The next CESRA Workshop will be held between July 3-7, 2023 in the University of Hertfordshire, located in Hatfield, just outside Greater London. It will be hosted by the Centre for Astrophysics Research.

Key discussion topics will feature observations, modelling and theory contributions related to Important dates: Scientific Organising Committee: Local Organising Committee:

The registration fee for the entire workshop is £225. The registration fee allows you to attend all workshop sessions and includes coffee breaks, workshop dinner, reception, and local tour.

To register with or without submitting an abstract, please complete the registration form below. You will receive an email with the instruction on how to pay the fee.

Financial support (registration fee discount) may be available to a small number of early career researchers. If you would like to be considered, please complete the appropriate section in the registration form. The deadline for requesting financial support is April 25, 2023.

You can register as an accompanying person by completing the registration form without submitting an abstract. You can specify "n/a" in the "affiliation" and "country of affiliation" fields. There is no special registration fee for accompanying persons.

Registration and abstract submission

The deadline for registration, abstract submission and fee payment is May 7, 2023.

Participants are required to familiarize themselves with UK entry requirements, current Covid requirements and other travel rules. Official information about travel to the UK can be found here. If you require an invitation letter to apply for a UK visa, please complete the form below after registering.

If you require a visa to enter the UK, please complete this form
Official information on UK entry requirements can be found here.

The meeting will start at 14:00 BST on Monday, July 3, 2023, and finish at 13:00 BST on Friday, July 7, 2023.

The workshop will include a plenary session, as well as four specialist working groups:

WG1: Sun-Earth connection and the inner heliosphere
Leaders: Jasmina Magdalenic and Ludwig Klein

Solar radio bursts provide us important information on the associated eruptive processes, such as flares and coronal mass ejections (CMEs), but also on the characteristics of the ambient plasma through which the radiation propagates. In this working group we focus mostly on the radio observations by the space based instruments on board e.g. WIND, Stereo, PSP (Parker Solar Probe) and SolO (Solar Orbiter). The diagnostics of coronal plasma employing radio observations at large wavelengths can be directly combined with the in situ and remote sensing observations, which is in particular the case for the novel PSP and SolO observations at close to the Sun distances. This working group aims to discuss on the recent findings, theories and models related to the radio emissions in the inner heliosphere, on what information about ambient coronal plasma such radio observations can provide us, but also on how the novel in situ and remote sensing observations by PSP and SolO can help us in advancing our knowledge on the radio emission processes.

WG2: Electron acceleration and radio emission in solar flares
Leaders: Alexander Warmuth and Hamish Reid

Different types of radio emission provide unique diagnostics on energy release and particle acceleration/transport in solar flares. Together with hard X-ray observations, they provide information on timing, location, and spectral characteristics of the nonthermal electrons, as well as their environment and associated physical processes. New observational assets allow us to put tighter constraints on acceleration and transport models. Conversely, there has been significant progress in numerical simulations of magnetic reconnection and particle acceleration. This working group aims to discuss how we can exploit these advanced observing and modeling capabilities to better understand radio emitting energetic electrons in solar flares.

WG3: Coronal mass ejections and associated radio emissions
Leaders: Alexander Nindos and Pietro Zucca

Coronal mass ejections (CMEs) are large-scale expulsions of coronal plasma and magnetic field propagating through the heliosphere. Because CMEs are observed by white-light coronagraphs which, by design, occult the solar disk, supporting observations (e.g. in EUV, soft X-rays, Halpha and radio) must be employed for the study of their source regions and early development phases. Radio observations have the potential of tracking both the CME and its possible shock wave from their formation in the low corona all the way to the inner heliosphere. These observations provide valuable diagnostics about the sites of electron acceleration, the properties of energetic electrons as well as the bulk properties of the CME magnetized plasma. In recent years new solar-dedicated and general-purpose radio instruments have been developed and old ones have been upgraded. These instruments provide extremely high cadence imaging spectroscopy observations, and have opened up new horizons in the study of CMEs, especially when they are paired with the latest EUV and white-light instruments. These developments indicate that it is a timely endeavor to review recent advances in radio CME research and highlight potential avenues for further studies. To this end, we welcome contributions by all colleagues who, at some point, have used radio observations for the study of CMEs.

