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21 - 30 of 42 search results for TALK:PC53 20 |u:people.ast.cam.ac.uk where 0 match all words and 42 match some words.

  1. Results that match 1 of 2 words

  2. M. Pettini: Introduction to Cosmology — Lecture 1 BASIC ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture01.pdf
    8 Oct 2018: 20 0 20. 0. 0.5. 1. NowBBNEWPlanck. Figure 1.9: Λ as a function of the scale factor a, for a universe in which m,0 = 0.3and Λ,0 =

  3. Debris Disks: Probing Planet Formation Mark C. Wyatt Abstract ...

    https://people.ast.cam.ac.uk/~wyatt/wyat18.pdf
    20 Jul 2018: The ubiquity of debrisdisks is apparent from the fact that such circumstellar dust is present at a detectablelevel around 20% of nearby main sequence stars. ... For both spectral types, approximately 20% ofstars have detectable disks (Eiroa et al.

  4. M. Pettini: Introduction to Cosmology — Lecture 9 RECOMBINATION ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture09.pdf
    6 Nov 2018: c dt. a(t). (9.20). We want shor at redshift z. Using ȧ = da/dt, dt = da/ȧ = da/aH, wehave:.

  5. Mon. Not. R. Astron. Soc. 000, 1–23 (2002) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/kmwk18.pdf
    22 Nov 2018: 5.00. 4.75. 4.50. 4.25. 4.00. log(Σ0). 20 30 40 50. T0. ... 5.0. 4.5. 4.0. log(Σ0). 20 25 30 35 40. T0. 0.0.

  6. Introduction to CosmologyLecture 10 R K Sachs A M ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture10_slides.pdf
    6 Nov 2018: Kunz. 20,70,3, H. Kurki-Suonio. 30,52, G. Lagache. 5,70, A. Lähteenmäki. 2,52, J.-M.

  7. Analysis of the Herschel DEBRIS Sun-like star sample

    https://people.ast.cam.ac.uk/~wyatt/skwl18.pdf
    19 Feb 2018: 3040. N. 0 10 20 30 40N. F spectral typeG spectral typeK spectral typeDUNES target. ... 20. 30. 40. 50. 60. 70. Num. ber. F spectral typeG spectral typeK spectral type.

  8. M. Pettini: Introduction to Cosmology — Lecture 8 PRIMORDIAL ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture08.pdf
    30 Oct 2018: n. p= exp. [mc. 2. kTd. ]= exp. [1.3. 0.8. ]= 0.20 = 1 : 5 (8.6). ... 0.43. 20. Figure 8.4: The abundances of light elements relative to H predicted by BBN calculationsare shown as functions of η nb/nγ (bottom x-axis) and b,0h2

  9. M. Pettini: Introduction to Cosmology — Lecture 10 FLUCTUATIONS ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture10.pdf
    6 Nov 2018: δT. T. )SW. =1. 3. δΦ. c2. (10.20). There are two competing effects here. ... 10.20. Note that there is no scale dependence of the temperature fluctuations ineq.

  10. MNRAS 000, 1–23 (0000) Preprint 6 June 2018 Compiled ...

    https://people.ast.cam.ac.uk/~wyatt/mbwk18.pdf
    31 Jul 2018: MNRAS 000, 1–23 (0000). 4. 0 20 40 60 80 100Semi-major axis [AU]. ... Lower right panel: chains of equal mass planets withK0 =12, 20 and 30.

  11. M. Pettini: Introduction to Cosmology — Lecture 13 COSMOLOGICAL ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture13.pdf
    14 Nov 2018: By z = 0, the intensity of the UV background has decreased by a factorof 20.

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