Announcements of Upcoming Meetings

The Nancy Grace Roman Space Telescope, planned to launch in late 2026, will be capable of surveying the sky 1000 times faster than the Hubble Space Telescope with similar sensitivity and resolution. A combination of near-infrared imaging and spectroscopic surveys, designed by Roman's community-defined Core Community Surveys and General Astrophysics Survey programs, will generate unique data-sets and large-area maps of the sky that will catalyze scientific discovery across all of astrophysics. Roman's accurate mapping of stars, galaxies, and galaxy clusters will offer the unique ability to map our Universe, both the seen and the unseen.

This conference aims to focus on the intersection of galaxy formation and evolution with dark matter and dark energy. It will explore the novel research that is possible only with large cosmic surveys and simulations and discuss how the community will be able to optimize scientific output with Roman in the future. Topics of discussion will include, but are not limited to, the expected impacts from Roman observations of galaxy clustering, baryon acoustic oscillations, weak lensing, galaxy clusters, supernova cosmology, stellar streams, and dwarf galaxies. The conference will also strive to foster synergies between contemporaneous experiments to Roman, such as Euclid, Rubin's LSST, DESI, and Simons Observatory. The schedule will feature invited talks, contributed talks, posters, discussion panels, and fun social activities.

Attendance: The workshop will be a hybrid event (in-person and virtual). To maximize engagement, in-person attendance is encouraged for all participants, especially speakers.

SOC

Ami Choi (NASA Goddard Space Flight Center; Co-Chair), Javier Sanchez (STScI; Co-Chair), Alexandra Amon (Princeton University), Ori Fox (STScI), Konrad Kuijken (Leiden University), Patricia Larsen (Argonne National Laboratory), Lado Samushia (Kansas State University), Yun Wang (Caltech/IPAC), Yuanyuan Zhang (NOIRLab)

LOC

Leslie Beauchamp (STScI), Annalisa Calamida (STScI), Samantha Hoffmann (STScI), Max Mutchler (STScI), Cristina Oliveira (STScI), Melissa Shahbandeh (STScI), Shemiah Smith (STScI)

Further information:

The workshop is intended to be in-person to ease productive discussion and will lead to the publication of conference proceedings.

For additional questions, please see the workshop website.

The International Conference on General Relativity and Gravitation is organised every three years under the guidance of the International Society on General Relativity and Gravitation. It is the principal international meeting for scientists working in all areas of relativity and gravitation.

The Edoardo Amaldi Conference on Gravitational Waves is organised every two years under the guidance of the Gravitational Wave International Committee. It is the principal international meeting for scientists working in all areas of gravitational-wave science.

In 2025, the 24th International Conference on General Relativity and Gravitation (GR24) and the 16th Edoardo Amaldi Conference on Gravitational Waves (Amaldi16) will be held together as a joint meeting, bringing together experts from across classical and quantum gravity, mathematical and applied relativity, gravitational-wave instrumentation and data-analysis, and multimessenger astronomy.

The GR24-Amaldi Meeting will be held as a primarily in-person event at the Scottish Event Campus, Glasgow. Online resources will be made freely available after the event. Meeting organisation is led by the Institute for Gravitational Research at the University of Glasgow and the Institute of Physics.

For additional questions, please see the conference website.

The LIGO–Virgo–KAGRA Collaboration invites the core-collapse supernova (CCSN) astronomy and astrophysics community for a 5-day Symposium on July 21–25, 2025, at the University of Warsaw, Poland. CCSNe are among the most violent explosions known to occur in the Universe, and the next Galactic or near-extra-Galactic exploding massive star will be one of the most interesting, and most important, astronomical events of the century. This Symposium aims to bring CCSN experts together to address how to maximize the scientific potential of the first detection of core collapse supernova gravitational waves (GWs). The Symposium hopes to bring together GW astronomers and CCSN modelers, as well as neutrino and nuclear theorists, neutrino astronomers, and astronomers across the electromagnetic spectrum.

The sensitivity of GW detectors and progress on CCSN modeling are unprecedented, and we expect them to further advance in the coming years. A joint effort across communities has great potential to fully utilize these advances for CCSN GW discovery. Each day, we will host (before lunch) a set of lectures on one of the key topics listed below, to establish a common understanding and a common language. Moreover, each day (after lunch) will also include invited and contributed talks, as well as discussion. The focus topics of the Symposium are:

• Day 1: CCSN Theory
• Day 2: CCSN Gravitational Wave Detection and Parameter Estimation
• Day 3: CCSN Neutrino Detection
• Day 4: CCSNe across the Electromagnetic Spectrum
• Day 5: CCSNe over the Next Ten Years

The proceedings of the Symposium will be published in a special issue of Classical and Quantum Gravity. We hope the proceedings will serve as a reference for students, postdocs, and faculty in, or entering, the field, serve to capture the current state of core collapse supernova gravitational wave astronomy and astrophysics, outline lessons learned, and provide recommendations for future development.

