My research mostly focusses on the formation
and evolution of stars and their planetary systems. In particular
I am interested in the dusty debris material that surrounds some stars,
including the Sun, during their main sequence phase. The dust is heated
by the star and is observed by its thermal emission in the mid-IR to
this thermal emission is detected either as an excess above the star's
photospheric emission or as emission that is extended from the
point-like star. In the few (6 as of 12/9/00) cases where the dust
has been mapped, it is seen to lie in a disk around the star. It is
that in much the same way that the disk of dust in the solar system,
the zodiacal cloud, is created by the break-up of the solar system's
and comets, this exozodiacal dust is also the end product of the
of the remnants of the system's planetary formation phase. As Vega was
the first main sequence star other than the Sun that was shown to
infrared emission in excess of its photospheric emission, stars with
excesses are known as Vega-type stars. Whether their excess
is debris disk
emission, and what these debris disks can tell us
about how these stars formed and the status of planetary formation
them, is the subject of my research.
The research can be broken down into four main areas:
The following publications are available for download in pdf format:
- Identification - The first area concerns identifying
sequence stars may have debris disks. This involves comparing surveys
IR sources (such as IRAS and MSX) to catalogs of main sequence stars
the Michigan Spectral Catalog). The issues associated with this area
how to determine the stellar properties, in particular how to determine
the contribution of the stellar photosphere to the IR flux, how to
between different types of IR excess emission (e.g., free-free emission
and debris disk dust emission), as well as contending with the other
uncertainties such as position and flux errors and IR contamination by
- Debris disk database - We have compiled a web-based
of information (from SIMBAD, VIZIER, published and unpublished
plus some modelling analysis) on the 300 or so debris disk candidates
were identified in surveys of the IRAS databases. This is accessible
- Observation - A debris disk system is so complicated
are many observations that need to be done before we can even begin to
understand it. As well as general information about the stellar system
(such as age, spectral type, are there any binary companions, etc, all
of which may require a further set of observations), here follows a
of some of the types of observations that we are doing:
- Broad band photometry - The spectral energy
thermal emission is important since it allows us to determine the
of the dust, which in turn gives its distance from the star. Using IRAS
mid-IR and far-IR fluxes it was shown that the dust emission from most
Vega-type stars is cool (50-100 K) implying that the dust is in regions
analagous to the Kuiper belt of comets in the solar system (>30 AU
the star). We have carried out sub-mm (450 and 850um) photometry using
SCUBA at the JCMT to extend the SEDs to longer wavelengths. The benefit
of these observations is that the slope of the SED at these wavelengths
is indicative of the largest grains in the disk.
- Imaging - Ideally we would like a direct measurement
distribution of the dust around the star. The problem is that we are
by the resolution and sensitivity of currently available astronomical
which mean that only the closest and brightest disks are resolvable. So
far 4 disks have been resolved in the sub-mm using SCUBA (Vega, beta
Fomalhaut, and epsilon Eridani), and a further two have been imaged in
the mid-IR using OSCIR (HR 4796 and HD 141569; these have also been
in the near-IR using NICMOS on the HST). We have observing programs in
place to image debris disks using both of these instruments.
- Spectroscopy - There are several spectral features
shown to be indicative of the composition of the debris dust (e.g., the
9.7um silicate feature). Observations of these features can be modelled
to obtain information on the size, composition and spatial extent of
dust. We aim to obtain such observations using OSCIR, MICHELLE, and
- Spectral line - It is of great importance to determine
stars still have gas around them, since the gas is indicative of the
status of the disk system. We have carried out a search for CO J=3-2
emission from a sample of bright debris disks from the JCMT.
- Zodiacal cloud - While we have only been talking about
clouds until now, the same arguments apply for the zodiacal cloud.
since it is closer, and hence ubiquitous, we have to use different
Most information on the zodiacal cloud thermal emission comes from
satellites such as IRAS, COBE, ISO, MSX, SIRTF. However, there is much
more information available about the zodiacal cloud system, since we
measure the sources of dust (the asteroids and comets) as well as
the properties of the dust itself.
- Modelling - The interpretation of debris disk
on the method of comparing those observations with pretend observations
of a model of the disk. This model will have various free parameters
will be constrained by the observations. The more observational
that is available, the more complicated the model. This means that a
of the zodiacal cloud can have far more free parameters than a debris
for which we may only have broad band photometry. The input for one of
my model observations depends on the theory being tested, but in
- Spatial distribution - A model of the
of material in the disk. This can range in complexity from a simple
model with free parameters of the inner and outer cutoffs with a power
law distribution in between, to a full dynamical model that can
dust clumps and asymmetries.
