Find a PhD Project Here
Opportunities for fully funded PhD or EngDoc research projects are available in all fields of research within the School. You may search for current projects on this page. APPLY HERE for a PhD Place.
Search current PhD opportunities in the School of Physics & Astronomy:-
Cloud formation has become a major stumbling stone for understanding planetary atmospheres. Clouds leave a trace of an individually depleted gas which determines the spectral appearance of the planet/Brown Dwarf as well as it does influence the dynamic behaviour of the atmosphere. The complex interaction between clouds and their surrounding gas has lead to a oversimplification in present retrieval approach resulting in a large uncertainty regarding the physical meaning of the retrieved cloud parameters.
Using the detailed model of dust formation developed by Woitke & Helling in a 3D atmosphere simulation, possible topics include:
1) Atmosphere's response on planetary evolutionary events
like volcanism, dust/gas accretion, mass loss during star-planet interaction
2) 3D atmosphere simulations for transiting planets like WASP43b, the M-dwarf planet GJ1132b, or the radio active planet HAP-P-11b.
The student will work with Dr Christiane Helling as part of the LEAP group.
http://leap2010.wp.st-andrews.ac.uk/ Please contact Ch Helling for more details.
Recent studies of the magnetic fields of very low mass stars shows a strange and so far unexplained behaviour. Some have strong, simple magnetic fields, and some have much weaker, complex, solar-like field magnetic fields. We do not fully understand why this difference occurs, but this project involves using the maps of the magnetic fields of these star to explore the physics of their coronae and winds and to examine the impact on any orbiting planets.
Many solar-like stars show cool, dense clouds of gas trapped within the million-degree plasma of their outer atmospheres (or coronae). These so-called ``slingshot prominences'' carry away angular momentum when they are ejected and also are also responsible for mass-loading of the stellar wind. As a result, they may form an important part of the spin-down of young stars, and their impact on orbiting planets may lead to enhanced stripping of the planetary atmosphere.
A main diagnostic of the particle dark matter is its annihilation rate, which depends sensitively on the dark matter density profile. The student will explore various density models of the dark matter, taking into account the effects of black holes and baryonic dynamics.
What is the lowest mass object that can form like a star? And how many massive planets are ejected from their planetary systems during the formation process? These two questions will be tackled in this project.
Over the last years, we have carried out a search for the lowest mass free-floating objects in star forming regions, in a project called SONYC (short for Substellar Objects in Nearby Young Clusters). In SONYC we used the largest existing ground-based telescopes to make ultradeep surveys of the youngest clusters on the sky. While we found plenty of brown dwarfs (with some interesting evidence for environmental difference in the formation of brown dwarfs), we did not find many objects with super-Jupiter masses, the presumed ejected giant planets. If they exist (and we expect that they do), they will be below our mass threshold of 5 Jupiter masses and are still to be discovered.
In the next step of this project (and in this PhD project) we will use the James Webb Space Telescope to explore the domain of free-floating rogue planets with masses between 1 and 5 Jupiter masses. We have good chances to get observing time to get this project started right after the JWST begins operation in 2018. The student will prepare the observations and explore follow-up avenues, with JWST and other facilities, and then be the first to analyse the data. In addition, we will work with the second data release from Gaia to pin down the fundamental parameters of young brown dwarfs. This will lead to new contraints on star formation simulations and insights into the transition from star to planet formation.
This will be a strongly observational project, which requires to learn the details of optical and infrared observations, the physics of ultracool objects, the intricacies of disentangling emission from objects, disks, and accretion, as well as an interest in collaborating with people from the theory side, including atmospheric physics and star/planet formation.
More than 3000 exoplanets have been discovered which have a unprecedented diversity compared to the solar system planets, ranging from inflated hot Jupiters to lava planets. All planets do develop an atmosphere that changes its chemical composition during the planet’s evolution, and most of them will form clouds. As the atmosphere is the window through which we observe and analyse the planets, it is essential to understand how clouds effect the atmosphere. Cloud formation modelling is still the largest uncertainty in exoplanet atmosphere research, but also in Earth climate modelling. Parameterisations are often used as a first approach to achieve first results.
This project will built on the kinetic cloud formation approach developed by Helling & Woitke that described the formation processes of the cloud particle from the gas phase in detail. The project will extend this model to include inter-cloud particle processes similar to processes studied in protoplanetary disks. 1D atmosphere and 3D atmosphere simulations are envisioned to link with observations.
