Our MSc projects are open to students from various Physics & Astronomy MSc tracks, including Astronomy & Astrophysics, Theory and GRAPPA. Students from other MSc programs such as Computer science or Chemistry can potentially also enroll in certain MSc projects, provided that they have sufficient (technical) background. 

If you are interested in a project and want more details, please contact the project advisor(s). For general questions, please contact project coordinator Dr. Alessandra Candian.

List of projects for 2025 sorted by presentation day

Mon March 31, Location: SP D1.112

Alessandra Candian 

(C4.111, a.candian2@uva.nl)

I am interested in the  evolution of  carbon-containing molecules in space and in the atmosphere of Titan. I use quantum chemistry calculations, modelling and spectroscopic observations (when available) and laboratory data. Here an idea for a projects, but feel free to propose your own ideas.

 

Project 1

How do large irregular carbon molecules break down? A computational study

Label: Computational astrophysics/astrochemistry

More than 300 molecules have been detected in space and the large majority are carbon-based. Among them we have molecules like carbon dioxide, methanol,  formamide but also larger Polycyclic Aromatic Hydrocarbon (PAH) molecules and fullerenes (C60). 

The strong UV irradiation coming from stars can dissociate these interstellar molecules providing building blocks to build new ones, initiating the so-called top-down interstellar chemistry. While the standard way to build large molecules from smaller ones (bottom-up interstellar chemistry) is well studied, the top-down chemistry is still largely unexplored.

Recent JWST observations of the Orion Bar photodissociation region (PDR) have unveiled new characteristics of Polycyclic Aromatic Hydrocarbon (PAH) molecules  astro population. In particular it seems now clear that PAHs have quite irregular shapes in the more shielded region of the PDR, and then FUV photons break them down, leaving only the most symmetric one. In this project you will explore how these irregular shapes break down using molecular dynamics simulation and identify the products of this destruction. The goal is to predict specific IR spectroscopic features that could be identified in the high-resolution JWST spectra. 

Requirements: Previous chemical knowledge is not needed.

Project 2

Investigating the hydrocarbon chemistry on Titan

Label: Experimental astrophysics/Observational astrophysics/ applied data science

Titan, the largest moon of Saturn, is a place like nowhere else in the Solar System. A dense, nitrogen-rich atmosphere, very similar to the one on Earth, is the place where very interesting photochemistry, started by solar photons, forms organic (made of C, H, N and sometimes O), molecules that are the precursors of the haze present in the atmosphere. The haze particles than "rain" on the surface where they are moved by wind to form dunes, lakes, and seas of hydrocarbons.

Understanding the inventory of molecules present in the atmosphere and how this evolves responding to the physical and chemical conditions is of great importance because Titan is one of the best places in the Solar System to look for life.

We have experimental IR spectra on proton bombardment of pure and mixed hydrocarbons (C2H2, C14H10 and a mixture of both). Both molecules have been detected in the atmosphere of Titan and are expected to “freeze” at lower altitudes, creating ice clouds. Galactic Cosmic Rays and solar wind can process this ice, leading to new chemistry,  You will analyse the experimental infrared spectra taken over a range of temperatures or over a range of proton fluences and identify the physico-chemical evolution of the ‘ices’ and their compositions (e.g. structural changes, new molecules forming).

 

Rudy Wijnands

(C4.146; r.a.d.wijnands@uva.nl) 

My primary research interests lie in studying the extreme physical processes occurring in and around neutron stars and black holes. Additionally, I investigate how these enigmatic objects form during some of the most violent explosions in the universe. My work primarily involves ultraviolet observations, although X-ray data is frequently used as well. I analyze data obtained from satellites and am also in the process of building a ground-based near-UV telescope. The projects listed below are all centered around these scientific topics. The scope and focus of each project will be tailored in collaboration with the student to align as closely as possible with their specific interests.

Project 1: Investigating Accretion Physics and Compact Objects in the Ultraviolet

Label: Observational astrophysics

This project offers the exciting opportunity to explore the fascinating world of compact objects — such as neutron stars, stellar-mass black holes, and supermassive black holes — by studying their accretion processes using ultraviolet (UV) data from the UV/Optical Telescope (UVOT) aboard the Swift satellite. You will have access to a unique dataset spanning two decades of UV observations, with new data collected daily, enabling you to investigate long-term variability, flaring events, and periodicities in these extreme systems. Using a state-of-the-art Python-based analysis pipeline developed by our research group, you will gain new insights into the accretion disks and the powerful processes that drive these cosmic phenomena. The project will focus on a specific subset of accreting systems, offering you the opportunity for in-depth independent research and contributing to the broader understanding of UV variability in some of the universe's most dynamic environments. In collaboration with me, the exact type of accreting systems will be tailored to your specific interests.

Project 2: Testing Our New Ground-Based Near-UV Telescope

Label: Instrumentation, Observational astrophysics

This project offers a unique opportunity to play a key role in testing a prototype for our ground-based near-ultraviolet (NUV; 300-350 nm) telescope, designed to study extreme cosmic phenomena such as supernovae and accretion outbursts from neutron stars and black holes. By the start of your MSc project in September, the prototype will be nearly complete, and you will assist in performing and analyzing initial test observations. These tests, which will take place in the Netherlands and potentially at higher altitudes at a site in Europe, will allow you to evaluate the telescope’s performance and assess the NUV characteristics of the Earth's atmosphere. In addition, you will conduct deep NUV exposures of celestial objects such as starburst galaxies and star clusters, focusing on their hot star populations and the dynamics of star formation and accreting compact objects.

Project 3: Exploring Atmospheric Phenomena with a Ground-Based Near-UV Telescope

Label: Instrumentation, Observational astrophysics, Atmospheric science

As an exciting and unconventional addition to my research, the NUV telescope also offers significant potential for atmospheric studies.  It can be used to investigate ozone layer variability and auroral emissions, driven by solar wind interactions with Earth's atmosphere. These atmospheric phenomena are directly relevant to human life, as the ozone layer plays a crucial role in protecting life on Earth from harmful ultraviolet radiation, while auroral emissions can offer insights into space weather, which can affect satellite operations, GPS systems, and even power grids. This unique aspect of the prototype telescope project allows you to explore the intersection between astronomical instrumentation and atmospheric science, contributing to the development of an advanced research tool. Additionally, specific observations related to these atmospheric studies may be possible, as identified by the student during the project, providing the opportunity to analyze real obtained data. We may also conduct observations of Jupiter's Aurora to study atmospheric phenomena on Jupiter and compare them with similar phenomena observed on Earth. 

