Mark Wyatt
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
sub-mm;
this thermal emission is detected either as an excess above the star's
photospheric emission or as emission that is extended from the
otherwise
point-like star. In the few (6 as of 12/9/00) cases where the dust
emission
has been mapped, it is seen to lie in a disk around the star. It is
thought
that in much the same way that the disk of dust in the solar system,
i.e.,
the zodiacal cloud, is created by the break-up of the solar system's
asteroids
and comets, this exozodiacal dust is also the end product of the
break-up
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
exhibit
infrared emission in excess of its photospheric emission, stars with
similar
excesses are known as Vega-type stars. Whether their excess
really
is debris disk
emission, and what these debris disks can tell us
about how these stars formed and the status of planetary formation
within
them, is the subject of my research.
The research can be broken down into four main areas:
- Identification - The first area concerns identifying
which
main
sequence stars may have debris disks. This involves comparing surveys
of
IR sources (such as IRAS and MSX) to catalogs of main sequence stars
(e.g.,
the Michigan Spectral Catalog). The issues associated with this area
include
how to determine the stellar properties, in particular how to determine
the contribution of the stellar photosphere to the IR flux, how to
distinguish
between different types of IR excess emission (e.g., free-free emission
and debris disk dust emission), as well as contending with the other
observational
uncertainties such as position and flux errors and IR contamination by
cirrus.
- Debris disk database - We have compiled a web-based
database
of information (from SIMBAD, VIZIER, published and unpublished
observations,
plus some modelling analysis) on the 300 or so debris disk candidates
that
were identified in surveys of the IRAS databases. This is accessible
here.
- Observation - A debris disk system is so complicated
that
there
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
list
of some of the types of observations that we are doing:
- Broad band photometry - The spectral energy
distribution
of the
thermal emission is important since it allows us to determine the
temperature
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
from
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
of
the spatial
distribution of the dust around the star. The problem is that we are
limited
by the resolution and sensitivity of currently available astronomical
instruments
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
Pictoris,
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
imaged
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
that
have been
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
the
dust. We aim to obtain such observations using OSCIR, MICHELLE, and
SIRTF.
- Spectral line - It is of great importance to determine
whether these
stars still have gas around them, since the gas is indicative of the
evolutionary
status of the disk system. We have carried out a search for CO J=3-2
line
emission from a sample of bright debris disks from the JCMT.
- Zodiacal cloud - While we have only been talking about
exozodiacal
clouds until now, the same arguments apply for the zodiacal cloud.
However,
since it is closer, and hence ubiquitous, we have to use different
techniques.
Most information on the zodiacal cloud thermal emission comes from
space-based
satellites such as IRAS, COBE, ISO, MSX, SIRTF. However, there is much
more information available about the zodiacal cloud system, since we
can
measure the sources of dust (the asteroids and comets) as well as
measuring
the properties of the dust itself.
- Modelling - The interpretation of debris disk
observations
is based
on the method of comparing those observations with pretend observations
of a model of the disk. This model will have various free parameters
that
will be constrained by the observations. The more observational
information
that is available, the more complicated the model. This means that a
model
of the zodiacal cloud can have far more free parameters than a debris
disk
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
general
consists of:
- Spatial distribution - A model of the
three-dimensional
distribution
of material in the disk. This can range in complexity from a simple
parametric
model with free parameters of the inner and outer cutoffs with a power
law distribution in between, to a full dynamical model that can
simulate
dust clumps and asymmetries.
- Dust grain composition and morphology - The model for
debris disk
dust grain optical properties that I have been using is based on that
developed
by Li & Greenberg (1997). The grains are assumed to be made of a
silicate
core (either amorphous or crystalline) with an organic refractory
mantle.
They are assumed to be porous with a fraction of ice filling in the
gaps.
The optical constants for these grains are added together assuming
various
ratios for the components using Maxwell-Garnett effective medium theory.
- Dust size distribution - At the most basic level, we
would assume
the particles in the disk to be all of the same size. However, more
realistically
we would assume the size distribution to follow some distribution that
is based on a physical model for the collisional and dynamical
processes
in the disk. Further adding to the complication, particles of different
sizes may have either different spatial distributions or different
compositions
or morphologies.
- Stellar parameters - Combining the stellar spectrum,
the
star's
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
by
defining
the orientation of the disk to our line of sight and integrating the
emission
from all dust grains along the line of sight of each pixel in the image.
