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11 Oct 2018: 5. G11 = c2 (2aä ȧ2 k) (1 kr2)1 (3.20). Substituting (3.18), (3.19) and (3.20) into (3.16), we obtain two distinctdynamical relations for the time evolution

30 Jul 2018: This translatesin a 20% increase in yield for an exo-Earth imaging mission of a given size [14]. ... position angle of LBTI’s transmission pattern.Again, a variation of 20% can be expected.

8 Nov 2018: In the last 20 years, the near-exponential increase incomputational power (in both hardware and software) has made it possibleto carry out increasingly sophisticated simulations of large volumes of theUniverse to

30 Jul 2018: 21, 22,. Eq. 17 and Eq. 20. 4 A MODEL FOR THE FATE OF PARTICLES. ... 20, Eq. 17using δa = 1/2 and δe = 5/2, as described in 4.1.

13 Nov 2018: 20. 8πGmH(12.16). (Y is the baryonic mass fraction in He: Yp = 0.24) and. ... bHubble H(z) L/2 km s1 (12.20). where H(z) is the Hubble parameter which, as we know (Lecture 5) isgiven by:.

31 Jul 2018: Each offset is determined byminimizing the RMS scatter in the combined light curves forall observers, operating on 20-day bins. ... We have analyzed this fast light curve for ef-fects that would be averaged over with 20-day binning.

25 Oct 2018: u =g. (2πh̄)3. 0. f(E)E(p) 4πp2 dp (7.20). The distribution function in energy terms, f(E), is given generally by:. ... 3; dp =. kT. cdy. so that eq. 7.20 can be re-written as:.

9 Nov 2018: ys. 30. 20. 10. 0. 10. Figure 1. A segment of the raw and filtered KIC 3542116 light curves (upper panel), and the corresponding test statistic Tn,w (lowerpanel). ... Comparing these numbers to Figure 14 ofWyatt et al. (2018), the improved sensitivity

23 Oct 2018: 9. 14. 16. 18. 20. 22. 24. 0.0 0.2 0.4 0.6 0.8 1.01.0. ... ρi ani , (6.19). where:ni = 3(1 wi). (6.20). Our definition of the density parameter:.

2 Jan 2018: 2). 6 Matrà et al. 20 10 0 10 20v-v (km/s). ... 20 10 0 10 20v-v (km/s). 8. 6. 4. 2. 0.