The student will work with Dr Christiane Helling as part of the LEAP group.
http://leap2010.wp.st-andrews.ac.uk/ Please contact Ch Helling for more information.
Wild, Dr Vivienne - firstname.lastname@example.org
To understand how galaxies form and evolve, we use telescopes to obtain images and spectra of hundreds of thousands of galaxies, and explain their observables in terms of their formation history. However, the observations are only half the story: to really understand what shapes galaxies, we also use computers to run large simulations, and construct models of galaxies from our current theories of galaxy formation and evolution. These galaxy models need recipes for e.g. star formation and supernova feedback, and their simulated spectra are used to interpret the features of observed galaxy spectra.
For this project, you will work on building a library of galaxy merger models. You will construct the progenitor galaxy models, you will merge these models under different orbital configurations, and you will analyse the resulting merger models. You will incorporate various astrophysical recipes for star formation, feedback, etc. in these simulations, and process the output into mock observations to compare the outcomes to real galaxies from the MaNGA survey (Mapping Nearby Galaxies at Apache Point Observatory, http://www.sdss.org/surveys/manga), which is obtaining integral-field spectroscopic datasets for 10,000 galaxies.
The school of physics and astronomy at the University of St Andrews is a member of the UK participation group in SDSS-IV (fourth generation of Sloan Digital Sky Surveys, www.sdss.org), a large international collaboration encompassing several astronomical surveys (including MaNGA). The SDSS is one of the most impactful astronomical surveys, with more than 7000 published papers based on SDSS data, and 30% of the US astronomical community reporting the use of SDSS data in their research. A large part of SDSS’s success is its policy of public data releases, ensuring accessible data sets through detailed documentation, and its involvement with education and public outreach. You will be able to continue this tradition by making your merger library publicly available, developing easy to access web tools and applications, and writing documentation, tutorials and outreach activities (possibly involving citizen science). You will develop skills that not only allow you to create large data sets, but also to present them to various types of audiences (professional astronomers, teachers, students, general public) and making big data visible and accessible.
Please contact the lead supervisor, Vivienne Wild for more information (email@example.com).
Weijmans, Dr Anne-Marie - firstname.lastname@example.org
Wild, Dr Vivienne - email@example.com
How galaxies form and evolve is one of the outstanding questions of modern astrophysics. Extremely large spectroscopic surveys are providing an increasingly detailed census of both local and distant galaxies. Considerable progress is being made on quantifying the changing demographics of the galaxy population over the majority of the age of the Universe, but significant improvements in methods are demanded by the increasingly large samples, but often decreasing quality of the individual observations.
In the last decade a Bayesian approach to the fitting of sophisticated models to high quality spectra and/or multiwavelength photometry has become common place in the analysis of galaxies at all redshifts (Walcher et al. 2011). This works well for high quality observations of individual galaxies - but how can we use the same approaches for lower quality observations of increasingly large samples? Empirical, or hierarchical, Bayes techniques have appeared in the astronomical literature to solve problems as diverse as QSO redshift estimation (Bovy et al. 2011), exo-planet orbit analysis (Hogg et al. 2011), properties of SN 1a light curves (Mandel et al. 2009), and photometric redshifts (Leistedt et al. 2016). They differ from standard Bayesian methods by fitting the entire dataset in a coherent manner, instead of single objects using pre-defined priors. By applying these methods to galaxy evolution studies, we will improve our ability to break degeneracies, either by fitting complete populations of single object spectra, or entire IFU datacubes in a single process.
The school of physics and astronomy at the University of St Andrews is a member of the UK participation group in SDSS-IV (fourth generation of Sloan Digital Sky Surveys, www.sdss.org), a large international collaboration encompassing several astronomical surveys (including MaNGA and eBOSS). Dr Tojeiro is also involved in DESI, which will provide an unprecedented high-density, highly complete local spectroscopic sample of galaxies to a magnitude limit of r=19.5 over 14,000 deg2 of sky. The project involves the development of statistical techniques to make them applicable to astronomical datasets. Applications from students with a background in maths or physics and interest in astrophysics are welcome, as well as from students with a background in astrophysics but strong aptitude for maths and statistics.
Note that access to data from the SDSS-IV survey is rare in the UK, and guaranteed through the supervisors core involvement in the survey.