- Dust grain composition and morphology - The model for
dust grain optical properties that I have been using is based on that
by Li & Greenberg (1997). The grains are assumed to be made of a
core (either amorphous or crystalline) with an organic refractory
They are assumed to be porous with a fraction of ice filling in the
The optical constants for these grains are added together assuming
ratios for the components using Maxwell-Garnett effective medium theory.
- Dust size distribution - At the most basic level, we
the particles in the disk to be all of the same size. However, more
we would assume the size distribution to follow some distribution that
is based on a physical model for the collisional and dynamical
in the disk. Further adding to the complication, particles of different
sizes may have either different spatial distributions or different
- Stellar parameters - Combining the stellar spectrum,
luminosity and mass, we can calculate the temperature, radiation forces
and emission efficiencies of the dust grains.
- Orientation - A map of the disk emission can be made
the orientation of the disk to our line of sight and integrating the
from all dust grains along the line of sight of each pixel in the image.
- Physics - For any interpretation of the observation, we
that is based on an understanding of the physical processes affecting
disk's evolution so that the observations can be directly related to
physics. In the case of the zodiacal cloud, that physics is relatively
well defined, whereas in debris disk systems we are much more unsure
what we are looking at. In this instance we have to consider how all
physical processes that may be both currently and in the recent past
the disks. The issues that I am studying at the moment are:
- Planets - How do the gravitational perturbations of
planets to the
orbits of the debris material affect the structure of a debris disk?
we use observations of asymmetrical or clumpy debris disk structures to
infer the existence of unseen planets that may be hiding in the disk?
of the zodiacal cloud show that planetary perturbations do cause
asymmetries in the structure of the zodiacal cloud. We also showed that
secular planetary perturbations could be causing the asymmetry observed
in the structure of the HR 4796 disk. Also, resonant planetary
may cause clumps in the structure of a debris disk that follow the
around its orbit.
- Collisions - The short collisional lifetimes of dust
the debris disks means that they cannot be primordial, rather they must
have been created by collisions between larger bodies, which may
have been created by collisions between even larger bodies. Such a
cascade is how the dust in the zodiacal cloud is produced, by the
down of the asteroid belt. However, collisional processes are not
understood even in the solar system; e.g., while the LDEF (Long
Exposure Facility) result that most of the cross-sectional area of dust
being accreted onto the Earth is in grains between 100-200 micron in
is understood in terms of the interplay between Poynting-Robertson drag
and collisions, this result has not been used to obatin quantitative
about the collisional evolution of the zodiacal cloud. In terms of
disks, one important question that remains to be answered is whether
collisions between the largest members of the disk could cause clumps
as those observed in the disk around Epsilon Eridani) to form, and
this is statistically likely.
- Stellar Wind and Lorentz Forces - These are forces
ignored when modelling debris disks. In the case of the zodiacal cloud
it is certainly true that they can be ignored: stellar wind forces
act like Poynting-Robertson drag to make the particles spiral into the
star) are 1/3 as strong os those from radiation forces, Lorentz forces
are also substantially lower than other perturbing forces (except maybe
in the outer solar system). However, this rationale may not be
to dust around other main sequence stars where these forces may even
the dust's evolution; but we do not generally know the structure and
of a star's wind, nor do we know the structure of its magnetic field.
- Binary Companions and Stellar Flybys - Gravitational
from a binary companion, or from a stellar flyby, may act to perturb
disk in a similar way to perturbations from a planetary sytem,
in distinctive features in the structure of the disk. Of the six
debris disks,.three are in wide binary systems (Fomalhaut, HR 4796, HD
141569), and another exhibits structure that can be explained in terms
of a recent stellar flyby (beta Pictoris). Is this coincidence? Or is
existence of a disk linked to the binarity of the system, maybe because
the passing of a companion stirs up the normally quiescent disk,
more violent collisions and a corrsepondingly brighter disk? Certainly
if a disk is in a binary system, the binary orbit must be determined if
we are to understand its effect on the evolution of the disk; this is
always easy in the case of wide binary orbits!
- The Exozodiacal
Dust Problem for Direct Observations of ExoEarths
Roberge A., Chen C. H., Millan-Gabet R., Weinberger A. J., Hinz P. M.,
Stapelfeldt K. R., Absil O., Kuchner M. J. Bryden G., \& the NASA ExoPAG SAG1
Team 2013, PASP, in press.
