By analogy to the Earth and other bodies in the Solar System endowed with an organized large-scale magnetic field, black holes and neutron stars can be surrounded by a “relativistic magnetosphere”. This region plays a pivotal role in the formation of plasma outflows and particle acceleration. Like their non-relativistic analog, relativistic magnetospheres are intrinsically dynamic and sometimes reorganize abruptly via various plasma processes such as magnetic reconnection which give rise to pronounced particle acceleration and bursts of energetic radiation directly observable from Earth.

The emission of short pulses of light shaped by spinning neutron stars (pulsars) is a famous example of an astrophysical phenomenon most certainly involving an active relativistic magnetosphere. Although pulsars were discovered more than fifty years ago by radio astronomers, the origin of this emission remains today an outstanding puzzle. Giant X-ray magnetar flares – and their possible connection to the mysterious Fast Radio Bursts – are far more extreme and less well understood phenomena that involve another flavor of neutron star magnetospheres. Supermassive black hole magnetospheres may also play a crucial role in launching extragalactic relativistic jets observed in active galaxies. The first images of the M87* and SgrA* black holes obtained by the Event Horizon Telescope bring for the first time direct constraints on the innermost regions close to the black hole horizon possibly hosting a jet-launching magnetosphere. The discovery of hotspots orbiting at a few gravitational radii away from the SgrA* hole thanks to the exquisite astrometric measurements of the Gravity collaboration at the VLTI and ALMA provides other possible hints of an active magnetosphere.

The aim of this workshop is to bring together experts in the field of relativistic plasma astrophysics to highlight recent progress but also major shortcomings in our understanding of plasma flows and dissipative processes within the magnetospheres of compact objects from an observational, theoretical and computational perspective.

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The ambition of ASTROPHYSICS2025 is to be a pre-eminent international forum to accentuate novel developments, share new conceptions, research results, and development experiences, and provide networking opportunities with rivals to help inaugurate connections for early professional scientists.

For more information: https://astrophysicsmeet.org/

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The focus of this conference will be understanding the role of star formation and stellar feedback in driving galactic evolution; The conference aims at identifying a number of key steps in the feedback ladder and using studies of nearby galactic sources dominated by feedback to quantitatively understand the role of feedback in shaping the local universe around us.

The meeting will focus on:

• Stellar feedback on molecular cloud scales
• Stellar feedback and galactic ecology
• Stellar feedback in extreme environments
• Stellar feedback galactic scales

By developing a “feedback ladder” from the scale of individual O stars, to small clusters, to super star clusters, to galactic outflows, we expect to quantitatively address the role of stellar feedback in the ecology of galaxies and how feedback by massive stars depend on the properties of the environment.

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Closer collaboration between computer scientists and astrophysicists can be extremely beneficial for both. The same data can be used by astrophysicists to draw physical conclusions, and by computer scientists for analytics/processing/mining purposes. In addition, many AI frameworks have become publicly available and are slowly becoming a significant part of our every day lives and activities. However, the introduction of AI to the broader public has not happened without some amount of controversy. Astrophysics and cosmology are among the very few, if not the only, disciplines where AI applications can explore their full potential without ethical constraints.

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The most massive M* > (10)11 and oldest galaxies account for more than half of the total stellar mass in the local Universe. Their formation and evolution still represent an open contentious question in present-day astrophysics and cosmology. Recent observations have revealed the presence of massive quiescent galaxies even in the first cosmic epochs (out to z>4), representing a challenge for galaxy formation models: it is unclear how they became so massive  over such short timescales, how their stellar metallicity grew so fast to solar or supersolar values and, finally, what quenched these objects so quickly and efficiently. 

The main aim of this symposium is twofold: 

1. Review  results from the latest observations of massive quiescent galaxies in the Universe, from high-z to z~0; then,

2. Critically analyze to what extent state-of-the-art theoretical models of galaxy formation and evolution can reproduce observations. 

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Topics:

• Black holes and pulsars in dense clusters
• Galactic Nuclei, dynamics and evolution
• Galactic and Extragalactic Star Clusters
• Stellar Population in Star Clusters
• Formation of black hole binaries in star clusters
• Simulations of realistic cluster dynamics with various codes
• Multi-messenger astronomy

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The conference aims to provide a platform for researchers, academicians, and professionals to share their groundbreaking research findings, explore new theories, and engage in thought-provoking discussions on a wide array of topics. Key themes include black hole physics, cosmology, stellar evolution, planetary science, and space exploration technologies.

Attendees will have the opportunity to participate in a diverse range of sessions, including keynote speeches from renowned experts, panel discussions, workshops, and poster presentations. These sessions are designed to foster collaboration, inspire new research directions, and address the challenges and opportunities in the rapidly evolving landscape of space science.

In addition to the formal sessions, the conference will offer ample networking opportunities, allowing participants to connect with peers, establish collaborations, and exchange ideas in an informal setting. The vibrant city of Budapest, with its rich cultural heritage and stunning architecture, will provide a picturesque backdrop for the event, enhancing the overall experience for attendees.

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We hereby invite proposals from colleagues who are interested in organising a Symposium, a Special Session, or a Lunch Session at the EAS Annual Meeting 2025.

A broad range of parallel sessions can be accommodated as:

(A) Symposia: which normally consist of up to 6 blocks of 1.5 hours, stretching over 2 days, although exceptionally and in well-justified cases these symposia can be longer,
(B) Special Sessions: consisting of up to 3 blocks of 1.5 hours on the same day.
(C) Lunch Sessions: taking place during the lunch break for 1-1.5 hours on one day.
(D) Special Sessions with a Lunch Session: combining the blocks during parallel scientific sessions and a session during the lunch break on one day (for special purposes, e.g., hands-on session, etc; this option is not to extend the length of scientific blocks).

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NAM2025 covers the full range of astronomy research in the UK, including the instrumentation and astro-particle communities, as well as other key issues relevant to the UK astronomy community. Beside the UK’s astronomy community, the meeting includes the UK Solar Physics (UKSP), and the Magnetosphere Ionosphere and Solar-Terrestrial (MIST) communities.

It is centrally located in the modern purpose-built Teaching and Learning Centre (TLC) and the opposing Ogden Centre West (OCW) building which hosts the majority of the astronomy research at Durham University.

NAM2025 is a hybrid conference but where the majority of participants are expected to attend in person. By using a hybrid model we aim to allow as many people as possible to experience the conference and learn about the exciting astronomy and space science research being conducted around the UK and further afield.

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