WG4: Solar atmosphere, radio wave propagation and turbulence
Leaders: Gregory Fleishman and Christian Vocks

This working group is devoted to the radio studies related to active regions, the quiet solar atmosphere structure and dynamics, coronal heating, turbulence, radio wave scattering, refraction. We invite participants of the CESRA meeting to attend and present contributions that are relevant to these range of science topics. In particular, we would like to emphasize the following aspects: radio diagnostics of magneto-thermal coupling in chromosphere and corona, diagnostics of turbulence, and its role in plasma heating as well as wave propagation.

Where to stay

Perhaps the best option would be to stay in Hatfield, within walking distance from the University, or in the city of St. Albans (20-30 minutes by bus, 15-20 minutes by taxi). However, you can commute to the University from places such as Welwyn Garden City, north and central London and others. For a wider selection of hotels, see the travel sites.


Very basic options - Travelodge Hatfield - very basic option, about 10min walk

- Travelodge St Albans - basic option, about 20-30min by bus

- Travelodge Welwyn Garden (very close to Welwyn Garden City train station) - basic option, about 20-30min by bus

see prices at
Budget options - Premier Inn St Albans - about 30min by bus

- Premier Inn Welwyn Garden City - about 30min by bus

see prices at
More upmarket options - The Comet London Hatfield - about 10min walk

- Tapestry Collection Hilton St Albans - about 30min by bus
University accommodation To be confirmed...


The workshop will be held in the University of Hertfordshire (The University of Hertfordshire, Hatfield AL10 9EU, UK.)

Getting here by plane

from Luton - You can take a taxi (costing from £45-50 for private hire companies, such as Uber, one way) - 30min

- A cheaper option (around £10 one way) would be to take a train to St Albans City and then bus towards the University of Hertfordshire - 60min

- Even cheaper option would be to take a bus to Luton Town, and then bus 610 from Luton Town to the University of Hertfordshire - 90min

from Gatwick - Take a train from the airport to St Albans City (there are direct trains) and then local bus to the University of Hertfordshire (around £40 RETURN) - 90min

from Heathrow - Take Elizabeth line train, change at Farringdon, travel to St Albans City, then take a local bus to the University of Hertfordshire (around £20 one way) - 120min

- Take bus 724 from Heathrow bus station to Hatfield (around £12 one way) - 120min

from City airport - Use DLR/underground to get to Kings Cross/St Pancras, from there take a train to St Albans City (normally depart from St Pancras) or to Hatfield (normally depart from Kings Cross), then take a local bus to the University of Hertfordshire (around £20 one way) - 60-90min

from Stansted - There is a limited number of direct coach services evry day, costing from £10 one way and taking around 75min, see NX

- Otherwise, you have to take a train to London Liverpool Street, then use underground to get to Kings Cross/St Pancras, then take a train to St Albans City or Hatfield, then take a local bus to the University of Hertfordshire

NB For train times and prices, please visit see NR website

Getting here by train

Eurostar - You will arrive at St Pancras station. From there take a train to St Albans City (usually departs from St Pancras) or to Hatfield (usually departs from Kings Cross), then take a local bus to the University of Hertfordshire

Domestic - Travel either to St Albans City or Hatfield (Herts) station, then take local bus to the University of Hertfordshire

NBThere are several direct coach services every day from Oxford, Milton Keynes and other locations within UK. For times and fares please see see NX website.

Getting here by car

Parking in the University is available at extra cost. If you require parking, please contact Mykola.

For further help, please contact SOC chair Eduard Kontar or LOC chair Mykola Gordovskyy.

In case of technical problems when registering and submitting abstracts, or if you need to cancel your registration, please contact the registration support.