- Resolved Debris Discs Around A
Stars in the Herschel DEBRIS Survey
Booth M., Kennedy G. M., Sibthorpe B., Matthews B. C., Wyatt M. C.,
Duchene G., Kavelaars J. J., Rodriguez D., Greaves J. S., Koning A., Vican L.,
Rieke G. H., Su K. Y. L., Moro-Martin A., Kalas P. 2013, MNRAS, 428, 1263.
debris disk around gamma Doradus resolved with Herschel
Broekhoven-Fiene H., Matthews B. C., Kennedy G. M., Booth M., Sibthorpe B.,
Lawler S. M., Kavelaars J. J., Wyatt M. C., Qi C., Koning A., Su K. Y. L.,
Rieke G. H., Wilner D. J., Greaves J. S.
2013, ApJ, 762, 52.
- A Self-Consistent
Model of the Circumstellar Debris Created by a Giant Hypervelocity Impact in the
Johnson B. C., Lisse C. M., Chen C. H., Melosh H. J., Wyatt M. C., Thebault P., Henning W. G.,
Gaidos E., Elkins-Tanton L. T., Bridges J. C., Morlok A.
2012, ApJ, 761, 45.
- A DEBRIS Disk
Around The Planet Hosting M-star GJ 581 Spatially Resolved with Herschel
Lestrade J.-F., Matthews B. C., Sibthorpe B., Kennedy G. M., Wyatt M. C.,
Bryden G., Greaves J. S., Thilliez E., Moro-Martin A., Booth M., Dent W. R. F.,
Duchene G., Harvey P. M., Horner J., Kalas P., Kavelaars J. J., Phillips N. M.,
Rodriguez D. R., Su K. Y. L., Wilner D. J.
2012, A&A, 548, A86.
imaging of 61 Vir: implications for the prevalence of debris in low-mass
Wyatt M. C., Kennedy G., Sibthorpe B., Moro-Martin A., Lestrade J.-F.,
Ivison R. J., Matthews B., Udry S., Greaves J. S., Kalas P., Lawler S.,
Su K. Y. L., Rieke G. H., Booth M., Bryden G., Horner J., Kavelaars J. J.,
Wilner D. 2012, MNRAS, 424, 1206.
- Debris disks
as signposts of terrestrial planet formation. II Dependence of
exoplanet architectures on giant planet and disk properties
Raymond S. N., Armitage P. J., Moro-Martin A., Booth M., Wyatt M. C.,
Armstrong J. C., Mandell A. M., Selsis F., West A. A.,
2012, A&A, 541, A11.
- 99 Herculis:
Host to a Circumbinary Polar-ring Debris Disk
Kennedy G., Wyatt M. C., Sibthorpe B., Duchene G., Kalas P.,
Matthews B., Greaves J. S., Su K. Y. L., Fitzgerald M. 2012, MNRAS,
- Spitzer Evidence for a Late
Heavy Bombardment and the Formation of Urelites in eta Corvi at ~1 Gyr
Lisse C. M., Wyatt M. C., Chen C. H., Morlock A., Watson D. M., Manoj P.,
Sheehan P., Currie T. M., Thebault P., Sitko M. L., 2012, ApJ, 747, 93.
Observations of HD69830: High Resolution Spectroscopy and Limits to
Beichman C. A., Lisse C. M., Tanner A. M., Bryden G., Akeson R. L., Ciardi D. R.,
Boden A. F., Dodson-Robinson S. E., Salyk C., Wyatt M. C., 2011, ApJ, 743, 85.
Modelling of the beta Leo Debris Disc: 1, 2 or 3 Planetisimal Populations?
Churcher L. J., Wyatt M. C., Duchene G., Sibthorpe B., Kennedy G., Matthews B. C., Kalas P.,
Greaves J. S., Su K., Rieke G., 2011, MNRAS, 417, 1715.
- Debris disks
as signposts of terrestrial planet formation
Raymond S. N., Armitage P. J., Moro-Martin A., Booth M., Wyatt M. C.,
Armstrong J. C., Mandell A. M., Selsis F., West A. A.,
2011, A&A, 530, A62.
- Forming the first planetary systems: debris
around Galactic thick disc stars
Sheehan C. K. W., Greaves J. S., Bryden G., Rieke G. H., Su K. Y. L.,
Wyatt M. C., Fischer D. A., Beichman C. A., 2010, MNRAS, 408, L90.