 

Lex Kaper

Our research group focuses on the formation, evolution and fate of massive stars. Research projects range from the study of young massive clusters, the origin of OB runaway stars, mass loss and evolution of massive stars, high-mass X-ray binaries to gamma-ray bursts.

Project 1: On the origin of OB runaways high above the Galactic plane

Label: Observational Astrophysics

OB runaways are massive stars that travel through space with supersonic velocity. They obtain such a high velocity (up to 200 km/s) via the dynamical ejection from a young stellar cluster or due to the supernova explosion of their binary companion. With the astrometric date from the ESA Gaia mission, OB runaways and their potential parent young massive clusters can be studied in great detail. The aim of this project is to investigate OB runaways located far above (or below) the Galactic plane, up to a kpc or more. Even though they have a high space velocity, these OB runaways may not have had enough time to reach these distant locations. As most, if not all massive stars are expected to have formed in the Galactic plane, these high Galactic heights are a mystery. We will reconstruct their path, taking into account the Galactic potential. When the OB runaways explode as a supernova in these tenuous parts of our Galaxy, the impact of their supernova on the surrounding medium is much bigger than if they would have exploded in the Galactic plane. This has important consequences for the chemical and dynamical evolution of our Galaxy.

Gudmundur Stefansson

( C4.115, g.k.stefansson@uva.nl )

In my group, we are interested in the discovery and characterization of planets orbiting nearby low mass stars leveraging new technologies and multiple different techniques including the transit, radial velocity method, astrometric, and the upcoming radio method. In particular, I am particularly interested in comparing how both the physical properties and the architectures of planetary systems around low mass stars compare to the population of planets orbiting hotter stars.

Project 1: Spectroscopic and Magnetic Investigations of Gaia Candidate Exoplanets and Brown Dwarfs

Label: Observational Astrophysics

Description:

Through its astrometric monitoring of the whole sky, Gaia is revolutionizing our understanding of numerous areas of astrophysics. For exoplanet science, Gaia is expected to detect hundreds if not thousands of exoplanets and brown dwarfs at intermediate orbital distances using the astrometric technique—which relies on measuring the miniscule gravitational wobble of a star due to an orbiting companion. Some of these stars are low mass stars, but finding massive planets or brown dwarfs orbiting such stars is particularly interesting, as such companions are known to be intrinsically rare around such stars. Some such systems could also generate radio emission that can be probed with state-of-the-art facilities such as the LOFAR telescope in the Netherlands. 

We are conducting a program to spectroscopically follow-up Gaia astrometric exoplanet and brown dwarf candidates with the Habitable-zone Planet Finder and NASA NEID spectrographs in the Northern hemisphere around nearby low mass stars to confirm if those targets are compatible with the planet or brown dwarf scenario, and to rule out false-positive scenarios such as double-lined binaries. 

In this project, there are different possible routes. You could work on spectroscopic data and other supporting datasets to understand these intriguing systems with the potential to help detect rare high-value exoplanets and brown dwarfs with Gaia. There are also opportunities for more theoretical model investigations to study possible radio emission in these systems, which could be probed with LOFAR. Knowledge of python and MCMC methods for this project would be beneficial.

Anna Watts (and Yves Kini)

My research group is interested in the physics of neutron stars - the supranuclear density matter in their interiors, and the phenomena that occur on their surfaces. Over the last few years we have refined the technique of pulse profile modeling - a relativistic ray-tracing simulation and inference method that lets us measure the mass and radius of the star (which depends on the dense matter) and to make maps of hot X-ray emitting regions on their surfaces. This has given us new insights into neutron star magnetic field geometries and accretion/burning flow patterns.  

Project 1:  Complex and evolving surface patterns on neutron stars - making realistic maps.

Label: Theoretical Astrophysics

Description:  ​​Over the last few years we have used pulse profile modeling to make measurements of mass/radius and surface maps for several rotation-powered millisecond X-ray pulsars - where the X-rays come from the heated magnetic poles - using data from the NICER telescope.  We have also extended the technique to apply it to accreting and bursting neutron stars, where hotspots form as a result of channeled accretion or some kind of asymmetric thermonuclear burning.  In order to do this, we have to specify a prescription for describing the range of potential hot spot surface patterns. Right now, we use models based on overlapping circles to form uniform or two temperature regions with shapes including rings or crescents. But nature is much more complex than this! The magnetic poles of rotation-powered pulsars are likely to have smooth temperature gradients. And flame spread on the surface of bursting neutron stars will give rise to complex shapes and may leave large smooth wave patterns in the burning ocean.  

In this project you will expand our existing relativistic ray-tracing code to simulate more complex temperature distributions and shapes, and then apply it to investigate an astrophysical problem of your choice.  For example, you could look at whether the presence of temperature gradients could bias our estimates of neutron star mass and radius using NICER data. Or you could simulate flame spread on the surface of a bursting neutron star and compare this to real data, in an attempt to solve a nearly 30 year old mystery!

Thu April 3 , Location: SP D1.112

Jason Hessels & Nina Gusinskaia 

Project 1:

Label: Tests of Gravity with pulsar timing

Radio pulsars are fascinating objects that keep delivering important insights into fundamental physics after more than a half century since their discovery. Precise pulsar timing experiments have provided the most stringent constraints on alternative theories of gravity and the equation of state (EoS) of dense matter inside neutron stars. However, precision of pulsar timing is highly affected by the systematics in the timing residuals (caused by e.g. propagation through the dynamic interstellar medium) or unaccounted gravitational and astrometric effects. 

The project offers the opportunity to test gravity with a very unique triple system pulsar PSR J0337+1715. Due-to its hierarchical structure, this system is a perfect testbed for Strong Equivalence (SEP) test, directly probing gravitational interaction of a very strongly gravitating neutron star in comparison with weakly gravitating white dwarf companion with the third body. Two independent tests (Archibald et. al. 2018 and Voisin et al. 2020) have provided almost identical constraints on SEP violation, but both suffer from significant systematics. There are multiple theories as to what can cause such systematics, including a potential 4th planetary body in the system (Voisin et al. 2025). We have just a perfect dataset to test these hypotheses. Would you like to give it a try?