Everyone who wishes to advance the field of CCSN GW science is welcome!

Confirmed Lecturers:

Organizing Committee:

Marek Szczepańczyk (University of Warsaw); Marco Cavaglià (Missouri University of Science and Technology); Anthony Mezzacappa (University of Tennessee, Knoxville); Jade Powell (Swinburne University of Technology); Adam Szereszewski (University of Warsaw)

For additional questions, please see the conference website.

We are pleased to announce the inaugural open community conference for NASA's Habitable Worlds Observatory, to be held at the Johns Hopkins Bloomberg Center in Washington, DC, from July 28 - 31, 2025. This milestone event will bring together scientists, engineers, industry and community stakeholders to propel the development of HWO, a mission expected to usher in a new era of astrophysics discovery and address one of humanity's oldest questions "Are we alone?"

The Habitable Worlds Observatory is NASA Astrophysics' next flagship mission, and builds on the heritage of the Hubble, Webb, and Roman Space Telescopes. It will deploy advanced ultraviolet, optical, and infrared technologies to identify potentially habitable worlds and analyze their atmospheres for signs of life. This same technology will empower astronomers to address fundamental, persistent questions in cosmology, galaxy evolution, the origins of elements, and our Solar System's place in the universe.

HWO has made significant progress in the past year, with NASA establishing a dedicated Technology Maturation Project Office at Goddard Space Flight Center, working in close collaboration with the Jet Propulsion Laboratory, Ames Research Center, and Marshall Space Flight Center. This initiative advances critical technologies and science cases, and fosters collaboration across government, academia, and industry. Results of HWO working groups will be showcased together with contributions from the global astronomy and engineering communities.

Topics of interest include, but are not limited to:

Science:

• Galaxy Growth: Cosmic Web (Intergalactic & Circumgalactic Medium), Active Galactic Nuclei & Black Holes, Galaxy Evolution
• Evolution of the Elements: Stars & Stellar Populations, Star Formation & Interstellar Medium, Cosmic Explosions
• Cosmology: Nature of Dark Matter & Dark Energy, Distance Scale, Hubble Tension
• Planetary Systems: Formation, Evolution, Architectures, Our Solar System, Exoplanet Demographics
• Search for Life: Target Stars & Systems, Biosignatures, Habitability

• Starlight Suppression: Contrast Technology & Methods
• Ultrastable Telescope and Observatory Technology
• Ultraviolet, Optical, & Near-Infrared Instrument Technologies: mirror coatings, gratings, detectors, spectroscopic multiplexing technologies
• L2 Servicing technology and commercial synergies
• Emerging Technologies: photonics, quantum sensing
• Artificial Intelligence & Machine Learning for mission development, engineering, science research

For additional questions, please see the conference website.

The High Energy Phenomena in Relativistic Outflows (HEPRO) conferences are a series of biennial meetings devoted to the discussion of the most recent theoretical, phenomenological, and observational developments in the field of high-energy phenomena associated with relativistic winds and jets. Previous editions were held in Dublin (2007), Buenos Aires (2009), Barcelona (2011), Heidelberg (2013), La Plata (2015), Moscow (2017), Barcelona (2019), and Paris (2023).

The HEPRO IX edition will be held in Rio de Janeiro, Brazil, from August 4 to August 8, 2025. Some specific topics covered during the meeting will be gamma-ray and neutrino production in relativistic outflows, multi-wavelength jet emission, formation and propagation of relativistic jets on different scales, PeVatron sources, and particle acceleration in various relativistic contexts.

The sessions will be held in "Casa de Rui Barbosa" in Botafogo, Rio de Janeiro, Brazil.

For additional questions, please see the conference website.

