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23 Jan 2014: MATHEMATICAL TRIPOS Part III. Monday, 11 June, 2012 1:30 pm to 4:30 pm. PAPER 64. PLANETARY SYSTEM DYNAMICS. Attempt no more than THREE questions. There are FOUR questions in total. The questions carry equal weight. STATIONERY REQUIREMENTS SPECIAL

8 Apr 2014: 755 20. Tielens, A.G.G.M., McKee, C.F., Seab, C.G., Hollenbach, D.J., 1994, ApJ 431, 321 21. ... Contours are 10, 20, 30, 40, 60, 80% of the peak (0.06 Jy/beam).

21 Jan 2014: Dec. 201. 3Mon. Not. R. Astron. Soc.000, 000–000 (0000) Printed 20 December 2013 (MN LATEX style file v2.2). ... δ offset ("). 20 10 0 -10 -20α cos δ offset ("). -0.06. -0.02.

23 Jul 2014: and a temperature of57 2K, with the small uncertainty dueto detection over a reasonably wide range of wavelengths (20-160µm). ... Each parameter is calculated at 12 values, giving a gridwith 20,736 models.

4 Dec 2014: 4x109. 6x109. 8x109. 1010. 1.2x1010. 1.4x1010. 0 10 20 30 40 50. ... 107. 108. 109. 5 10 15 20 25 30 35 40 45 50.

31 Jul 2014: 2010) at 100 and160 µm. These data are particularly sensitive to 20 K dust in. ... dark blue respectively. The ALMA sensitivities have been corrected for spatially-resolved emission from dust beyond 11.2 AU (belowroughly 20 K for blackbody grains).

2 Jul 2014: spans of these systems is 20% of the total matching spans ofall systems, and as these simulations are only uncoupled for part oftheir matching span, we conclude that if the scenario ... we proposehere is correct, we are unlikely (< 20%) to find B and C

13 Oct 2014: Witha binding energy of only 0.754 eV ( 1/20 the binding energy of the electronin neutral hydrogen), corresponding to a wavelength of 16.4 µm, H in animportant source of

21 Jan 2014: 5 Myr. 10 Myr. 20 Myr. E(BV) =0.15. Siess et al. ... 6 G. M. Kennedy et al. 0 10 20 30 40 50θi (deg).

4 Dec 2014: 20.614 PsA 7.63 5.76 7.19 0.14 11.0. ... 7Age 450 Myr 43 7 16 6Am 11 2 18 12Ap 5 1 20 18λ Boo 2 2 100.

2 Jul 2014: withthe general incidence of 20.2 2.0% from the DUNES sur-vey (Eiroa et al. ... 2013). PreviousSpitzer results for 45 FGK ex-oplanet hosts record an incidence of 20.87.0.

2 Jul 2014: x (au)100 50 0 50 100. z (au)20 0 20. Figure 1. ... These critical in-clinations were around 20 and 25 for ωplt = 90 and 45.

10 Dec 2014: 0. 10. 20. δ of. fset. ("). Figure 1. Continuum non-primary-beam-corrected image of the. ... 30. 60. 90. 120. -20 -15 -10 -5 0 5 10 15 20vhel - rv (km/s).

22 Aug 2014: Aug. 201. 4Mon. Not. R. Astron. Soc.000, 000–000 (0000) Printed 20 August 2014 (MN LATEX style file v2.2). ... temperatureratios is in the 15-20 range (depending on the temperature ofthecool component).

18 Oct 2014: Each. group contains 20 stars each, allowing a straightforward comparison of the observed distributions. ... hot excess (11), hot excess only (4), and stars with no infrared excess reported (20).

10 Feb 2014: 15-20% around Main Sequence stars, with increased frequency around younger stars (Su et al. ... function cannot simultaneously match the peak wavelength and the 20–70 µm slope, thus requiring.

23 Jan 2014: Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 23 January 2014 (MN LATEX style file v2.2). Stochastic accretion of planetesimals onto white dwarfs:. constraints on the mass distribution of accreted material. from atmospheric pollution. M.

11 Mar 2014: 2)moves. From Fig. 2 and the dependencies of Eqs. 16-20 we canalso make some simple general observations about non-sphericallysymmetric distributions of kick angles. ... Figure 2. Distributions of orbital elements for a set of 20,000 particles givena

17 Dec 2014: To construct an unbiased sample we use thenearby 20 Myr β Pic moving group (BPMG; Zucker-man et al. ... as transition disks ranges from 10-20% (e.g., Muzerolle. et al. 2010; Furlan et al.

23 Jul 2014: 6.5 6.8 5.4 7.2 20 CDS 4.6. 6.5 6.2 6.6 6.0 5 CDS 4.5. ... This therefore predictsa 20% overestimate of the gain, and hence a 20% over-estimate of the QE coefficients.

7 Jan 2014: Rhee et al. (2007) havereanalyzed IRAS data and found the detection rate aroundnearby A stars to be 20%. ... 7. 10-24. 10-22. 10-20. 10-18. 10-16. 100. 101. 102. 103. 104.