Jason Hessels

Project 1: Ultra-high-cadence monitoring of hyperactive repeating FRBs

Label: Observational astrophysics, Instrumentation

In this project, you will use the Westerbork RT1 single-dish radio telescope (in the Netherlands) to perform ultra-high-cadence observations of hyperactive repeating fast radio bursts (FRBs). By using a relatively small radio telescope we can afford to observe individual sources for hundreds, and even thousands of hours. A large radio telescope could never afford to do this. With this strategy we can probe the maximum energetics of FRBs, which is a key diagnostic for understanding their progenitor and emission mechanism. You will learn how to schedule observations with the telescope, perform real-time search processing, and how to analyse the burst properties to extract valuable scientific information. Because the Westerbork telescope is being upgraded with a new receiver, called ALF (Ambient L-band Feed), you can also participate in the testing and first scientific observations with that new wide-band system. For any questions, please contact Jason Hessels (j.w.t.hessels@uva.nl), with an email subject "API MSc project", or stop by C4.118.

Project 2: Enabling raw voltage recording with the Nançay radio telescope

Label: Observational astrophysics, Instrumentation

The most raw form of data that a radio telescope can provide is called "voltages". These encapsulate the electromagnetic signal properties sampled at the Nyquist rate, and normally also for two orthogonal polarisation channels. Such data provide maximum flexibility in decoding the spectro-tempo-polarimetric properties of fast radio bursts (FRBs). These properties give us information about propagation effects incurred during the bursts' journey to Earth (dispersion, scattering, scintillation, and Faraday rotation) and they allow us to study the intrinsic emission on the shortest-possible timescales and narrowest bandwidths. With the Nançay Radio Telescope (NRT, in France) we have a programme called ÉCLAT in which we regularly monitor the most active and interesting repeating FRB sources. In this project, you will learn how to schedule the telescope, search for bursts and analyse their properties to form an astrophysical interpretation, and you will help develop a new capability on the telescope to store raw voltage data when a burst is detected. For any questions, please contact Jason Hessels (j.w.t.hessels@uva.nl), with an email subject "API MSc project", or stop by C4.118.

Project 3: Finding not-so-fast radio bursts with CHIME/Slow

Label: Observational astrophysics, Instrumentation

Co-supervised with Ziggy Pleunis

Typical fast radio bursts (FRBs) have durations of only milliseconds. Recently, however, a new class of "long-period transients" (LPTs) has been discovered by exploring timescales of hundreds of milliseconds up to minutes. Time-domain astronomy is about charting how the Universe changes on a variety of timescales and it opens our eyes to previously unseen phenomena. In this project you will use the CHIME radio telescope (in Canada) to chart a new parameter space for astrophysical sources. Whereas the CHIME/FRB system searches on timescales from about 1-16 ms, you will help develop the CHIME/Slow system to search for coherent radio bursts on timescales of 16ms up to seconds. In this project, you will learn how a cutting-edge, wide-field radio telescope operates, you will help develop a real-time burst search pipelines, and you will perform astrophysical interpretation of the new discoveries. For any questions, please contact Jason Hessels (j.w.t.hessels@uva.nl), with an email subject "API MSc project", or stop by C4.118.

Project 4: Data mining of FRBs to identify distinct progenitor populations

Label: Observational astrophysics, Data science, Artificial Intelligence

Co-supervised with Daniela Huppenkothen and Ziggy Pleunis

Thousands of fast radio bursts (FRBs) have now been detected, and for each of these we can study how the radio brightness varies as a function of radio frequency and time (a so-called "dynamic spectrum"). While the physical origins of FRBs remain mysterious, we don't even know whether the bursts we've detected all come from the same type of astrophysical source. Both repeating and apparently non-repeating FRBs have been found. Do they have fundamentally different physical origins, like long and short gamma-ray bursts, or are the apparent non-repeaters simply less active sources that will eventually be seen to repeat? Likewise, the all-sky rate of FRBs is far too high for them to all originate from cataclysmic events (like the merger of compact objects), but we don't yet know whether some small fraction of the observed FRBs are associated with cataclysmic explosions. In this project, you will use advanced machine learning techniques to decipher and classify FRB dynamic spectra to investigate whether there are trends and hints at multiple populations of bursts. For any questions, please contact Jason Hessels (j.w.t.hessels@uva.nl), with an email subject "API MSc project", or stop by C4.118.

Sera Markoff

Project 1:  Better understanding black hole astrophysics

Label:  theoretical/computational astrophysics 

Within my group we do a wide variety of projects relating to black holes (and sometimes neutron stars!), particularly focusing on questions relating to their relativistic jets, particle acceleration and multiwavelength emission properties.  The more numerical side of the group uses and develops our in-house general relativistic magnetohydrodynamics (GRMHD) GPU-accelerated code H-AMR together with GR ray-tracing codes (a new one is in development in Julia, PICASSO) to model and interpret data from the Event Horizon Telescope, both alone and together with multiwavelength data.  The more semi-analytical side uses and develops our leptonic/lepto-hadronic jet models “BHjet and HADjet” to better understand the physics via modelling multiwavelength data from a wide variety of objects.  

I prefer to meet with students and customise a project to their interests and skills they would like to learn, so do not have ‘pre-defined’ projects but will give some examples and ideas during my short presentation.

Ziggy Pleunis

I co-lead the AstroFlash research group with Jason Hessels, and I am particularly interested in using fast radio transients as astrophysical tools to study the Universe at large, which is possible as each radio transient signal holds a record of the magnetized gas it has travelled through. We’re currently mostly interested in unraveling the origins of fast radio bursts (FRBs), luminous flashes of us–ms duration that are detectable over extragalactic distances. 

Project 1: Choose your own FRB adventure with CHIME/FRB and its Outriggers

Label: Instrumentation, Experimental astrophysics, Observational astrophysics

CHIME/FRB is the current most powerful FRB discoverer in the world, detecting about 3 FRBs/day. We are on the verge of releasing our second catalog of FRBs with over 3500+ sources, and we have recently upgraded our experiment with three Outrigger stations that will again revolutionize the field by allowing subarcsecond localization precision on one-off FRBs, letting us associate those FRBs to within their host galaxies and unlocking them as more precise astrophysical tools as we can measure the host galaxies’ redshifts through optical follow-up observations. Within CHIME/FRB there are many possibilities for a MSc project, e.g. focusing on some aspect of the data analysis, a subset of interesting FRBs or commissioning and early science of the Outriggers upgrade. Come talk to me about your interests and we can come up with a MSc thesis project together. There are also opportunities for cosupervision here. For example, if you’re interested in a combination of data science and radio astronomy, we can work together with Daniela Huppenkothen.

