, early GRB afterglows, protostellar disk winds and jet launching, AGN jet bases, and jetted TDEs, establishing mm/sub-mm astronomy as a cornerstone of time-domain and multi-messenger jet physics in the 2040s and beyond.

Explore related subjects

astro-ph.HE astro-ph.IM

Keep this discovery

Explore connections, maps & timelines

BibTeX RIS

Karri I. I. Koljonen, Thomas D. Russell, Britton Jeter, Lauren Rhodes, Alexandra J. Tetarenko, María Díaz Trigo, Talvikki Hovatta, Pau Bosch-Cabot, Mamta Pandey-Pommier, Alessio Marino, Jakob van den Eijnden, Dieu D. Nguyen, Melania Del Santo, Thomas Maccarone, Anna Y. Q. Ho, Maria C. Baglio, Sera Markoff, the ALMA2040 Transient, Time-Domain Astronomy working group. 2026-10-14. mm-jets in the multi-messenger era. https://arxiv.org/abs/2610.20741

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Hydrodynamic instabilities in long-term three-dimensional simulations of neutrino-driven supernovae of 13 red supergiant progenitors

We present long-term three-dimensional (3D) simulations of Type-IIP supernovae (SNe) for 13 non-rotating, single-star, red-supergiant (RSG) progenitors with zero-age-main-sequence masses between 12.5 M$_{\odot}$ and 27.3 M$_{\odot}$. The explosions were modelled with a parametric treatment of neutrino heating to obtain defined energies, ${}^{56}$Ni yields, and neutron-star properties in agreement with previous results. Our 3D SN models were evolved from core bounce until 10 days to study how the large-scale mixing of chemical elements depends on the progenitor structure. Rayleigh-Taylor instabilities (RTIs), which grow at the (C+O)/He and He/H interfaces and interact with the reverse shock forming after the SN shock has passed the He/H interface, play a crucial role in the outward mixing of ${}^{56}$Ni into the hydrogen envelope. We find most extreme ${}^{56}$Ni mixing and the highest maximum ${}^{56}$Ni velocities in lower-mass (LM) explosions despite lower explosion energies, and the weakest ${}^{56}$Ni mixing in the 3D explosions of the most massive RSGs. The efficiency of radial ${}^{56}$Ni mixing anti-correlates linearly with the helium-core mass and correlates positively with the magnitude of a local maximum of $ρr^3$ in the helium shell. This maximum causes shock deceleration and therefore facilitates high growth factors of RTI at the (C+O)/He interface in the LM explosions. Therefore fast-moving ${}^{56}$Ni created by the asymmetric neutrino-heating mechanism is carried into the ubiquitous RT-unstable region near the He/H interface and ultimately far into the envelopes of the exploding RSGs. Our correlations may aid improving mixing prescriptions in 1D SN models and deducing progenitor structures from observed SN properties..

astro-ph.HE↗

arXiv2026

A Unified Solution to the Low-Mass X-ray Binary Diversity Puzzle: Saturated Magnetic Braking Coupled with Irradiation-Driven Winds

The standard magnetic braking (MB) model has long failed to explain key properties of low-mass X-ray binaries (LMXBs)---including their accretion rates, the formation of ultracompact binaries, and orbital expansion---casting doubt on binary evolution and gravitational-wave progenitor predictions. Phenomenological modifications exist, but a unified, physically grounded mechanism has been missing. Here we show that the overlooked coupling between magnetic saturation and irradiation-driven winds (IDW) provides this missing framework. Accretion-powered irradiation enhances the donor wind, which in turn amplifies MB exactly where needed. Our Saturated MB + IDW (SMB+IDW) model simultaneously resolves three outstanding discrepancies with no fine-tuning: (1) it reproduces the full observed distribution of accretion rates across persistent and transient LMXBs; (2) it naturally explains ultracompact X-ray binary formation; and (3) it quantitatively matches the orbital period distribution of descendant millisecond pulsar (MSP) binaries---a critical independent test failed by all previous models. Critically, the SMB+IDW model transforms MB from an externally imposed condition into a self-consistently regulated process tied to the accretion history. By unifying LMXB evolution to MSPs in a single physical picture, our work resolves the long-standing diversity puzzle and establishes a physics-based foundation for next-generation population synthesis, gravitational-wave progenitor predictions, and compact binary interpretation across cosmic time.

astro-ph.HE↗

arXiv2026

Gamma-ray calorimetry of Seyfert winds

Two stacking analyses with the Fermi Large Area Telescope (LAT) detected GeV emission from radio-quiet Seyferts, one selected by an X-ray ultra-fast outflow (UFO) and one hard-X-ray-bright, with similar luminosities attributed to different mechanisms: wind shocks and the accretion-disk corona. We investigate how efficiently Seyfert outflows convert mechanical power into GeV photons, whether the two detections require distinct mechanisms, and how Seyferts compare with low-ionization nuclear emission-line regions (LINERs). Without new Fermi-LAT data reduction, we homogenize published measurements to 0.1-100 GeV, place local mechanical accelerators on one L_gamma-Edot diagram, and express eta = L_gamma/Edot as a fraction rho of the complete-calorimetry efficiency eta_max ~ 2.5%, inverting rho for the ambient density required by pp losses. Winds from Seyfert active galactic nuclei (AGN) have rho = 0.020 (+0.018/-0.011) for acceleration efficiency 0.1, a factor of ~13.5 below starburst superwinds (rho = 0.26 (+0.37/-0.16)). The difference exceeds a factor of three with probability 0.95 and is independent of acceleration parameters common to both classes; it is conditional on the wind kinetic powers, collapsing only if every wind sits at its minimum launch radius. The implied densities, ~10 and ~100 cm^-3, are consistency values: density, shock radius and speed are degenerate. The two stacking detections agree within a factor of 1.75 in gamma-ray output per unit Eddington luminosity, but the 95% interval, 0.26-24, is too wide to distinguish them. A third stack, of 186 low-luminosity AGN, extends the comparison 1.5 dex lower, ordered by AGN power. GeV detectability of non-jetted AGN is set by the product of mechanical power and calorimetric fraction. LINER outflows fail on power; for the adopted wind energetics, Seyfert UFO winds fail on calorimetry; starburst superwinds succeed on both.

astro-ph.HE↗