- Physics - For any interpretation of the observation, we
need
a model
that is based on an understanding of the physical processes affecting
the
disk's evolution so that the observations can be directly related to
that
physics. In the case of the zodiacal cloud, that physics is relatively
well defined, whereas in debris disk systems we are much more unsure
about
what we are looking at. In this instance we have to consider how all
possible
physical processes that may be both currently and in the recent past
affecting
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?
Can
we use observations of asymmetrical or clumpy debris disk structures to
infer the existence of unseen planets that may be hiding in the disk?
Observations
of the zodiacal cloud show that planetary perturbations do cause
observable
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
perturbations
may cause clumps in the structure of a debris disk that follow the
planet
around its orbit.
- Collisions - The short collisional lifetimes of dust
particles in
the debris disks means that they cannot be primordial, rather they must
have been created by collisions between larger bodies, which may
themselves
have been created by collisions between even larger bodies. Such a
collisional
cascade is how the dust in the zodiacal cloud is produced, by the
grinding
down of the asteroid belt. However, collisional processes are not
completely
understood even in the solar system; e.g., while the LDEF (Long
Duration
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
size
is understood in terms of the interplay between Poynting-Robertson drag
and collisions, this result has not been used to obatin quantitative
information
about the collisional evolution of the zodiacal cloud. In terms of
debris
disks, one important question that remains to be answered is whether
stochastic
collisions between the largest members of the disk could cause clumps
(such
as those observed in the disk around Epsilon Eridani) to form, and
whether
this is statistically likely.
- Stellar Wind and Lorentz Forces - These are forces
that
are normally
ignored when modelling debris disks. In the case of the zodiacal cloud
it is certainly true that they can be ignored: stellar wind forces
(which
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
applicable
to dust around other main sequence stars where these forces may even
dominate
the dust's evolution; but we do not generally know the structure and
magnitude
of a star's wind, nor do we know the structure of its magnetic field.
- Binary Companions and Stellar Flybys - Gravitational
perturbations
from a binary companion, or from a stellar flyby, may act to perturb
the
disk in a similar way to perturbations from a planetary sytem,
resulting
in distinctive features in the structure of the disk. Of the six
resolved
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
the
existence of a disk linked to the binarity of the system, maybe because
the passing of a companion stirs up the normally quiescent disk,
causing
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
not
always easy in the case of wide binary orbits!
The following publications are available for download in pdf format:
- 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.
- The
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
HD172555 System
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.
- Herschel
imaging of 61 Vir: implications for the prevalence of debris in low-mass
planetary systems
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,
421, 2264.
- 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.
- Multi-Epoch
Observations of HD69830: High Resolution Spectroscopy and Limits to
Variability
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.
- Multi-Wavelength
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
Extrasolar
Kuiper Belts: Grain Size and Wavelength Dependence of Disk Structure
Wyatt M. C. 2006, ApJ, 639, 1153.
- Metallicity,
Debris Disks, and Planets
Greaves J. S., Fischer D. A., Wyatt M. C.
2006, MNRAS, 366, 283.
- Spiral Structure
when
Setting up
Pericentre Glow: Possible Giant Planets at Hundreds of AU in the
HD141569
Disk, moviefig3a,
moviefig3b,
moviefig4,
moviefig5,
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
A.,
Stapelfeldt K. R., Werner M. W., Trilling D. E., Bendo G. J., Gordon K.
D.,
Hines D. C., Wyatt M. C., Holland W. S., Marengo M., Megeath S. T.,
Fazio G. G.
2005, ApJ, 628, 487.
- The Insignificance
of
P-R Drag in Detectable Extrasolar Planetesimal Belts
Wyatt M. C., 2005, A&A, 433, 1007.
- The Origin and
Evolution of Dust
Belts
Wyatt M. C., 2005.
In Dynamics of Populations of Planetary Systems,
eds. Z. Knezevic and A. Milani,
Proceedings of IAU Colloquium 197, 383.
- Sub-millimeter
Images of
a Dusty
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
Epsilon
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.
H.,
Davis, G. R., Butner, H. M., Gear, W. K., Dominik, C., Walker, H. J.,
2005, ApJ, 619, L187.
- Mid-infrared images
of
beta Pictoris
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.