Project 2: Unlocking polarization information for all fast radio bursts detected by the Nancay Radio Telescope

Label: Observational astrophysics

Description: Fast radio bursts (FRBs) are very brief pulses of radio waves that originate from other galaxies. Of the thousands of unique sources of FRBs that have been detected, a few dozen are also known to repeatedly emit bursts. Currently, we do not exactly understand which astrophysical objects produce FRBs, or how. Some of the most promising theories suspect highly magnetized neutron stars are the culprit.

The strong magnetic fields of these candidate progenitors, as well as the potentially violent and turbulent environments surrounding them, can drastically alter the observed polarisation properties of FRBs. By studying these polarisation properties, and how they evolve over time and with observing frequency, it is possible to indirectly infer properties of the local environment or progenitor, even though these sources are situated millions to billions of lightyears away!

Over the past few years we have been using the Nançay Radio Telescope (located south of Orléans in France) to regularly monitor a dozen repeating FRBs sources.  The NRT is the second most powerful radio telescope in Europe, and all the observations have incredible time resolution (16 microseconds) and full polarisation information. In this project, the student will take charge of developing the polarisation pipeline for the NRT, with the aim of determining how the Faraday rotation measure, polarisation angle and polarisation fraction of repeater bursts vary over months to years timescales. The student will gain familiarity with transient radio astronomy, polarimetry, and obtain hands-on experience developing a pipeline for one of the largest radio telescopes in the world.

This project will be cosupervised by postdoctoral researcher Dr. Danté Hewitt.

Project 3: A first search for ultracool dwarfs with the CHIME telescope

Label: Observational astrophysics, Theoretical astrophysics 

Description: Magnetic fields play a key role throughout the lives of planets, shaping their formation and atmospheric escape. At planetary scales, magnetism is driven by the motion of electrically conductive material in their interiors. Therefore, magnetic fields are a unique probe of a planet's interior structure. In our solar system, planetary magnetic fields are signposted by their bright radio emission, driven by electrons trapped within the magnetic field. Despite extensive searches, radio emission from an exoplanet has so far eluded detection. As a result, our understanding of magnetism on extrasolar planets is in its infancy. 

While exoplanets remain undetected at radio wavelengths, Jupiter-like objects known as ultracool dwarfs (UCDs) have been detected at radio wavelengths for over two decades. These objects share many structural similarities to Jupiter, and are therefore ideal targets for advancing our understanding of magnetic fields on Jupiter-like exoplanets. In this project, the student will take charge of a novel search for UCDs at radio wavelengths using the CHIME telescope, which has a large 200 sq. deg. field of view in which 1,024 beams are formed. As UCDs have yet to be detected in the 400–800 MHz frequency range where CHIME is sensitive, this project will open a new window of study for these objects.

Parallel to implementing a search with the CHIME telescope, the student will work with theoretical astrophysicist Rob Kavanagh (ASTRON/UvA) on characterising the magnetic fields of the UCDs using the observational data gathered during the project via numerical models. 

This project will be co-supervised by postdoctoral researcher Dr. Rob Kavanagh. 

Jakob van den Eijnden

I am a Marie Curie fellow in the massive stars group, focusing on the energetic processes powered by massive stars and in particular, their winds. These processes can take place on a range of scales – in their direct surroundings, for instance in binaries with a compact object, the interstellar medium around a single massive star, or in stellar clusters hosting an entire population of massive stars. Depending on your interests, your project can focus on any of these scales and their related questions. All options will be co-supervised with Lex Kaper, and will include additional API and non-API researchers to discuss with on a semi-regular basis. 

Project 1: The energetic impact of massive stars in binaries and beyond

Label: Observational astrophysics

Description: Massive stars may be rare, but play a crucial role in a wide range of astrophysical processes. Throughout their lifetime, these stars launch powerful stellar winds that can release the equivalent mechanical energy of a supernova into their surroundings, albeit on a longer time scale than the supernova explosion. These winds power numerous highly energetic processes, such as accretion and jet launching in binary systems, and the formation of particle-accelerating shocks in the interstellar medium. While both those processes have been known for a long time, we are only now able to study these effectively in the radio band: the advent of sensitive radio telescopes such as MeerKAT in South Africa and ASKAP in Australia allows us to study massive stars in accreting binaries, as well as the shocks they drive in the ISM, at the lowest frequencies. 

For this MSc project, I like to match your interests in terms of topic and type of research. The project can either focus on (A) radio observations of the massive star in accreting binaries (BP Cru and Vela X-1, specifically), where you will observe and model the complex interaction between the stellar wind, accreting neutron star, and jet, along the orbit. Alternatively, (B), you can focus on detailed data analysis and modelling of ISM shocks around a small number of massive stars, aiming to find the first detection of such shocks at 5.5/9 GHz and predicting (the detectability of) their high-energy (X-rays/gamma-rays) emission. Finally, (C), there is the option to systematically search for and characterize the ISM shocks around a large number of massive stars. You will use these shocks as tracers of the interstellar medium in and around clusters of stars, and understand if the ISM conditions are favorable for cosmic ray acceleration in these clusters. 

 

Daniela Huppenkothen

Project 1: Teaching AI to read the light of the most massive stars (with Alex de Koter)

Label: Applied Data Science/Observational Astrophysics

The evolution of massive stars toward their supernovae and remnant compact objects is poorly understood, especially for very massive stars with initial masses >100 solar masses (e.g., Brands et al. 2023). How do these stars evolve? What are their supernova progenitor properties and resulting supernova characteristics? How massive are the black holes these stars leave behind? 

We explore these questions by analysing the emitted light of stars, which allows us to characterize their properties. In turn, confronting stellar evaluation models with these measured properties of many stars helps us constrain the physics that controls the lives of stars, hence furthers our understanding of the way stars evolve and end. Progress is severely hampered by the complexity and CPU-intensive nature of spectral analysis, a problem that is particularly urgent given upcoming large-scale spectroscopic surveys planned for WEAVE/WHT, 4MOST/VISTA, and later MOSAIC/ELT, which will produce thousands of spectra of massive stars in galaxies in the Local Group and beyond.

In this MSc project, we will develop a neural network (NN) approach to predict the spectra of massive stars. Exploratory NN-predictions of the spectra of these stars considering five stellar properties (5D: temperature, gravity, radius, mass-loss rate, helium-to-hydrogen abundance) have yielded very promising results. Higher dimensional analysis (considering many more stellar properties) now needs to be developed, tested, explored and optimized. Developing a versatile and robust NN methodology for massive stars in the range 8-300 solar masses is the goal of this project. This is a great project for a student who’s excited about stars and interested in delving deeper into how we can use machine learning in astrophysical modelling, and would like to tinker with some neural networks.