Binary stars lie at the heart of many key astrophysical phenomena. Various explosive cosmic events result from binary stars, as do close double black holes/neutron stars/white dwarfs, type Ia supernovae, X-ray binaries, millisecond pulsars etc. Relying on existing large scientific facilities, classical optical, radio and X-ray observations are discovering increasingly large numbers of such binary stars. A decade ago, the ground-based LIGO/Virgo detected the merging of two stellar-mass binary black holes, opening a new window in gravitational wave astronomy. In the future, with the support of next-generation astronomical instruments, we shall discover many more binary-related celestial objects. Against this backdrop, we convene this conference, inviting all international observers and theoreticians in the field of stellar science to participate in and exchange recent progress related to binary stars and to look forward to future collaboration and development of new directions for research.

Topics:

• Binary star interactions: from mass transfer to common envelope evolution.
• Supernovae: from progenitor modeling to explosion simulation.
• Gravitational wave sources: from double black holes to white dwarfs.
• Exotic stars: X-ray binaries, binary pulsars, luminous red novae, hot subdwarfs, cataclysmic variables, symbiotic stars, etc.
• Binary population synthesis studies on binary objects.
• Binary star observations from large facilities: Gaia, TESS, LAMOST, JWST, FAST, etc.

Floor Broekgaarden; Xuefei Chen; Hongwei Ge (Chair); Zhanwen Han; Natalia Ivanova; Christopher Adam Tout

Local Organizing Committee:

Hailiang Chen; Hongwei Ge; Yanjun Guo; Wenyan Ji (Secretary); Shi Jia; Dengkai Jiang; Jiangdan Li; Jiao Li; Zhenwei Li; Zhengwei Liu (Chair); Xiangcun Meng; Bo Wang; Jianping Xiong; Lifu Zhang

For additional questions, please see the conference website.

Understanding the evolution of the interstellar medium (ISM) is essential for comprehending star formation and galaxy evolution. Galaxies are composed primarily of stars and the ISM, and the physical properties of the ISM—such as density, temperature, and kinematics—serve as the initial conditions for star formation, making them fundamental to understanding galactic evolution. The ISM encompasses various physical states, from hydrogen gas (atomic and molecular) to hot plasma and high-energy particles. These states span several orders of magnitude in density (10^-4—10³ cm^-3), temperature (10^–1 billions of Kelvins), and spatial scale (parsecs to hundreds of kiloparsecs), each governed by distinct radiative processes and interacting dynamically with one another. Therefore, it is crucial to investigate the multi-phase structure of the ISM across various wavelengths. This includes cold gas, which is the bulk of the ISM mass, diffuse hot plasma, and high-energy processes that dominate volume and energy. A comprehensive understanding requires a multi-wavelength approach, capturing the ISM's evolution over its wide temperature and density range. However, such multi-faceted studies remain challenging due to the diverse observational techniques and limitations across wavelengths. This symposium invites observational and theoretical researchers interested in the evolution of the ISM through multi-wavelength analyses. It will also explore the prospects of employing next-generation telescopes to advance multi-wavelength studies and aim to foster new collaborations.

While the following topics are expected to be central themes, we strongly encourage contributions on any related subjects to foster broad and inclusive discussions.

1. Impact of Galaxy Interactions on the ISM and Star Formation (Large-Scale Impact)
• How do large-scale gas flows triggered by galaxy interactions drive star formation?
• What are the observable signatures in gases and dust?
• How do tidal interactions and mergers heat the interstellar gas?
2. The Impact of Stellar Feedback on the ISM (Medium-Scale Impact)
• How does gas heating and ionization occur due to stellar radiation?
• How do cosmic rays contribute to ISM ionization and heating?
• What is the impact on subsequent star formation?
3. Shock-Cloud Interactions and Cosmic Ray Acceleration (Small-Scale Impact)
• How do shock-cloud interactions induce turbulence?
• What gamma-ray signatures originate from high-energy interactions, such as particle acceleration and cosmic-ray interactions with gas?
• How do shocks contribute to cosmic ray acceleration and impact the surrounding medium?

Aya Bamba (The University of Tokyo); Yasuo Fukui (Nagoya University); Kathryn Kreckel (Heidelberg Unviersity); Knox Long (Space Telescope Science Institute); Martin Pohl (Deutsches Elektronen-Synchrotron DESY); Manami Sasaki (Friedrich-Alexander University Erlangen-Nürnberg); Kengo Tachihara (Nagoya University); Kisetsu Tsuge (Gifu University; SOC/LOC chair)

For additional questions, please see the conference website.

