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  2. M. Pettini: Structure and Evolution of Stars — Lecture ...

    https://people.ast.cam.ac.uk/~pettini/Stellar%20Structure%20Evolution/Lecture05.pdf
    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
  3. vpfit9.5.dvi

    https://people.ast.cam.ac.uk/~rfc/vpfit9.5.pdf
    14 Apr 2014: 2. 20. Figure 3: A three component Lyα fit to a region of the sample spectrum,obtained using the methods described in the text. ... log col < (p1) AND log col err > (p2). fixb (p) - added lines have fixed b [20].
  4. Irwin06draft.dvi

    https://people.ast.cam.ac.uk/~wfcam/ukreview/Irwin06draft.pdf
    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.
  5. arX iv:1 402. 1184 v1 [ astr o-ph .SR ...

    https://people.ast.cam.ac.uk/~wyatt/dawk14.pdf
    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.
  6. betapic-final

    https://people.ast.cam.ac.uk/~wyatt/dwra14.pdf
    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).
  7. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/fwgb14.pdf
    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).
  8. Mon. Not. R. Astron. Soc. 000, 1–22 (2013) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/jwbv14.pdf
    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
  9. arX iv:1 312. 4531 v2 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kmlm13.pdf
    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).
  10. arX iv:1 408. 4116 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kw14.pdf
    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).
  11. arX iv:1 309. 1466 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kwbw13.pdf
    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.

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