Project 2: Cutting-edge statistical inference for massive stars (with Alex de Koter)

Label: Applied Data Science/Observational Astrophysics

Massive stars emit copious amounts of ionizing radiation, feature powerful stellar winds, and end in highly energetic supernova explosions. Their cumulative feedback effects control an important part of the evolution of their host galaxies. Massive stars are characterized through quantitative spectroscopy, i.e., through analysis of the light they emit. Currently, spectroscopy uses genetic algorithms to fit spectral models to data. However, we now have access to a pilot neural network surrogate model for the physics model, which enables the use of state-of-the-art statistical algorithms for model fitting, which are expected to be dramatically faster than previously used approaches. In this project, we first develop a spectral fitting approach using this pilot neural network to predict stellar spectra. The new spectral analysis method will then be applied to the full X-Shooter/VLT (XShootU) optical and STIS/HST (ULLYSES) ultraviolet datasets, programs in which over 250 massive stars in Local Group galaxies have been studied. In this way, we achieve the largest homogeneous analysis of massive stars to date. Confronting their stellar properties to predictions of stellar evolution will yield important new insights regarding the physics of, a.o., rotation, core-overshooting, and mass loss. In the context of this project, we will focus on one of these physical processes for the most massive stars in the sample, to be decided when the analysis is concluded. 

A statistical inference methodology relying on neural-network generated stellar spectra is anticipated to be significantly faster than the current state-of-the-art methods of spectral fitting. This is a timely problem given upcoming large-scale spectroscopic surveys planned for WEAVE/WHT, 4MOST/VISTA, and later MOSAIC/ELT, which will produce thousands of spectra of massive stars in galaxies in the Local Group and beyond. This is a great project for a student who is curious about stars, and interested in exploring cutting-edge approaches to statistical modelling, including probabilistic programming.

Project 3: Searching for Magnetar Starquakes in NICER data

Label: Applied Data Science/Observational Astrophysics

Magnetars are among the most extreme objects in the universe. They are neutron stars with extreme magnetic fields, and show short X-ray bursts with energies otherwise only seen from accretion events or stellar explosions. The detection of rare oscillations in a few of their X-ray light curves opened up the potential of neutron star seismology: exploring the interior of the star through these oscillations. However, these oscillations are rare and difficult to find, and require new statistical approaches. In this project, we will look for oscillations in observations taken with the X-ray telescope NICER, using a recently developed statistical technique. This project would be great for someone who is curious about delving deeper into time series analysis and excited about high-energy astrophysics. 

Fri April 4 , Location: SP A1.24

Julia Bodensteiner & Sarah Brands

Project 1: The most massive stars

Label: Observational astrophysics

Description

Massive stars strongly impact their surroundings and drive the evolution of their entire host galaxies. In particular, both the chemical and mechanical feedback they provide are dominated by the most massive stars that are present. Despite their importance in models and predictions, which have a large impact on many different aspects of modern astrophysics, it remains unclear how massive the most massive star can become.

In this MSc project, we want to revisit the most massive stars known to date, which are situated in the core of R136, the so-called "Tarantula Region", in our neighboring Galaxy, the Large Magellanic Cloud. To reassess their masses, which were previously reported to be way above 150 x the mass of our own Sun, we will use a novel dataset obtained with the ERIS integral-field spectrograph at the Very Large Telescope in Chile. Using the unprecedented spatial and spectral capabilities of ERIS, which operates in the near-infrared, to obtain high-quality spatially resolved spectroscopy of the most massive stars, crucial to characterize the stellar parameters and put stringent constraints on their stellar mass.

Requirements: previous knowledge on stellar atmospheres and spectra is beneficial, but not required. Proficiency in python will be useful in the project.

Joe Callingham

Project 1: Why are you so bright radio star? 

Label: Observational Astrophysics

Magnetospheric processes seen on gas giants such as aurorae and circularly polarized radio emission have recently been detected coming from radio stars. This is unexpected. In this project, you will characterise the types of stars we have detected, understand the origin of their radio emission, and model the type of magnetic fields that are necessary to drive such emission. Through you will gain experience in using Python, supercomputers in reducing LOFAR and GMRT data, and will complete regular visits to ASTRON (Netherlands Institute for Radio Astronomy). 

Mon April 7 , Location: SP D1.112

Jacco Vink

I work on hot plasmas and nonthermal X-ray and gamma-ray emission from supernova remnants and other high-energy sources.

Project 1:does hot plasma supports strong shock wave around stellar clusters?

Label: Observational astrophysics

In the Milky Way there are energetic sources accelerating particles (electrons, protons, helium nuclei and other) to energies of at least 3 PeV. Supernova remnant shocks seem in general not to be able to accelerate to these energies. New gamma-ray data suggest that perhaps stellar cluster can do that, but we do not know how and where? Is it the cluster itself, the shock surrounding it, or the even larger bubble created by the stellar cluster? 

In this project we will look for the energetics of a well-studied and very energetic cluster, Westerlund 1, in X-rays. We will study the diffuse emission created by colliding stellar winds. In particular we are interested in the energy contained in the hot gas, and whether this can drive strong enough shocks for particle acceleration. We will also look at the dynamics of the gas by probing the equilibration properties of the hot gas. The project will use a new deep Chandra X-ray observation.

Project 2: Investigating IR synchrotron radiation from Cassiopeia A using JWST data

Label: Observational astrophysics

Cas A is a young (350 yr) well studied supernova remnant in the Galaxy. The accelerated electrons can be studied using synchrotron radiation, which can be detected from radio to X-ray wavelength, caused by respectively GeV to 10 TeV electrons, spiraling in a magnetic field of 100-500 micro-gauss. However, the higher the energy of the electrons, the fast they lose their energy. In X-rays the electrons lose their energy in 10-20 yr, in the radio the loss time scales are much longer than the age of Cas A. The infrared is interesting, as the electrons lose their energy in 50-300 yr. We therefore expect gaps in the IR synchrotron maps, depending on how old that part of the remnant is and what the magnetic-field strength is.

For this project we will study high resolution JWST data of Cas A, in particular taken with the NIRCAM instrument. A particular band is dominated by synchrotron radiation. We will quantitatively compare these NIRCAM maps with radio and X-ray maps in order to probe the age of the synchrotron emitting regions and constrain the magnetic-field properties.