Observations of the local and high-z Universe confirm that star formation is an inherently clumpy and clustered process and, as a consequence, the physical properties of star clusters are expected to be intimately linked with those of their hosts. In particular, the long-lived massive star clusters can be used to trace galaxy assembly and the gas properties at the time of their formation, and they may be one of the primary sources of reionization of the Universe. This field is currently undergoing a revolutionizing phase. Large surveys carried out with ground and space based telescopes (such as Gaia, HST, Euclid, ALMA, ESO/VLT) have enabled unprecedented photometric and spectroscopic studies in the Local Universe and the JWST's access to rest-frame optical wavelengths at z>3 along with the magnification power of gravitational lensing are opening a new era in the study of the star-forming modes well within the reionization epoch allowing us to directly probe star cluster formation and constrain unprecedented/unexpectedly dense stellar systems as possible sites of GC formation.

The formation and evolution of star clusters is inherently a multi-physics and multi-scale problem, involving star formation and feedback, galaxy formation and evolution, N-body dynamics, stellar and binary evolution. As a consequence, the broad range of interconnected issues concerning the study of star clusters and their host galaxies can be addressed only with an interdisciplinary approach.

In this exciting and rapidly changing context, we aim at bringing together observers and theorists from both the local and high-z Universe communities. The goal is to inspire discussions and exchange ideas about how to perform a transformative leap in the field, build a comprehensive picture of star cluster formation and evolution, explore the link between old massive, young star clusters and high-z proto-globular clusters, their connection to galaxy formation and their potential role in the reionization of the Universe. Focus will be given to how efficiently leverage available observations spanning different spatial, temporal and physical scales, along with those that will be soon on-line thanks to the several upcoming new giant facilities (such as E-ELT, Vera Rubin Telescope, Nancy Grace Roman Space Telescope, GMT), and the new generations of dynamical and cosmological hydro-dynamical simulations at spatial scales suitable to resolve stellar clusters.

Confirmed Invited Speakers:

Angela Adamo (Stockholm University); Oscar Gonzalez (STFC UKRI); Sebastian Kamann (Liverpool LJMU); Natalia Lahén (Max Planck Institute); Hui Li (Tsinghua University); Matteo Messa (INAF Bologna); Massimo Ricotti (Maryland University); Elena Sabbi (NOIRLab)

Scientific Organizing Committee:

Emanuele Dalessandro (INAF Bologna; co-Chair); Alison Sills (McMaster University; co-Chair); Mario Cadelano (University of Bologna); Michela Mapelli (Heidelberg University); Florent Renaud (Observatoire Astronomique de Strasbourg); Eros Vanzella (INAF Bologna); Enrico Vesperini (Indiana University)

Local Organizing Committee:

Emanuele Dalessandro (INAF Bologna); Greta Ettorre (INAF Bologna); Alessandro della Croce (INAF Bologna); Mario Cadelano (University of Bologna); Cristiano Fanelli (INAF Bologna); Silvia Leanza (University of Bologna); Raffaele Pascale (INAF Bologna)

For additional questions, please see the conference website.

The decisive role of massive black holes in galaxy evolution is implied through scaling relations with galaxy properties and observations of ubiquitous nuclear outflows across a wide redshift range. In simulations, accretion onto black holes is a key ingredient in matching observed galaxy mass functions. Recently, the surprisingly high abundance of AGN at z>4 revealed through JWST observations has sparked renewed interest in massive black hole seeding and growth during the first billion years from both observational and theoretical sides.

The conference aims at bringing together researchers studying massive black holes across and beyond the electromagnetic spectrum, as well as theorists and simulators to discuss recent advances in the research of massive black hole growth, evolution, demographics, and impact across cosmic time.

We will focus on the following key themes:

• Observational indicators of massive black holes across cosmic time
• Observational constraints on black hole masses through a variety of techniques and across wavelengths (including stellar dynamics, reverberation mapping, single-epoch virial relations, scaling relations, and gravitational waves)
• Black hole demographics as a function of redshift through simulationsConstraints on massive black hole formation (including seeding models) and growth pathways through theory, and in combination with observations
• Impact of black holes on galaxy evolution evidenced through feedback and scaling relations in observations and simulations

Xiaohui Fan (University of Arizona); Jenny Greene (Princeton University); Sophie Koudmani (Herts/KICC); Roberto Maiolino (KICC, co-chair); Chris Moore (KICC/IoA/DAMPT); Priyamvada Natarajan (Yale University); Debora Sijacki (KICC); Hannah &Ueml;bler (MPE, co-chair)

Local Organising Committee:

Sophie Koudmani(Co-chair); Jan Scholtz(Co-chair); Leah Bigwood; Steve Brereton(admin); Stephanie Buttigieg; Sophia Geris; Lucy Ivey; Xihan Ji; Ignas Juodžbalis; Roberto Maiolino; Eun-jin Shin; Debora Sijacki; Alison Wilson (admin)

For additional questions, please see the conference website.