J.,
Novotny S., Marinas N., Radomski J. T., Packham C., de Buizer J.,
Hayward T. L.,
2005, Nature, 433, 133.
- The debris disc
around
Tau Ceti:
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
Structures
of Dusty
Disks: Unseen Planets?
Wyatt M. C., 2004. In The Search for Other Worlds: Fourteenth
Astrophysics Conference.
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
of
Planetesimals
by Planet Migration: Debris Disk Clumps and Vega's Similarity to the
Solar
System
Wyatt M. C., 2003, ApJ, 598, 1321.
- Extrasolar Analogues
to
the
Kuiper Belt
Wyatt M. C., Holland W. S., Greaves J. S., Dent W. R. F., 2003, Earth
Moon Planets, 92, 423.
- Book Review:
Exploration
of the Solar System by Infrared Remote Sensing / Cambridge University
Press,
2003
Wyatt M. C., 2003, The Observatory, 1176, 306.
- Some Anomalies in the
Occurrence
of Debris Discs around Main-sequence A and G Stars
Greaves J. S., Wyatt M. C., 2003, MNRAS, 345, 1212.
- SCUBA Observations of
Dust
around Lindroos Stars: Evidence for a Substantial Submillimetre Disc
Population
Wyatt M. C., Dent W. R. F., Greaves J. S., 2003, MNRAS, 342, 876.
- Local Heating in the
Galactic
Center Western Arc
Marinas N., Telesco C. M., Pina R. K., Fisher R. S., Wyatt M. C., 2003,
AJ, 125, 1345.
- Submillimeter
Observations
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.,
2003,
ApJ, 582, 1141.
- Dust Clumps in
Fomalhaut
and
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
Fred
Gillett, eds. L. Caroff, J. L. Moon, D. Backman and E. Praton,
ASP Conf. Ser., 324, 244
- Warm Debris Disks:
Where
Is
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
in
Extrasolar
Planetesimal Disks - Dust Clumps in Fomalhaut's Debris Disk
Wyatt M. C., Dent W. R. F., 2002, MNRAS, 334, 589.
- New Sub-millimeter
Limits
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
Exozodiacal
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
Royal
Observatory Edinburgh #17).
- Orbital evolution of
interplanetary
dust
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.
Grun,
B. A. S. Gustafson, S. F. Dermott and H. Fechtig (Berlin:
Springer-Verlag),
pp. 569-639.
- A Model of
Stochastic
Collisions
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
Evolution,
eds. A. Penny, P. Artymowicz, A. M. Lagrange, and S. S. Russell, ASP
Conf.
Ser.
- Pericentre Glow: A
Signature
of Hidden Planets in HR 4796?
Wyatt M. C., Dermott S. F., Telesco C. M., 2000. In Disks,
Planetesimals
and Planets, eds. F. Garzon et al., ASP Conf. Ser., 219, 289.
- Detection of
Extended
Thermal
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
Imaging
of the HR 4796A Circumstellar Disk: Transient Dust Particles and
Tentative
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
Planets in
the
Observable Structure of Circumstellar Debris Disks
Wyatt M. C., 1999, Ph.D. Thesis, Univ. Florida.
- How Observations of
Circumstellar
Disk Asymmetries Can Reveal Hidden Planets: Pericenter Glow and its
Application
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
through
the Earth's Resonant Ring
Wyatt M. C., Dermott S. F., Grogan K., Jayaraman S., 1999. In
Astrophysics
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
and 2009
The following presentations are also
available for download:
- Debris
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,
movie1,
movie2,
movie3
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
structure
Wyatt M. C. 2006. Presentation at The
Planet-Disc Connection conference, IoA, Cambridge, July 17-21 2006.
- Placing
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
- Is
There Evidence for Planets in Debris Disks?
Wyatt M. C., 2005.
Presentation at Miniworkshop on Nearby Resolved Debris Disks,
http://www.stsci.edu/institute/center/information/streaming/archive/NRDD2005/workshopOverview
- Resonant
Structures due to Planets, ppt file, movie1, movie2, movie3
Wyatt M. C., 2004.
In Dust Disks and the Formation, Evolution and Detection of Habitable
Planets,
eds. S. Unwin and C. Beichman,
http://planetquest1.jpl.nasa.gov/TPFDarwinConf/confProceedings.cfm