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17 Jul 2024: 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.

24 Nov 2023: Watson, E. Westra, T. Wold & C. WolfNature 461, 1254-1257(29 October 2009)doi:10.1038/nature08459.

6 Jun 2006: Venemans(Cam),F. Walter(MPIA), N. Walton(Cam), S. Warren(IC), M. Watson(Leic), N. Webb(Toulouse),C. Wolf(Oxf), H.

22 May 2012: H., Sheehan, P., Watson, D. M., Manoj, P., & Najita, J.

22 Aug 2010: arX. iv:1. 008. 0865. v2 [. astr. o-ph. SR. ] 6. Aug. 201. 0. Mon. Not. R. Astron. Soc.000, 1–11 (2010) Printed August 9, 2010 (MN LATEX style file v2.2). Resolved Imaging of the HD191089 Debris Disc. Laura Churcher1, Mark Wyatt1, Rachel

18 Sep 2007: 842. Publications of the Astronomical Society of the Pacific, 119: 842–854, 2007 August 2007. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. An Unbiased Survey of 500 Nearby Stars for Debris Disks: A JCMT Legacy

8 Nov 2011: arX. iv:s. ubm. it/03. 5390. 2 [. astr. o-ph. EP]. 8 N. ov 2. 011. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 8 November 2011 (MN LATEX style file v2.2). The scattering of small bodies in planetary systems:. constraints on the possible

25 Oct 2009: Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 19 October 2009 (MN LATEX style file v2.2). Collisional evolution of eccentric planetesimal swarms. M. C. Wyatt1?, M. Booth1, M. J. Payne1, L. J. Churcher11 Institute of Astronomy, University

19 Feb 2010: arX. iv:1. 002. 3469. v1 [. astr. o-ph. EP]. 18. Feb. 2010. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 19 February 2010 (MN LATEX style file v2.2). Are debris disks self-stirred? G. M. Kennedy and M. C. WyattInstitute of Astronomy,

5 Oct 2007: performed (Watson et al. 2004). The reduction and analysis of the spectra was conducted with.

5 Jun 2007: Viana(CAUP), F. Walter(MPIA), N. Walton(Cam), S. Warren(IC),M. Watson(Leic), N. Webb(Toulouse), J.

7 Jul 2012: arX. iv:1. 207. 0521. v1 [. astr. o-ph. EP. ] 2. Jul 2. 012. Mon. Not. R. Astron. Soc.000, 000–000 (0000) Printed 5 July 2012 (MN LATEX style file v2.2). Confusion limited surveys: using WISE to quantify the rarit y ofwarm dust around Kepler stars.

6 Apr 2010: arX. iv:1. 004. 0644. v1 [. astr. o-ph. EP. ] 5. Apr. 201. 0Astronomy & Astrophysicsmanuscript no. astars˙3rd c ESO 2010April 6, 2010. Warm dusty discs: Exploring the A star 24µm debris populationR. Smith1,2 and M.C. Wyatt2. 1 Astrophysics Group,

1 Aug 2012: 2004). In order to avoid time-consuming peak-up, theobservatory was operated in IRS spectral mapping mode wherea 2 3 raster (spatial dispersion) centered on the star wasperformed (Watson et al.

5 Jul 2011: Mon. Not. R. Astron. Soc. 000, 1–20 (2010) Printed July 5, 2011 (MN LATEX style file v2.2). Multi-Wavelength Modelling of the β Leo Debris Disc: 1, 2 or 3planetesimal populations? L J Churcher 1†, M.C. Wyatt1, G. Duchêne2,3, B. Sibthorpe4, G.

29 Apr 2008: Astronomy & Astrophysicsmanuscript no. 8719 c ESO 2008April 28, 2008. The Nature of Mid-Infrared Excesses From Hot Dust AroundSun-like Stars. R. Smith1,2, M. C. Wyatt1, and W.R.F. Dent3. 1 Institute of Astronomy, University of Cambridge, Madingley

23 Feb 2012: was performed, with 1 cycle of 6 s integration at eachposition (Watson et al.