A working model for outbursts in dwarf novae was proposed by Prof. Yoji Osaki in 1974, which is currently known as the disk instability model. We are celebrating the 50th anniversary of the invention of this model by organizing an international workshop.

This workshop aims to review the history of the development of the disk instability model, understand the essential physics, and share the latest research results with participants.

We hope that this workshop will help young researchers set the direction for future research. Also, this workshop will provide smooth communication between senior leading researchers and young researchers & students.

For additional questions, please see the conference website.

MMC2025: Multi-phase, Multi-temperature, and Complex. How Feedback Shapes the Nature of the CGM, Halo Gas, and Galaxies from Galaxy Groups to Clusters

The mechanisms driving galaxy evolution — AGN and stellar feedback — remain central to our understanding of how baryons are redistributed in collapsed structures. Despite significant progress, our theoretical models continue to diverge, particularly when predicting the gas content and star formation activity in low-mass halos, the circum-galactic medium (CGM), and the evolution of central galaxies across different environments. Feedback processes, in particular, play a critical role, with varying effects depending on the scale of the system, from individual galaxies in low-mass halos to massive galaxy clusters.

MMC2025 will bring together experts to address these challenges, focusing on the latest observational results and state-of-the-art hydrodynamic simulations. We will explore the multi-phase, multi-temperature nature of the CGM and its complex interplay with AGN feedback, gas inflow, and star formation across diverse environments —from bright clusters at high redshifts to low-mass halos. The workshop will highlight key observational datasets, including X-ray, SZ, and IFU data, as well as advancements in radio and submillimeter observations, offering fresh insights into the gas and feedback processes shaping galaxies.

Join us in Olbia, Italy, to discuss how these feedback mechanisms drive the evolution of galaxies and clusters, with a special focus on the role of AGN feedback in low-mass halos and its effect on gas content and star formation. MMC2025 will be a unique opportunity to combine cutting-edge observational data with theoretical models to advance our understanding of large-scale structure and galaxy formation and evolution.

We look forward to your participation in this exciting scientific event!

SOC:

Paola Popesso (chair); Ilaria Marini; Marcella Brusa; Dylan Nelson; Klaus Dolag; Paolo Tozzi; Stefano Ettori; Esra Bulbul; Veronica Biffi; Veronica Strazzullo; Eleonora Sani; Silvia Bonoli; Lorenzo Lovisari; Celine Peroux; Celine Gouin; Fabio Gastaldello

LOC:

Ilaria Marini; Paola Popesso; Denisa Tako; Victoria Toptun; Natan de Isidio; Daudi Mazengo

For additional questions, please see the conference website.

The X-Ray Imaging and Spectroscopy Mission (XRISM), launched on September 7th, 2023, is a collaborative mission between JAXA and NASA, with contributions from over 70 institutions in Japan, the U.S., Canada, and Europe. With the successful combination of high-resolution spectroscopy and wide-field imaging, XRISM has provided us with an unprecedented view of the Universe, opening a new era of high-energy astronomy.

This conference will highlight the scientific achievements from the first two years of XRISM and identify key issues we should address in the next observation cycles. Conference topics also cover theoretical studies related to XRISM observations and synergies with other observatories, including future missions.

This is the first international conference for XRISM, launched in September 2023. Conference topics will include:

• Formation of the largest structures in the Universe
• Chemical evolution of the Universe
• Active galactic nuclei and their environment
• Endpoints of stellar evolution
• Accretion and outflow in compact objects
• New physics with high-resolution X-ray spectroscopy
• XRISM for multi-wavelength/multi-messenger astronomy

October is a good season in Kyoto with nice weather and full of tourists, so please make your hotel reservations as early as possible if you are planning to attend. The venue is within walking distance of Kyoto Station.

We look forward to seeing you there. Save the date!

For additional questions, please see the conference website.

*** SAVE THE DATE ***

We are pleased to announce the 4th TDAMM Workshop: Advancing Community Observing Plans for Rapid Follow-Up of Explosive Transients will be held October 27-30, 2025 in Huntsville, Alabama.