Project 3: Project 3: a pilot project to detect supernova light echoes

Label: Observational astrophysics

Supernovae are extremely bright for a few weeks, so bright that some light that scatters of dust clouds can still be detected several hundred years after  the light of the explosion reached us directly. We call these scattered lights “light echoes”. Since the light is scattered it should be polarized. In the near future a 2.6 m telescope with a 1x1 degree field of view, the VST, will be have a polarization detector. The Netherlands will be involved in this instrument. In the future the UvA is planning to use VST for ligh echo studies. But we can already start now: Previous surveys with this instrument did not have polarization data, but should still have detected light echoes. We will use the archival data, stored in Groningen, to hunt for light echoes, and other transients by comparing multiple observations of the same field.

This project is in collaboration with Gijs Verdoes of Kapteyn Institute Groningen.

Oliver Porth

My group works on simulations of relativistic plasma, with primary applications to X-ray binaries and EventHorizonTelescope targets. We are interested both in fundamental physical mechanisms and in modeling of global systems, where we focus on black hole and neutron star accretion (in particular using general relativistic magnetohydrodynamic simulations). If you have a project idea that fits into this scope, just talk to me or join one of our group meetings, sometimes the best projects start like that…

Project 1: Three-dimensional simulations of accreting neutron stars

Label: Computational astrophysics

With Pushpita Das (Columbia/NY)

Neutron stars are the densest objects in the universe and a unique laboratory to study the fundamental physics of ultra-dense matter and strongly curved spacetime. Some neutron stars called “accreting millisecond X-ray pulsars” are particularly interesting targets since we can in principle use their rapid pulsed X-ray emission to constrain mass and radius of the neutron star. However, to do this in practice, we first need to understand the complex interplay between 3D geometry, gravity, gas and magnetic fields that leads to the pulsed emission. While a lot of work has been done for accreting black holes, the field of magnetized neutron star accretion is still wide open. Recently, we showed how jets are launched and collimated by the surrounding accretion disk and we looked at the properties of the pulsed emission. But there is a lot more to be done: we want to know “what happens to the jet and the hotspots in misaligned disks?” “How does the accretion column and hotspots change when the disk becomes thin?” In this master project, you will try to answer these questions by extending an existing numerical setup, and by running and analyzing large 3D simulations on a supercomputer. If you are into computational high-energy astrophysics, this might be a good project for you!

Project 2: Radiative GRMHD simulations of accreting neutron stars
Label: Computational astrophysics

One of the prevailing cosmic mysteries are the Ultra-luminous X-ray sources (ULXs). These strong X-ray sources are too bright to be explained by (sub-Eddington) stellar mass compact objects (black holes or neutron stars) which has led to much speculation about what they can be. Detection of pulsed emission from some ULXs now indicates that at least some of them are neutron stars, seemingly accreting at super-Eddington rates. In this project, you will use a newly developed radiative general relativistic magnetohydrodynamics code (rad-GRMHD) to investigate the dynamics of accretion onto magnetized neutron stars under the influence of strong radiation fields. The simulations can help to answer important questions regarding which level of super-Eddington rates can be achieved, how much the radiation is beamed, how strong magnetic fields change the picture and how the electromagnetic spectrum looks like as a function of the viewing angle. This research line is quite novel which leaves a lot of room for discovery!

Phil Uttley

Project 1: Probing the regions close to accreting black holes with X-ray spectral-timing

Label: Mainly observational astrophysics w. some theoretical astrophysics & applied data science depending on the project and preferences of the student

X-ray spectral-timing is a technique which combines X-ray spectral information with the rapid variability shown by accreting black hole X-ray binaries on time-scales of seconds or less, to probe the innermost emitting regions - the disk and corona - close to the black hole. This project uses data from advanced X-ray telescopes NICER and HXMT to study these inner regions with spectral-timing and the physical models that can describe this kind of data. The project mainly involves X-ray data analysis but also in combination with model-fitting of the data. The data is so rich that the development of new analysis methods is also possible and it is possible to tailor the project to emphasise more the theory and model-development, or data-science aspects, depending on the interests of the student.

Project 2: X-ray variability states across the black hole mass-scale

Label: Applied data science, observational astrophysics

Accreting stellar-mass black holes in X-ray binary systems show distinct patterns of short-term variability, described by their Fourier spectra, which map directly on to the accretion ‘state’ of the system. It is of great interest whether these states also exist in accreting supermassive black holes in Active Galactic Nuclei (AGN), because this could help to explain why some AGN produce powerful jets or winds, which can sculpt the formation of galaxies and galaxy clusters. In this project you will use a state-of-the-art Gaussian process method to measure Fourier spectra of a sample of ~20 AGN with X-ray light curves covering time-scales from minutes to years. With this approach you will obtain the first unbiased view of whether or not AGN show the same X-ray variability states as XRBs, as well as measuring the AGN black hole mass directly from the characteristic variability time-scales.

Thu April 10 , Location: SP D1.112

Erik Kuulkers

Project 1: X-ray astronomy before you were born

Label: mix of experimental & observational astronomy plus applied data science

Almost 50 years ago, on 30 August 1974, Holland’s first astronomical satellite was launched: the Astronomical Netherlands Satellite, ANS. It was the first 3-axis stabilized X-ray/UV satellite (and so could stay on target for minutes to hours periods of time). Also, the on-board computer was the first European first reprogrammable digital computer flown in space. One of the instruments onboard was the Soft X-ray eXperiment (SXX), build by SRON Netherlands Institute for Space Research, sensitive to X-rays with energies between 0.2 and 7 keV (2-70 Å). It observed many exotic objects from 1974 to 1976, which were discovered at the time, ranging from binaries containing a compact object (white dwarf, neutron star or black hole) to flare stars to supernova remnants. For example, one of the sources observed of my interest was Cygnus X-1, a black-hole X-ray binary discovered in the 1960’s. The ANS data enable us to compare these early results with those of much later measurements and interpret them in light of what we know nowadays, and extend the long-term baseline for characterizing state change behaviour in Cygnus X-1. X-ray states in X-ray binaries are mainly defined by their spectra and timing behaviour; these states correspond to different accretion regimes of the compact object. So, the ANS data are not only of historical value!

The data from the SXX were only available on microfiche (!). They have been digitized and OCR’ed last year, and a manual (intensive) inspection of the data is ongoing. The instrument provided X-ray count rates in 7 channels. To get a handle on the absolute X-ray luminosity and emission spectral shape, the response of the instrument is needed. This response has been determined using on-the-ground and in-flight calibrations; the results are provided in the PhD thesis of A.J.F. den Boggenende (1979). The idea is to translate the info in the thesis into a response file, which can then be used to properly analyse the early exciting data of Cygnus X-1 again.