- Resolving debris discs in the far-infrared: early
highlights from the DEBRIS survey
Matthews B. C., Sibthorpe B., Kennedy G., Phillips N., Churcher L., Duchene
G., Greaves J. S., Lestrade J.-F., Moro-Martin A., Wyatt M. C., Bastien P.,
Biggs A., Bouvier J., Butner H. M. Dent W. R. F., Di Francesco J., Eisloffel
J., Graham J., Harvey P., Hauschildt P., Holland W. S., Horner J., Ibar E.,
Ivison R. J., Johnstone D., Kalas P., Kavelaars J., Rodriguez D., Udry S., van
der Werf P., Wilner D., Zuckerman B., 2010, A&A, 518, L135.
- Planets and Debris Disks: Results from a
Spitzer/MIPS Search for IR Excess
Bryden G., Beichman C. A., Carpenter J. M., Rieke G. H., Stapelfeldt K. R.,
Werner M. W., Tanner A. M., Lawler S. M., Wyatt M. C., Trilling D. E., Su K. Y. L.,
Baylock M., Stansberry J. A.
2009, ApJ, 705, 1226.
- Extra-solar Kuiper Belt dust disks
Moro-Martin A., Wyatt M. C., Malhotra R., Trilling D. E. 2008.
In Kuiper Belt, eds. A. Barucci, H. Boehnhardt, D. Cruikshank and A. Morbidelli,
(Tucson, Univ of Arizona Press), 465-480.
- An Unbiased Survey of 500 Nearby Stars for Debris Disks:
A JCMT Legacy Program
Matthews B. C., Greaves J. S., Holland W. S., Wyatt M. C., Barlow M. J., Bastien P.,
Beichman C. A., Biggs A., Butner H. M., Dent W. R. F., Di Francesco J., Dominik C.,
Fissel L., Friberg P., Gibb A. G., Halpbern M., Ivison R. J., Jayawardhana R., Jenness
T., Johnstone D., Kavelaars J. J., Marshall J. L., Phillips N., Schieven G., Snellen
I. A. G., Walker H. J., Ward-Thompson D., Weferling B., White G. J., Yates J., Zhu M.,
2007, PASP, 119, 842.
- New debris disks around nearby main sequence
stars: impact on the direct detection of planets
Beichman C. A., Bryden G., Stapelfeldt K. R., Gautier T. N., Grogan K.,
Shao M., Velusamy T., Lawler S., Blaylock M., Rieke G. H., Lunine J. I.,
Fischer D. A., Marcy G. W., Greaves J. S., Wyatt M. C., Holland W. S.,
Dent W. R. F. 2006, ApJ, 652, 1674.
- Dust in Resonant
Kuiper Belts: Grain Size and Wavelength Dependence of Disk Structure
Wyatt M. C. 2006, ApJ, 639, 1153.
Debris Disks, and Planets
Greaves J. S., Fischer D. A., Wyatt M. C.
2006, MNRAS, 366, 283.
- Spiral Structure
Pericentre Glow: Possible Giant Planets at Hundreds of AU in the
fig4 in colour
Wyatt M. C., 2005, A&A, 440, 937.
- The Vega Debris Disk
A Surprise from Spitzer
Su K. Y. L., Rieke G. H., Misselt K. A., Stansberry J. A., Moro-Martin
Stapelfeldt K. R., Werner M. W., Trilling D. E., Bendo G. J., Gordon K.
Hines D. C., Wyatt M. C., Holland W. S., Marengo M., Megeath S. T.,
Fazio G. G.
2005, ApJ, 628, 487.
- The Insignificance
P-R Drag in Detectable Extrasolar Planetesimal Belts
Wyatt M. C., 2005, A&A, 433, 1007.
- The Origin and
Evolution of Dust
Wyatt M. C., 2005.
In Dynamics of Populations of Planetary Systems,
eds. Z. Knezevic and A. Milani,
Proceedings of IAU Colloquium 197, 383.
Kuiper Belt around Eta Corvi, fig1 (high res),
Wyatt M. C., Greaves J. S., Dent W. R. F., Coulson I. M., 2005,
ApJ, 620, 492.
- Structure in the
Eridani Debris Disk
Greaves, J. S., Holland, W. S., Wyatt M. C., Dent, W. R. F.,
Robson, E. I., Coulson, I. M. C., Jenness, T., Moriarty-Schieven, G.