NASA's new Astrophysics Cross-Observatory Science Support (ACROSS) initiative is organizing the 4th Time Domain and Multi-Messenger Astrophysics (TDAMM) Workshop. This workshop will focus on developing community observing plans to enable the rapid and coordinated follow-up of explosive transients by space-based and ground-based observatories. NASA invites US and international members of the ground and space science communities to attend the workshop and contribute to its final product, a publicly available white paper with findings for relevant agencies and the broader astrophysics community.

If you are interested in attending and/or would like to be on our email list to receive further updates please fill out the following Google form here.

Please visit the website for additional information.

Active galactic nuclei (AGN) are among the most dynamic and powerful sources in the universe, powered by supermassive black holes (SMBHs) through mass accretion. The accretion rate influences many AGN properties, with high accretion rates playing a key role in growing black holes and launching outflows that may shape the host galaxy's growth. Highly accreting AGN, particularly at low redshift, offer a benchmark to understand the rapid growth of the first SMBHs in the early Universe, which remains a mystery to be solved.

Significant theoretical and observational advancements have been made in understanding fast-accreting systems, thanks to long-running observatories like VLT, ALMA, JVLA, Chandra, XMM, HST, and NuSTAR, as well as the recently launched JWST, Euclid, and IXPE. With the first light of the ELT on the horizon and the recent results from JWST on the growth of SMBH at high redshift, now is the ideal time to convene and share insights on highly accreting SMBHs. The workshop will gather astronomers to summarize the field's current status, bridging the accretion history from the early to the local Universe, and explore the mechanisms driving their growth and impact on the Universe.

This workshop will focus on the following key themes:

• NLS1s and other low-z highly accreting AGN and their cosmological implications;
• Outflows, jets, feedback in highly accreting sources from the nearby Universe to cosmic dawn;
• Surrounding environment and host galaxy properties of highly accreting AGN at all epochs;
• Theoretical and observational advances in the nuclear properties of extreme accreting AGN from low-z to high-z;
• Changing-look, tidal disruption event and their implication in changing the accretion state of AGN;
• Recent progress in the study of QSOs at high-z and AGN evolution;
• Recent observations with state-of-the-art facilities (JWST, ALMA, XMM-Newton), future observations with new facilities (Vera Rubin, Athena, ELT, SKA, 4MOST, AXIS, PRIMA), theoretical modeling and AI.

For additional questions, please email to agn2025_loc[AT]eso[DOT]org or check out the conference website.

The 33rd Texas Symposium on Relativistic Astrophysics will take place in the vibrant city of Tempe, AZ, from December 8 – 12, 2025. The event will be hosted at The Omni Hotel, very near Arizona State University, which offers state-of-the-art facilities to ensure a productive and enjoyable meeting.

We are thrilled to announce that John Mather, Jim Peebles, Adam Riess, George Smoot (TBC), and Frank Wilczek have already agreed to participate and attend the symposium.

Beyond the symposium, Tempe in December offers a perfect blend of outdoor adventures and festive activities, making it an ideal winter getaway. The mild temperatures invite visitors to explore the scenic beauty of Tempe Town Lake, hike the iconic Hayden Butte, or stroll through the Desert Botanical Garden. You can also experience the Tempe Fantasy of Lights Boat Parade, a dazzling display of holiday lights along the lake. The city hosts various seasonal events, including holiday markets, outdoor concerts, and ice skating rinks, offering attendees a chance to enjoy the warm desert climate while celebrating the holiday season.

The symposium will cover all major topics on high-energy and particle astrophysics, cosmology, and relativity. It will include morning plenary sessions and afternoon parallel sessions, which will function as mini-symposia in each sub-field. The plenary sessions will consist of ~45-minute review talks. The afternoon sessions will feature oral talks (about 15-30 minutes) and poster contributions. Registration will open in early May.

We will be hosting a major international workshop on black hole accretion and jet formation at The University of Oxford between March 23-27, 2026. Our goal is to address the scaling of these phenomena across the mass and accretion rate spectra. We will consider all aspects of accreting black holes, including black hole transients, X-ray binaries, tidal disruption events, active galactic nuclei and the role of black hole accretion physics in cosmological simulations.

We aim to bring a new perspective to these problems, and hope to bring together the above diverse communities which too rarely intersect, and to do so in an engaging and efficient way.

We will have an in-person capacity of around 100, and to stream all talks and discussions online for free.

SOC: Rob Fender, Sera Markoff, Francesca Panessa, Jiri Svoboda, Erin Kara (to be expanded)

To express interest and be added to the mailing list for the meeting, please send a simple email to: blackholes2026[AT]physics[DOT]ox[DOT]ac[DOT]uk

For additional questions, please see the conference website.