Please contact Vivienne Wild. the lead supervisor for the project, for more information (firstname.lastname@example.org)
Bovy J., Myers A. D., Hennawi J. F. et al. arXiv:1105.3975
Hogg D. W., Myers A. D., Bovy J., 2010, ApJ, 725, 2166
Leistedt B., Mortlock D., Peiris H., 2016, MNRAS, 460, 4258
Mandel K. S.; Wood-Vasey W. M., Friedman A. S., Kirshner R. P., 2009, ApJ, 704, 629
Walcher C. J., Groves B., Budavri T., Dale D., Ap&SS, 2011, 331, 1
Extensive layers of diffuse ionized gas are observed in the Milky Way and other galaxies. This project will study the structure, ionization, heating, and dynamics of diffuse ionized gas using a combination of 3D Monte Carlo radiation transfer codes and recent 3D dynamical models of a supernova driven ISM.
The University of St Andrews is a founding institutional member of the Wide-Angle Search for Planets (WASP) project, which is a consortium comprising 6 UK universities and 3 overseas observatories. We use two arrays of wide-field camera lenses backed by large-format CCDs to perform high-precision photometry of millions of stars each night, looking for the 1% dips in light that betray gas-giant planets whose orbital planes are close enough to the line of sight that they transit their host stars. Our current catch stands at 166 planets confirmed by radial-velocity follow-up.
St Andrews is a member of the HARPS-N consortium for radial-velocity follow-up of super-Earth and sub-Neptune sized transiting planets from the NASA Kepler/K2 mission using the HARPS-North radial-velocity spectrometer on the 3.5-m Telescopio Nazionale Galileo (TNG) on La Palma. The consortium has 80N/year of guaranteed time on HARPS-N, and is preparing to follow up targets from the NASA TESS mission, due for launch in late 2017. The St Andrews group specialises in spectroscopic characterisation of planet-host stars, in order to isolate the planetary radial-velocity signals from the spurious quasi-periodic signals generated by magnetic activity.
Andrew Cameron is a member of the Science Team for the Swiss-led ESA CHEOPS mission, with responsibility for the work package on light curve analysis. CHEOPS is due for launch in 2018. It will search for transits in known radial-velocity planets, and improve the precision of transit profiles for planets discovered with TESS.
Possible PhD projects for the 2017 intake include development of new Bayesian approaches to determining the ages and masses of transiting planets characterised with these facilities, using kinematic and parallax information from ESA's Gaia astrometry mission; follow-up and characterisation of new WASP planets; Bayesian statistical studies of the underlying planet populations studied by WASP and HARPS-N; and the application of machine-learning methods to exploration of other types of astrophysical object among the 31 million light curves in the WASP data archive.
Light travel time delays enable micro-arcsecond mapping of accretion disks and broad emission-line regions around the super-massive black holes in the nuclei of active galaxies. RoboNet provides the UK with unique datasets for measurement of black hole masses, accretion rates, and luminosity distances. The student will acquire and analyse such datasets, using parameterized models and Hornes maximum entropy fitting code MEMECHO.
Most stars form in clusters, where energetic feedback from massive
(proto)stars--including outflows, ionization, heating, and
winds--shapes the environment and impacts accretion. The relative
importance of different feedback processes is a key outstanding
issue in our understanding of massive star formation.
The aim of this project is to conduct the first large-scale
observational study of the role and physics of feedback in massive
(proto)clusters. This will involve analyzing high-resolution data
from recently-upgraded (sub)mm and cm-wavelength interferometers, in
particular the Submillimeter Array (SMA), the Jansky Very Large Array
(VLA), and, potentially, the Atacama Large Millimeter/sub-millimeter
Array (ALMA). The observational results will be compared with
simulated observations of numerical models of massive star and
Dust grains in protoplanetary discs generally charge up due to photo-effect, electron attachment, and charge exchange reactions with molecular ions. Grain-grain collisions can possibly lead to an additional statistical charging (contact electrification), which has not yet been thoroughly discussed in the disc community yet (see e.g. Muranushi 2010). If grains of different sizes collide, charge up size-dependently, and move selectively (by gravitational settling), a large-scale charge separation could build up, leading to lightning in discs. This scenario has been proposed to explain intra-cloud lightning observed in volcano plumes, as well as lightning in the Earth’s atmosphere and in exo-planets (Helling et al. 2016). Similar effects could take place in protoplanetary discs, causing radio emission and having a long-term impact of the chemical composition of the gas.
* Is frictional charging a key process for midplane ionisation and the MRI in discs?