Davis, G. R., Butner, H. M., Gear, W. K., Dominik, C., Walker, H. J.,
2005, ApJ, 619, L187.
- Mid-infrared images
and the possible role of planetesimal collisions in the central disk
Telesco C. M., Fisher R. S., Wyatt M. C., Dermott S. F., Kehoe T. J.
Novotny S., Marinas N., Radomski J. T., Packham C., de Buizer J.,
Hayward T. L.,
2005, Nature, 433, 133.
- The debris disc
a massive analogue to the Kuiper Belt
Greaves J. S., Wyatt M. C., Holland W. S., Dent W. R. F.,
2004, MNRAS, 351, L54.
- Modeling the
Disks: Unseen Planets?
Wyatt M. C., 2004. In The Search for Other Worlds: Fourteenth
AIP Conf. Proc., 713, 93.
- Sub-mm Observations
and Modelling of Vega-type Stars
Sheret I., Dent W. R. F., Wyatt M. C., 2004, MNRAS, 348, 1282.
- A Search for Debris
Discs around Stars with Giant Planets
Greaves J. S., Holland W. S., Jayawardhana R.,
Wyatt M. C., Dent W. R. F., 2004, MNRAS, 348, 1097.
- Resonant Trapping
by Planet Migration: Debris Disk Clumps and Vega's Similarity to the
Wyatt M. C., 2003, ApJ, 598, 1321.
- Extrasolar Analogues
Wyatt M. C., Holland W. S., Greaves J. S., Dent W. R. F., 2003, Earth
Moon Planets, 92, 423.
- Book Review:
of the Solar System by Infrared Remote Sensing / Cambridge University
Wyatt M. C., 2003, The Observatory, 1176, 306.
- Some Anomalies in the
of Debris Discs around Main-sequence A and G Stars
Greaves J. S., Wyatt M. C., 2003, MNRAS, 345, 1212.
- SCUBA Observations of
around Lindroos Stars: Evidence for a Substantial Submillimetre Disc
Wyatt M. C., Dent W. R. F., Greaves J. S., 2003, MNRAS, 342, 876.
- Local Heating in the
Center Western Arc
Marinas N., Telesco C. M., Pina R. K., Fisher R. S., Wyatt M. C., 2003,
AJ, 125, 1345.
of an Asymmetric Dust Disk around Fomalhaut
Holland W. S., Greaves J. S., Dent W. R. F., Wyatt M. C., Zuckerman
B., Webb R. A., McCarthy C., Coulson I. M., Robson E. I., Gear W. K.,
ApJ, 582, 1141.
- Dust Clumps in
Other Debris Disks
Wyatt M. C., Holland W. S., Dent W. R. F., Greaves J. S., 2004. In
Debris Disks and the Formation of Planets: A Symposium in Memory of
Gillett, eds. L. Caroff, J. L. Moon, D. Backman and E. Praton,
ASP Conf. Ser., 324, 244
- Warm Debris Disks:
Their Dust and Why?
Wyatt M. C., 2002. In Observing with the VLTI, eds. G. Perrin
and F. Malbet, EAS Publ. Ser. 6, 293.
- Collisional Processes
Planetesimal Disks - Dust Clumps in Fomalhaut's Debris Disk
Wyatt M. C., Dent W. R. F., 2002, MNRAS, 334, 589.
- New Sub-millimeter
on Dust in the 55 Cancri Planetary System
Jayawardhana R., Holland W. S., Kalas P., Greaves J. S., Dent W. R.
F., Wyatt M. C., Marcy G. W., 2002, ApJ, 570, L93.
- The Potential of
Disk Clumps to Confound the Search for Terrestrial Planets
Wyatt M. C., 2001. In Techniques for the Detection of Planets and Life
beyond the Solar System, ed. W. R. F. Dent (Occasional Reports of the
Observatory Edinburgh #17).
- Orbital evolution of
Dermott S. F., Grogan K., Durda D. D., Jayaraman S., Kehoe T. J. J.,
Kortenkamp S. J., Wyatt M. C., 2001. In Interplanetary Dust, eds. E.
B. A. S. Gustafson, S. F. Dermott and H. Fechtig (Berlin:
- A Model of
as the Cause of Clumps in Debris Disks
Wyatt M. C., Dent W. R. F., Greaves J. S., Holland W. S., 2001. In
Planetary Systems in the Universe: Observation, Formation and
eds. A. Penny, P. Artymowicz, A. M. Lagrange, and S. S. Russell, ASP
- Pericentre Glow: A
of Hidden Planets in HR 4796?