Nathalie Degenaar (C4.120, degenaar@uva.nl)

In my group we mostly study X-ray binaries: neutron stars or black holes feeding off their companion star. Using novel analysis techniques applied to data at X-ray, UV, optical, nIR and radio wavelengths from state-of-the-art observing facilities, we use X-ray binaries to study i) neutron star physics, ii) accretion physics, iii) jets and winds, iv) thermonuclear explosions, v) their impact on their environment. For this year, I have the following MSc projects in mind.

2025 Project 1: A cosmic cannibal seen through the eyes of a new X-ray telescope

In 2023 September, the high-resolution X-Ray Spectroscopy Mission (XRISM) satellite was successfully launched as a joint effort between the Japanese and American space agencies (JAXA and NASA). It provides unprecedented spectral resolution that has opened up a completely new parameter space to study hot plasma found near black holes and neutron stars. In this MSc project, you will be using some of the very first XRISM spectral data obtained, to study the hot plasms surrounding the neutron star X-ray binary 4U 1916-053. You will model these with state-of-the-art models to have a fully new and detailed investigation of the properties and location of the plasmas. This is expected to unravel new secrets of how neutron stars and black holes swallow gas and blow some of this back into space. This project will be co-supervised between Dr. Nathalie Degenaar (API) and Dr. Elisa Costantini (SRON), in collaboration with Dr. Maria Diaz Trigo (ESO).

Label: Observational astrophysics

2025 Project 2: Winds of change, an illustrious neutron star revisited

(joint with Rudy Wijnands from API and Stefanie Fijma from ESO)

Cygnus X-2 is one of the brightest X-ray sources in the sky. It shines so bright because it consists of a neutron star that is swallowing gas from a nearby star. While this so-called X-ray binary has been discovered decades ago and studied extensively with many X-ray satellites, much remains to be discovered about the table manners of this cosmic cannibal. In this project, you will perform the first detailed UV analysis of this neutron star using unpublished data obtained with NASA’s Hubble Space Telescope. This is expected to shed new light on how gas is transferred and ejected into space by this illustrious X-ray binary. This project will be co-supervised between Dr. Nathalie Degenaar and Prof. Rudy Wijnands (API), in close collaboration with Dr.-to-be Stefanie Fijma (ESO).

Label: Observational astrophysics

2025 Project 3: Scrutinizing an X-ray puzzle for the love of neutron star physics

Neutron stars in X-ray binaries spend long stretches (years) of time in quiescence, during which they must be accreting little or no matter. Apart from thermal X-ray radiation produced by the hot glowing neutron star, often a more energetic X-ray emission component is detected too, but its origin remains unknown. Is it coming from a residual accretion stream or is it produced by the magnetic field of the neutron star? Answering this question is crucial to know if we can determine what these neutron stars look like on the inside, which is one of the core pursuits of modern astrophysics. In this project, you will analyse X-ray data from the Chandra and XMM-Newton satellites of a large sample of quiescent neutron star X-ray binaries to scrutinize this long-standing puzzle.

Label: Observational astrophysics

2025 Projects 4 & 5: Cosmic explosions shedding light on long-standing mysteries

Relativistic jets produced by black holes and neutron stars play an important role in shaping our universe, from impacting the formation and evolution of galaxies, to regulating the spin evolution and mass growth of compact objects, to potentially enriching the cosmos with high-energy particles and exotic elements. Nevertheless, it remains largely unknown how jets are launched, and what their physical properties such as their speed, power and composition are. The recent discovery that thermonuclear explosions on the surface of neutron stars produce observable changes in their jet offers a very exciting, completely new opportunity to perform dynamical studies that can unravel the secrets of jets. Within this topic, several projects are possible, working either with multi-wavelength observational data (project 4), or developing a code to test if there are traces of exotic elements in the cosmic surroundings of neutron stars that may have been deposited there by their jets (project 5). The second option would require a high level of independence and creativity in determining how to approach this.

Labels: Computational astrophysics (project 5), Observational astrophysics (project 4)

 

2025 Project 6: Can we reproduce astrophysical jets in the lab?

Ultimately, the relativistic jets seen from black holes and neutron stars must be produced in an interplay between numerous complex and non-linear physical processes in extreme gravity. Several such processes are not captured by astrophysical observations, while it is essential to have constraints to allow for numerical simulations. An exciting, yet fully unexplored possibility is that we may obtain such constraints from nuclear plasma experiments in the laboratory. In  this MSc project you will explore which parts of the jet can possibly be simulated in the lab. This will be a joint effort with the nuclear physics laboratory ARCNL that is located at Science Park. This project will be co-supervised between Dr. Nathalie Degenaar and Dr. Oliver Porth (API) and Prof. Oscar Versolato (ARCNL).

Label: Theoretical/Experimental astrophysics

2025 Project X: Tailored project on multi-wavelength studies of X-ray binaries

Within the overarching theme of “observational studies of accreting neutron stars and black holes” there is a wealth of possibilities for exciting projects using data from different wavelengths and applying different analysis techniques. I’m happy to discuss projects tailored to your particular interests or learning goals.

Label: Observational astrophysics

 

Carsten Dominik

Project 1: Dust opacities of fractal aggregates as layers spheres

Label: computational astrophysics

Planet formation primarily uses the dust particles suspended in the gas disk circling young stars. The first step toward planet formation is the formation of large fractal aggregates of these dust grains.  They hit, and stick like that. The aggregates are fractals with a fractal dimension of about 1.5. Such aggregates are denser in the center, but then the density decreases outward, to extremely low values. We want to know what these look like when they are interacting with light in the planet-forming disks. Usually a very rough approximation is being used, there the aggregate is models as a sphere with just an average density, completely ignoring the actual structure.  A better approximation would be to treat the aggregated as a layered sphere with different densities in each layer. The goal of the project it to implement that approach and to compare it with several other approximations. The project will contribute to bringing the critical stages of planet formation into view.

Project 2: SPH code for computing collisions of planetesimals

Label: computational astrophysics

In planetary science, SPH cods are sometimes used to model the collisions of solids like planetesimals, despite the fact that SPH was made for computing hydrodynamics. I would like to understand better how SPH can be used to model solid bodies and what the limitations are. Therefore, I am offering an exploratory master project to procure such a code, study it and learn how to use it, and then apply it to collisions of planetesimals while they are growing to form planets.