* Can the gravitational settling of charged grains build up electrostatic fields in discs?
* Can this field overcome the break-down field to cause spontaneous discharge processes (lightning)?
* Where exactly, in the disc, are these processes most likely to occur?
* Could lightning lead to observable signals, like short-term radio variability?
* Could lightning have a long-lasting impact on the chemistry in the planet-forming region?
PhD-student is expected to implement triboelectric charging rates into ProDiMo, using typical turbulent dust velocities from MHD disc models. The resulting charge distribution of the grains will be studied depending on size and location in the disc, and consequences for large-scale electrification and lightning in discs shall be discussed.
GravityCam is a proposed mosaic camera composed of ~100 EMCCDs with a novel design that for the first time combines a wide field with a very fast readout, thereby achieving an angular resolution of 0.15’’ by means of lucky imaging and opening up an entirely new observing paradigm for ground-based astronomy, its only real competition being in space. A core science driver for GravityCam is a Galactic bulge microlensing survey that could go about 4 magnitudes deeper than current efforts for the same signal-to-noise ratio and exposure time, and thereby at the same sensitivity probe cool planets (or satellites) that are 100 times less massive, which gives access to a hitherto uncharted region in planet parameter space extending down to Lunar mass. In addition, as a unique and versatile instrument, GravityCam will be suitable for addressing a wide variety of scientific applications, including in particular studies of dark matter (by means of weak lensing), fast-varying astronomical objects, asteroseismology, variability and astrometry in crowded fields, occultations by small Solar-System bodies, and transiting extra-solar planets, while providing an extensive resource for general data mining of the high-speed variable sky.
You will have the opportunity to optimise the design of a GravityCam microlensing campaign by means of simulations in order to maximise the science output relating to the arising planet population statistics, which requires carefully balanced choices of exposure time and cadence dictating the total survey area. Moreover, you can take part in current observational efforts (MiNDSTEp and Robonet-II), pioneering crowded-field lucky-imaging photometry and real-time scheduling of microlensing targets across telescope networks.
New spatially resolved observations of protoplanetary discs have revealed so far unseen spatial structures within the discs, such as rings, holes, spiral arms, warps, shadows, and large vortices. They are detected at various wavelengths, in the gas and dust, in scattered light and in thermal emission. These structures are very likely direct signposts of the planet formation process in the discs, yet current hydrodynamical disc models suffer from a very basic uncertainty, namely the poor treatment of radiative transfer and heating/cooling effects in hydrodynamical disc models. The supervisor is an expert in the fields of chemistry, heating & cooling and radiative transfer, but these techniques need to be extended and merged with (magneto) hydrodynamics in 3D to get ready for the new challenges in the era of spatially resolved disc observations.
This project aims at merging current state-of-the-art modelling techniques concerning (magneto) hydrodynamics, chemistry and radiative transfer in protoplanetary discs. Based on the radiation thermo-chemical disc code "ProDiMo" which includes a very detailed treatment of 2D continuum and line radiative transfer, and gas energy balance, we aim at the production of numerical look-up-tables of equilibrium gas and dust temperatures, chemical and ice composition of the gas, and effective heating & cooling rates suitable for hydrodynamical disc simulations.
The task is to build a brigde between thermo-chemical and hydrodynamical disc simulations. The student will study and learn how to run both types of models, calculate the look-up-tables with ProDiMo, and then apply these in hydrodynamical disc simulations.
Extrasolar planet atmospheres form clouds and the emergence of lightning can be expected. Lightning events do affect the local chemistry such that chemical lightning tracer species do survive for months to years. Even more, lightning is suggested to play unimportant role in the formation of the first biomolecules in the atmosphere of the early Earth.
This project will apply lighting statistics to determine how the local chemistry changes globally building on the work carried out in the LEAP group. Of particular interest is the identification of lightning tracer molecules in atmospheres of different extrasolar planets. We aim to develop observational strategies for lightning in atmospheres of extrasolar planets.
he student will work with Dr Christiane Helling as part of the LEAP group.
http://leap2010.wp.st-andrews.ac.uk/ Please contact Ch Helling for more details.
The mass distribution of the Galaxy is being / will be mapped out in great detail in the next decade with the numerous surveys of the Galaxy, including Segue, RAVE, GAIA, and completed ones like 2MASS, DENIS. A model for the potential and phase space of the galaxy is essential to bring various pieces of information together. The student will develop such models building on experience from existing models.
