Relevant Conferences

This page provides a list of upcoming conferences and workshops that have EPRV-focused sessions. If you would like to see your event featured on this page, please contact us at

EPRV Splinter Session at Exoplanets IV

  • Date: May 3rd 2022, 2:30 - 5:30p PDT
  • Location: Molise Meeting Room 1-2, M Resort, Las Vegas, NV
  • Zoom Link:
  • Agenda (PDF)
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Description: This splinter session will be hybrid in format, allowing speakers and attendees to join in person or via Zoom, and does not require registration for the main Exoplanets IV conference. The session will be a combination of contributed talks and group discussions about new and evolving pathways towards achieving 10 cm/s RV detection capabilities. Presentations on all aspects of EPRV science, including but not limited to: observational efforts, instrumentation, data analysis techniques, solar studies, and stellar variability mitigation are invited. We encourage talks that showcase the nuances of current EPRV efforts, and note that presentations describing work-in-progress efforts are of particular interest.

Agenda for Exoplanets IV EPRV Splinter

Characterising Stellar Activity in thee Era of Extreme Radial Velocity Surveys of Low-Mass Planets Orbiting F-M Stars Session at Cool Stars 21

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Description: In this splinter session, we wish to focus on the spectroscopic manifestation of stellar variability, but covering a large range of spectral types (F-M), where similar processes are present but with different relative impacts on radial velocities. We will also focus on attempting to significantly improve our understanding of RV variability to enable the detection of very low-mass planets. We have therefore two main objectives: 1) The communities involved in these approaches have developed different techniques, with little exchanges between them (in particular, between solar-type stars and M dwarfs), although some processes are similar. The characterisation of stellar variability is also incomplete in both cases. For example, spot contribution is believed to be dominant in M dwarfs, with properties (lifetime in particular) that may be different from solar-type stars; however, there are indications that the inhibition of the convection in plages due to magnetic fields could play a role on long timescales even for such stars. On the other hand, the inhibition of the convective blueshift appears to play a dominant role for a star like the Sun, but many other processes cannot be neglected in the 0.5-1 m/s range, even at long timescales. Hence, it is crucial to cover a wide range of spectral types to have a more complete view of these processes, focusing here on main sequence stars, to exchange on these processes as well as on the techniques that have been developed so far. 2) Given the current challenges, it is important to have a community effort to identify the next steps and define what we need to improve our understanding of RV stellar variability. For example, future magnetohydrodynamic (MHD) simulations of these processes (3D MHD simulations of dynamos, structures such as spots or plages, convection…) will help to constrain models used to interpret RV data and build mitigating techniques based on physical conditions. We will also need inputs from other techniques (photometry for example) and/or simultaneous observations to be able to lift certain degeneracies.

Stellar Variability Session at UK National Astronomy Meeting (NAM)

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Description: Stellar variability can manifest itself as many different phenomena with a range of timescales and amplitudes, such as oscillations, granulation, starspots, plage, flares and long-term magnetic cycles. Some of these processes arise due to stellar magnetic fields which are poorly understood and notoriously difficult to measure. Studying these phenomena is, therefore, important in furthering our understanding of magnetic activity, as well as stellar inner structures and their underlying dynamo processes. Additionally, stellar variability also impacts the detection and characterisation of exoplanets and their atmospheres, as most techniques used to study exoplanets rely on indirectly detecting the signal of the exoplanet in the stellar light. Low amplitude stellar variability is the main obstacle that hinders the detection of Earth-twins in exoplanet Doppler surveys. In addition, stellar variability can bias our inference of planetary masses, sizes, obliquities, and atmospheric composition - the latter of which is particularly relevant to some of the main science goals of JWST. Ideally, we would like to see contributed talks from early career researchers and minority groups to showcase their most recent work followed by a discussion with everyone regardless of career stage. This will allow for an exchange of knowledge between different groups and an informal space to share ideas and foster collaboration. Overall, our main goal is to cover a wide variety of topics within the bigger umbrella of both stellar variability and exoplanet detection/characterisation, bringing together experts from many different groups within the UK. With the recent advances experienced in the development of precise instrumentation, stellar variability has now arguably become the main obstacle in the identification of exoplanets, as their signals can be orders of magnitude larger than the planetary ones. Understanding stellar physics is therefore crucial, particularly when searching for low-mass, long-period planets (Earth-twins), as their observable signatures are often drowned within stellar variability. This ultimately contributes to the wider picture as humanity continues its search for Earth 2.0 while understanding how planetary systems like ours were formed.