Project 3: Dust production during the earliest stages of a debris disk

Label: computational astrophysics

In a recent paper (https://ui.adsabs.harvard.edu/abs/2024A%26A...687A.109S/abstract) we have shown that at the critical moment when the amount of gas in a planet-forming disk is reduced and about to disappear, small planetary embryos and planetesimals can already collide and start the creation of a debris disk. In these disks, the dust is not primordial, but secondary.  It has been processed in a planetesimal and now re-appears as small grains that are visible. In the paper mentioned above, the relevance of this process was proved.  What is missing is a proper numerical model that self-consistently tracks dust production, stirring of planetesimals and settling and re-coagulation of dust in this situation. This will lead to a concrete prediction of observable properties of such early debris disks. I used to think that this might be for a PhD project, but I do now think that it is possible to build such a model in wa very ambitious master project. Any takers?

 Elisa Costantini (e.costantini@sron.nl)

Project 1:

Label: observational astrophysics

This project will investigate the complex nature of outflowing winds from a bright supermassive black hole, by means of high resolution X-ray spectroscopy and timing. You will learn about data analysis and modeling of the primary radiation of the accretion disk around the black hole as well as the chemical and physical characteristics of the photoionized gas as it varies with time. Multi-phase outflows are important in the so-called feedback process, as winds influence the growth of the host galaxy. This source has been observed by XRISM, the brand new Japanese satellite, launched in 2023, which is providing transformational results on outflowing winds.

Project 2:

Label: observational astrophysics and experimental astrophysics

Interstellar dust particles constitute the building blocks of  planetary systems and rocky planets like our own. The initial conditions for a system formation are therefore very important in understanding its fate. X-rays are a powerful tool to study a large variety of interstellar environments, from diffuse media to molecular clouds. This project is multidisciplinary. On the one side you  will study astronomical data of dust features from the brand new satellite XRISM. On the solid state physics side, you will analyze high resolution data collected at the Soleil synchrotron.
 

Wed April 16 , Location: SP D1.112

 

Ralph Wijers

Project 1: How can gamma-ray bursts happen in constant-density environments?

Label: GRB-constant

advisor: Ralph Wijers; co-advisor: Antonia Rowlinson

When a long gamma-ray burst explodes at the end of the life of a massive star, we can deduce the density profile of the circumstellar medium from the way the light curve of the GRB afterglow declines. From the behaviour of the light curves, we infer that GRB afterglows appear to be about equally divided between cases where the density is uniform, and where the density declines as 1/r^2, as one would expect from a stellar wind. Simple calculations however show that the uniform case should be occur only rarely, if ever. So what is going on?

In this project you will explore, partly analytically and partly computationally, the interaction between the wind of a massive star and its environment, and see what kinds of conditions are needed to allow uniform circumstellar media to be seen in GRB afterglows. Interest in massive stars and GRBs is helpful, and no particular aptitude for computational work is required.
 

Tjarda Boekholt & Silvia Toonen

Project 1:: Modeling tidal capture of satellites by terrestrial planets

Label:  Computational astrophysics

Description:

The role of a moon in the development of life on a habitable planet remains an open question.

On Earth, our Moon drives periodic tides and may help stabilize the planet's obliquity.

If the Moon had been significantly smaller or in a different orbit, the evolution of life might have taken a drastically different trajectory—or perhaps not occurred at all.

Current research on habitable exoplanets primarily focuses on their detection and atmospheric characterization.

However, it is equally important to investigate the potential formation histories and properties of exomoons orbiting these planets.

While Earth's Moon is thought to have formed through a giant impact, other formation mechanisms are hypothesized to contribute to the diversity of exomoon populations.

This project aims to conduct a numerical study on the tidal capture of satellites by terrestrial planets.

Utilizing the new N-body code TIDYMESS (Boekholt et al., 2023), the project will simulate and analyze a comprehensive set of dynamical histories.

By measuring capture probabilities and examining the theoretical distribution of the structural and orbital properties of exomoons,

this study will contribute critical insights into the detectability of exomoons and their potential influence on the habitability of exoplanets.
 

Project 2: Modeling gravitational wave capture in AGN disks

Label: Computational astrophysics

Description:

The discovery of gravitational waves has revolutionized our understanding of the Universe, providing a unique observational window into cosmic phenomena.

The observed rates and properties of gravitational wave sources impose stringent constraints on their astrophysical formation channels.

While theoretical studies have demonstrated the role of stellar evolution and dynamics in stellar systems in forming gravitational wave-emitting compact binaries,

an emerging scenario considers the capture of stellar-mass black holes by active galactic nucleus (AGN) accretion disks.

In this scenario, stellar-mass black holes from the galactic nucleus gradually align with the AGN accretion disk, forming a dynamic population of black holes within the disk.

Processes such as disk migration and orbital resonances can lead to close encounters between black holes, resulting in gravitational wave capture events.

This project aims to investigate the dynamics of black hole capture in the AGN channel through numerical simulations.

Utilizing the new N-body code TIDYMESS (Boekholt et al., 2023), the project will generate and analyze a comprehensive set of dynamical histories.

By measuring capture probabilities and examining the theoretical distribution of gravitational wave binaries and their signals,

this study will contribute towards understanding the role of the AGN channel to the cosmic rate of gravitational wave events.
 

Antonia Rowlinson

Project 1: Hunting for variable sources in commensal surveys with LOFAR and looking towards LOFAR2.0

Label: Observational Astrophysics & Applied Data Science

Radio transient astronomy has taken off during the past decade, thanks to excellent new radio telescopes coming online and increases in computational power. Exciting detections of strange sources that still need identifying have been made including the Galactic Burster, a LOFAR transient, dispersed transients by AARTFAAC and the new population of long period Galactic transients thought to be magnetars or extreme white dwarf systems. However, this just the tip of the iceberg – there are likely to be many variable sources lurking in the data that our search strategies currently miss.

We have developed a wide range of techniques to search for these unexpected variable sources. Most importantly, we developed the LOFAR Transients Pipeline to search large numbers of fits images. This pipeline is currently undergoing a huge overhaul to enable it to automatically handle the massive datasets we expect it to handle in the future.

LOFAR is also currently undergoing a big upgrade to LOFAR2.0, which we expect to come online in 2026. Our transient detection pipeline will run fully automatically on the majority of the LOFAR2.0 observations, giving the opportunity to find new and exciting sources within days.

This project will use large amounts of LOFAR observations to conduct a survey for variable sources using the new Transients Pipeline. You will develop techniques to automatically filter artefacts (such as removing extended sources) and new methods to pull out unusual sources. You will also use commissioning data from the LOFAR2.0 pipelines to characterise the data ready for the large automated data influx from LOFAR2.0.