Intensive monitoring of Galactic Bulge microlensing events is being used to discover cool planets in 1-5 AU orbits around the lens stars. Our PLANET/RoboNet team has just discovered a 5 earth-mass planet. In the next 4 years we aim to measure the abundance and mass function of cool planets to test theories of planet formation and migration. The student will work with our team to acquire and analyse observations, fit microlens models to characterize the planetary and other anomalies.
Rotation is a fundamental property of stars. The angular momentum regulation of stars is linked with the evolution of disks, the physics of magnetically driven winds, and the interior structure. Stars like the Sun start with a period of a few days, but spin down to periods of weeks and months over the course of billions of years. This project is focused on investigating the spindown of very low mass stars, the most abundant type of stars in our Galaxy, which present a serious challenge for our current understanding of stellar rotation. In contrast to solar-mass stars, they have long spindown timescales of ~1 gigayear or more. The extreme case are brown dwarfs, which do not seem to spin down over a Hubble time, comparable to giant planets. All this is probably related to the atmospheric physics, particularly the magnetic properties. We are therefore particularly interested in probing the link between rotation and magnetic activity. We have been granted observing time with the Kepler-2 mission to get lightcurves for very low mass stars and brown dwarfs are various stages of their evolution. Since these stars are magnetically very active, star spots cause a periodic modulation of the flux from which the rotation period can be measured with high accuracy. The same lightcurves also give information about magnetic spots. The archive of the Super-WASP planet search will also be used to study the longest timescales. Another dataset from the Very Large Telescope will be used to examine rotation rates in young free-floating planetary mass objects. There is scope for new observations carried out with large telescopes. We will measure rotation periods, probe the period-activity correlation, compare with new models for the stellar spindown, and investigate the possibility of gyrochronology (i.e. estimating ages from rotation rates) for red and brown dwarfs.
This project is to develop the first models of resolved star formation on galactic scales. This will involve modelling a full galactic potential and how it drives the formation of molecular clouds and the onset of gravitational collapse and star formation. feedback from ionisation and supernova will be included to assess molecular cloud lifetimes and star formation efficiencies.
Tau Boo is the only star for which we have been able to track the full cyclic reversal of the stellar magnetic field. This system is also well-known, however, because it hosts a Hot Jupiter that is so close to the star that it may lie within the stellar corona. What is the nature of the interaction between the star and planet in this case and is it related to the puzzling nature of the very short magnetic cycle? This project will investigate tau Boo and other similar star-planet systems.
When a newborn solar-like star emerges from its natal cloud it is still surrounded by a substantial disk of dust and gas. At this stage of pre-main sequence evolution the star interacts with the inner disk via its large-scale magnetic field, which channels gas onto the stellar surface at high velocity. Recent large observing programs have begun to reveal how their magnetic geometries are linked to their location in the Hertzsprung-Russell diagram. Tentatively, it appears as though solar-like stars are born with simple axisymmetric magnetic fields that become more multipolar/complex and non-axisymmetric as the stellar interior structure varies from fully to partially convective. Should this stellar structure change occur before the disk has dispersed it will have implications for the magnetic star-disk interaction, the coronal evolution of the star itself, the balance of torques in the star-disk system, and the rotation rate of the star. Using the latest observational data as a basis, the student will model the star-disk interaction and coronal magnetic evolution as stars evolve across the pre-main sequence.
For more evolved pre-main sequence stars, where the disk has dispersed but the star is still contracting under gravity, it has been observed that the scatter in X-ray luminosities decreases for stars in older star-forming regions, approaching main sequence cluster levels by about ~30 Myr (roughly the pre-main sequence lifetime of a solar mass star). Using new data currently being acquired as part of a large program at the Canada-France-Hawai'i Telescope we will model the coronal evolution of pre-main sequence stars, and produce a theoretical grounding for the observed evolution of their rotation-activity relationship.
There are several outstanding issues in current models of star formation. One of these is the role of feedback from young stars in producing subsequent generations of young stars. Triggering of star formation through supernova events is likely to be the dominant mechanism. Numerical simulations of SNII impacting on molecular clouds and the triggering of star formation will be used to develop physical models, and ultimately observational predictions and tests of the process.
