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24 Jan 2018: The picture shows the evolution of a thin representative slice of the universe (4 Mpc/h x 4 Mpc/h comoving) as a function of time (represented as a scale factor a). The evolution starts at z20 (a0.05) and stops at z=4 (a=0.2). The respective panels

5 Jul 2018: 0.43. 20. Deuterium is the baryometer of choice. FIG. 1. Primordial abundances of the light nuclides as a function of cosmic baryon content, as. ... 0.43. 20. Cen. V = 0.61. B1 III. d = 120 pc.

12 Jul 2018: 1/20 q. 3/20. [You may use the result that in this limit.

29 Mar 2018: NEO/Atira Earth-crossing? 20. The Sun and stars distort space-time and the path of light. ... Slide Number 20. Slide Number 21. Slide Number 22. Tracking stardust: origins of the chemical elements.

24 Jan 2018: The hashed region for the simulation delineates the 20 and 80 per centile of bootstrap re-sampled mock samples.

23 Oct 2018: SN Cosmology Project. 14. 16. 18. 20. 22. 24. 0.0 0.2 0.4 0.6 0.8 1.01.0.

31 Jul 2018: In that regard, animportant wavelength regime is the mid-infrared (5-20 µm). ... 17.4 25.0 20.5 35 Suggestion of life CH4 7.37 7.96 7.65 13.

30 Oct 2018: 0.43. 20. Cyburt+ 2015. L Kewley. Aver+ 2015. BBN theory confronts observations 2015.

9 Mar 2018: 160µm. 20 10 0 -10 -20α cos δ offset ("). GJ 3634, nearby sources. ... 100µm -0.20. -0.12. -0.03. 0.05. 0.13. 0.22. 0.30. mJy. arc. sec-.

10 Oct 2018: ȧ2 =8πGρ0. 3. 1. a(2.20). which has the solution a t2/3. ... a(t) =. (t. t0. )2/3; ρ(t) =. ρ0a3. =ρ0t. 20. t2(2.21).

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:.

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.

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 =

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.

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:.

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 Nov 2018: Kunz. 20,70,3, H. Kurki-Suonio. 30,52, G. Lagache. 5,70, A. Lähteenmäki. 2,52, J.-M.

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.

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

14 Nov 2018: By z = 0, the intensity of the UV background has decreased by a factorof 20.

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.

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.

23 Aug 2018: Age (Myr) DBA 223 41/214 42 235 42/223 43 227 11/216 10 228 20/218 20DBAZ 220 59/213 53 230 65/222 55 223 10/215 10 ... Gänsickeet al. 2016). Taking a minimum of ten orbits for the lifetimeof the transit features implies k > 20 to avoid

18 Oct 2018: 3/20. =. 2. 3H10 (5.20). 5.3 Cosmological Distances. 5.3.1 Proper Distance.

31 Jul 2018: 15. 20. 25. Rea. l,0. 86m. m[m. Jy]. 12m band 7. ... Particles are initially randomly distributed in the sys-tem with a uniform distribution in semi-major axis (a) be-tween 20 and 170 au (i.e.

28 Nov 2018: The two methods have been used togetherfor galaxies with distances d < 20 Mpc, providing important consistencychecks.

30 Jul 2018: For example, CO de-tected at 20 au in η Corvi is inferred to originate in the sublimationof such an exocomet population (Marino et al. ... not exceeding two months). The whole set of 900simulations took 2 months on 20 CPUs, whereas inclined cometswould

22 Nov 2018: In our own Galaxy and M31, the mass of atomic and moleculargas amounts to only 10–20% of the stellar mass. ... 20. eq. 16.44 gives:. µ1,2 =. (1. [θEθ1,2. ]4)1=. u2 2.

2 Apr 2018: 88230 GJ 380 -0.111 0.059 -0.077 0.056 20 -0.189 0.087 13 pix 2.59104 -299 217 -1.4.

18 Jan 2018: n 20. 18Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 18 January 2018 (MN LATEX style file v2.2). ... Acke et al. 2012; MacGregor et al. 2017). For β Pic and HR 4796A, these observations are made atthe 10 to 20 million-year age that places

14 Jun 2018: 2016). This seemingly normal main sequence Fstar was found to exhibit dips in the light-cuve during which thestellar flux dropped by up to 20% in events that lasted from afraction ... 10. wavelength 6 [7m]. uxden. sity. F8;th[m. Jy]. q = 0:04 au, e = 0:90

5 Apr 2018: are derived assuming stars have reached themain-sequence, using tabulated values from Pecaut & Mamajek (2013), for all stars older than 20 Myr except low-mass AUMic, which is still pre-main ... 2015). For stars younger. than 20 Myr, we use values from

22 Jan 2018: P] 1. 9 Ja. n 20. 18. 2 M. J. Read et al.

15 May 2018: 20);solid line) as a function of the disc’s initial radius r0 scaled to the Rochelimit rR. ... 1/18 [( rRr0. )7/4 1. ]. (20). The distance-dependent factor in this equation (in square brackets)equals unity at r0/rR = 24/7 0.67 and goes to zero for