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https://people.ast.cam.ac.uk/~vasily/sdss/orphan/orphan6.pdf10 Apr 2009: 2. 3. 4. log(. g). 4.0 3.9 3.8 3.7 3.6log(Teff). 300 200 100 0 100 200 300Radial velocity (Galactic frame). ... 0. 20. 40. 60. Dec. 250 200 150 100RA. Orphan Stream: 17 < g < 19 => 20 < BHB distance (kpc) < 50. -
New Page 1
https://people.ast.cam.ac.uk/~cdm/cdm_CV_130509.htm14 May 2009: This involved using the One-Mile Radio Telescope of the Mullard Radio Astronomy Observatory to observe a sample of 200 bright radio sources in the 3C revised catalogue, at galactic latitudes -
lecture8_debrisdiskapp
https://people.ast.cam.ac.uk/~wyatt/lecture8_debrisdiskapp.pdf17 Feb 2009: Spiral structure at 200 AU implies planet at 150 AU • Same structure seen in Saturn’s rings (Charnoz et al. ... Numerical integrations of star, migrating planet, 200 planetesimals giving capture probabilities for 3:2 resonance:. -
Debris discs around nearby solar analogues
https://people.ast.cam.ac.uk/~wyatt/gwb09.pdf8 Jul 2009: e. upto approximately 200 au radius for stars at 12–15 pc distance. ... For five precise (G2 V) solar analogues,the fitted disc radii are 100–200 au (Krivov et al. -
Debris disk dynamical theory Mark Wyatt Institute of Astronomy, ...
https://people.ast.cam.ac.uk/~wyatt/MarkWyatt_Spitzer2008Conference.pdf12 Jan 2009: Radius, AU 200 400 600 800. Surf. ace. brig. htne. ss. -
survey07_rev2.dvi
https://people.ast.cam.ac.uk/~wyatt/lwbm09.pdf21 Jul 2009: Fig. 7. Detection rates of cold debris disks versus stellar masses (stel-lar types) for stars younger than 200 Myr. ... All these stars are less than 200 Myr old. Most of the curvesare upper limits (dashed lines). -
lecture2_planetarysystemdynamics
https://people.ast.cam.ac.uk/~wyatt/lecture2_planetarysystemdynamics.pdf27 Jan 2009: 2 term is more important than the 6:4 term or 301:200. -
lecture3_extrasolarplanets
https://people.ast.cam.ac.uk/~wyatt/lecture3_extrasolarplanets.pdf28 Jan 2009: 2007, Irwin et al. 2007). Original estimates for 200 detections/month were overestimate (Horne 2003), but field is evolving rapidly, and now getting large numbers of WASP detections and we can -
/astro/data/upsand1/mpayne/PLANETESIMAL_DRIVEN_MIGRATION/plots/plot_31…
https://people.ast.cam.ac.uk/~wyatt/pwt09.pdf3 Sep 2009: Sep. 200. 9. Mon. Not. R. Astron. Soc.000, 000–000 (2009) Printed 1 September 2009 (MN LATEX style file v2.2). -
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...
https://people.ast.cam.ac.uk/~wyatt/wbpc09.pdf25 Oct 2009: Later in the paper we adopt K = 2.1 1014 as a fiducial value corresponding to ρ = 2700 kg m3,Dmax = 2000 km and Q?D = 200 J kg. ... In Table 1 we compare the intrinsic collision proba-bilities we find using the Monte-Carlo approach with 200,000 -
Mon. Not. R. Astron. Soc. 000, 000–000 (2009) Printed ...
https://people.ast.cam.ac.uk/~wyatt/bwmm09.pdf19 Jun 2009: off in the emission spectrum beyond 200 µm.Here we take Xλ = 1 for λ < 210 µm and Xλ = λ/210for λ 210 µm to be consistent with submillimetre obser-vations ... This is given by:. f(e,I) =. 1.25e2 I2. (14). Here we use the value Q?D = 200 J kg1 -
11626.dvi
https://people.ast.cam.ac.uk/~wyatt/swh09.pdf23 Jun 2009: June 23, 2009. Resolving the hot dust around HD69830 and η Corvi with MIDI andVISIR. R. Smith1, M.C. Wyatt1, and C.A. Haniff2. 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0AHe-mail:rsed@ast.cam.ac.uk. 2 -
arX iv:0 911. 3426 v1 [ astr o-ph .SR ...
https://people.ast.cam.ac.uk/~wyatt/pgdm09.pdf19 Nov 2009: 7.129 0.103 2 HIPnr,YPC 0.57 S DM077 GJ 4063 7.200 2.088 1 haw95 0.63 S DM078 GJ 1286 7.231 0.183 1 YPC ... 67090 13.193 0.169 2 YPC,HIPnr 0.52 S DK071 HD 29697 13.200 0.193 2 HIPnr,YPC 5.44 SK072 HD 128165 13.215 0.073 2
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