Weijmans, Dr Anne-Marie - email@example.com
Wild, Dr Vivienne - firstname.lastname@example.org
The Dark Energy Spectroscopic Instrument survey will gather spectra for many millions of galaxies over 14,000 sq. degrees of sky. The size and depth of DESI, particular the Bright Galaxy Survey, will allow us to study the large-scale structure and detailed local environment of each galaxy with unprecedented accuracy. Combined with careful spectral analysis of galaxies, which tells us about its formation history, chemical enrichment and dust content, we will be able to link the evolution of galaxies with their cosmological and local environment with unprecedented clarity.
However, current spectral analysis techniques, although successful, rely on much higher signal to noise data than will be delivered by DESI.
In the regime where we have very many N spectra of low S/N, you will explore forward-modelling techniques, whereby model populations of galaxies are forward-modelled through a survey’s window function, which includes selection and observational effects such as target selection, photon-noise, foregrounds, etc. In that regime, we are interested in recovering the mean physical properties of a set of M galaxy populations, where M << N (see Montero-Dorta et al. 2016 for a simplified application to another dataset). The potential of this technique lies in the fact that the redshift evolution of the galaxy populations may be measured in a completely self-consistent way, using a hierarchical Bayesian approach. In addition you will explore simpler, fully data-driven techniques to recover a mean signal from noisy data. This is a well-studied problem in applied statistics. Often called denoising or signal reconstruction algorithms, such methods work by either filtering (e.g., using wavelets); Gibbs sampling (e.g., Wandelt 2004 for a CMB-motivated approach); or noise subtraction (a common technique in speech recognition).
You will then be able to study the detailed evolution of galaxies within the intricate context of their environment, which will be beautifully characterised by DESI.
This project will suit a student with a keen interest in data analysis, algorithm development, applied statistics and data science.
The DESI survey: https://arxiv.org/abs/1611.00036v1
Montero-Dorta et al. 2016, MNRAS, 461, 1131
Wandelt 2004, arXiv:astro-ph/0401623
Currently popular models for the formation of stars like the Sun invoke accretion along magnetic field lines from a protoplanetary disk onto hot spots on the stellar surface. This star-disk model can explain the observed infrared emission from disks and also the ultraviolet excess emission produced from shocks of accreting material impacting the stellar surface. Young stars also display multi-wavelength variability on a wide range of timescales, again attributed to the accretion geometry. The on-going YSOVARS observing campaign is obtaining vast optical and infrared datasets on young stars revealing the complexities of their temporal variability. The goal of this PhD project is to use detailed three dimensional Monte Carlo radiation transfer simulations to model the observed multiwavelength data from the YSOVARs project. Working together with Kenny Wood and Aleks Scholz at St Andrews and in collaboration with members of the YSOVARS team in California, the student will explore different classes of variability and the different star-disk-magnetic field configurations that produce the observed light curves. By modeling data from the vast YSOVARs archive, we will learn about magnetic accretion geometries, disk warping, and the accompanying variability on a range of different time and spatial scales, all contributing to a greater understanding of the star formation process.
Informal enquiries to Kenny Wood: email@example.com
Carr & Najita (2008) have established that class II T Tauri stars usually exhibit rich molecular emission spectra of H2O, OH, CO2, HCN and C2H2. These emissions are often superpositions of many (up to hundreds of) individual emission lines. JWST/MIRI and, in the future SPICA/SMI, will observe protoplanetary discs with unprecedented spectral resolution and signal/noise.
In the frame of the supervisor's FP7 project "DIANA" we have developed the new fast line tracer FLiTs (yet unpublished work) which can compute formal solutions of the line radiative transfer problem for tens of thousands of spectral lines simultaneously, including the Keplerian velocity fields and physical line overlaps. These line radiative transfer calculations are based on ProDiMo (Woitke et al.2009) thermo-chemical disc models, which compute the chemical abundances and temperatures of gas and dust.
These two developments allow us to harvest future JWST and SPICA line observations of discs. Our models predict these lines fully consistently with the calculated 2D disc structures, which is a much
more powerful approach than previously used parametric LTE-slab models.
The science questions are
* What are the element abundances, and what is the molecular composition of the gas in the planet-forming regions of protoplanetary discs?
* Why do some T Tauri stars show strong molecular emission lines whereas others don’t? Why do Herbig Ae stars show weaker line emissions?
* Can we use IR molecular emission lines to determine the spatial disc structure and diagnose disc anomalies such as gaps, vortices and spiral waves at radial distances of a few AU?
* Can we conclude about dust opacities and gas/dust ratios in the planet forming region?