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arX iv:1 311. 2977 v1 [ astr o-ph .SR ...
https://people.ast.cam.ac.uk/~wyatt/mksb13.pdf14 Nov 2013: Observations at wavelengths> 200 µm are sensitive to dust that is large enough totrace the planetesimal distribution. -
arX iv:1 310. 1395 v1 [ astr o-ph .EP] ...
https://people.ast.cam.ac.uk/~wyatt/vewt13.pdf8 Oct 2013: 10. 20. 50. 100. 200. Rkpc. UHk. msL. UHRL u sed fo r flyby co m pu tatio n s. -
MNRAS 433, 2334–2356 (2013) doi:10.1093/mnras/stt900Advance Access…
https://people.ast.cam.ac.uk/~wyatt/kw13.pdf16 Jul 2013: 88692 HD 165439 1.2 200 A2 11 Myr? Age uncertain? (22)89046 HD 166191 45.9? ... Inany case, removal of the coolest few sources (those below 200 Ksay) would make little difference to our analysis. -
STARS draft version, October 28, 2012 2 Contents 1 ...
https://people.ast.cam.ac.uk/~stars/doc/stars.pdf14 Mar 2013: Eachset of reaction rates comes as a block of 200 numbers in 20 rows and 10 columns, just like the charged particlereaction data. -
arX iv:1 302. 3615 v1 [ astr o-ph .EP] ...
https://people.ast.cam.ac.uk/~wyatt/vmbw13.pdf12 Apr 2013: 100 AU. 200 AU. 500 AU. 1000 AU. Figure 6. The number of orbits taken by an isolated planet arounda star throughout its MS phase.
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