Wyatt M. C., Dermott S. F., Telesco C. M., 2000. In Disks,
and Planets, eds. F. Garzon et al., ASP Conf. Ser., 219, 289.
- Detection of
Infrared Emission around the Vega-like Source HD 141569
Fisher R. S., Telesco C. M., Pina R. K., Knacke R. F., Wyatt M. C.,
2000, ApJ, 532, L141.
- Deep 10 and 18 um
of the HR 4796A Circumstellar Disk: Transient Dust Particles and
Evidence for a Brightness Asymmetry
Telesco C. M., Fisher R. S., Pina R. K., Knacke R. F., Dermott S. F.,
Wyatt M. C., Grogan K., Holmes E. K., Ghez A. M., Prato L. A., Hartmann
L. W., Jayawardhana R., 2000, ApJ, 530, 329.
- Signatures of
Observable Structure of Circumstellar Debris Disks
Wyatt M. C., 1999, Ph.D. Thesis, Univ. Florida.
- How Observations of
Disk Asymmetries Can Reveal Hidden Planets: Pericenter Glow and its
to the HR 4796 Disk
Wyatt M. C., Dermott S. F., Telesco C. M., Fisher R. S., Grogan K.,
Holmes E. K., Pina R. K., 1999, ApJ, 527, 918.
- SIRTF: A Unique View
the Earth's Resonant Ring
Wyatt M. C., Dermott S. F., Grogan K., Jayaraman S., 1999. In
with Infrared Surveys: A Prelude to SIRTF, eds. M. D. Bicay et al., ASP
Conf. Ser., 177, 374.
Notes from the following lecture courses are
available for download:
- Part III lecture course on "Planetary system dynamics" given at DAMTP in Michaelmas term 2011 (and previously
in 2009, 2010)
- Part II lecture course on "Astrophysical fluid dynamics" given at IoA in Lent term 2012
- Graduate lecture course on "Planetary systems" given at IoA in 2006, 2007, 2008
The following presentations are also
available for download:
disk dynamical theory
Wyatt M. C. 2008. Presentation at "New Light on Young Stars: Spitzer's
View of Circumstellar Disks", Pasadena, 26-30 October 2008.
- Debris disks at high resolution,
Wyatt M. C., Smith R. 2008.
Presentation at "Workshop on Simulations for ALMA",
Grenoble, 8-10 September 2008.
- Debris disk imaging Wyatt M. C. 2008.
Presentation at "Science with the new Hubble Space Telescope after servicing mission
4", Bologna, 29-31 January 2008.
- Debris disk structure arising from
planetary perturbations Wyatt M. C. 2007.
Presentation at "The direct detection of planets and circumstellar disks in the
21st century: In the spirit of Bernard Lyot", University of California,
Berkeley, 4-8 June 2007.
- Debris disk evolution
Wyatt M. C. 2007. Presentation at "From stars to planets: connecting our understanding
of star and planet formation", University of Florida, Gainesville, 11-14 April 2007.
- Debris disks: dynamics of small particles in
extrasolar systems, theory and observation
Wyatt M. C. 2006. Lecture at "Kobe International School of Planetary Sciences 2006,
Small Bodies in Planetary Systems", Kobe University, December 4-6, 2006.
- SCUBA2 Legacy Debris Disk Survey
Wyatt M. C. 2006. Presentation at "The Submillimetre Revolution: Celebrating
the legacy of SCUBA and looking forward to the potential of SCUBA2" workshop,
ROE, Edinburgh, October 9-11 2006.
- Theoretical modelling of debris disk
Wyatt M. C. 2006. Presentation at The
Planet-Disc Connection conference, IoA, Cambridge, July 17-21 2006.
Our Solar System in Context: A 12 step program to learn to
accept disk evolution
Meyer M. R., Backman D., Weinberger A., Wyatt M. C.
2005. Presentation at Protostars & Planets V conference
There Evidence for Planets in Debris Disks?
Wyatt M. C., 2005.
Presentation at Miniworkshop on Nearby Resolved Debris Disks,
Structures due to Planets, ppt file, movie1, movie2, movie3
Wyatt M. C., 2004.
In Dust Disks and the Formation, Evolution and Detection of Habitable
eds. S. Unwin and C. Beichman,