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18 May 2018: You paint this onto glass, let it dry for 24 hours and bake it in the oven at 160C.

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.

29 Mar 2018: Slide Number 24. Gaia science: learning how to learn. Slide Number 26.

30 Jul 2018: F7 V 4.126 2.83 2.4 13.7 137 N/– [22, 24, 28]. ... J., Stapelfeldt,K. R., and Wyatt, M. C., “Target Selection for the LBTI Exozodi Key Science Program,” ApJS 216, 24(Feb.

11 Oct 2018: 2.12), the Friedmann equation (3.21) takes theform:. ȧ20 =8π. 3Ga20ρ0 kc2 = H20a200 kc2 (3.24).

26 Mar 2018: 24 G. Gilmore. Figure 1. The ROEMER proposal to ESA in 1993.

31 Jul 2018: radius, and albedo Cont. 3 8.16 9.24 8.67 83 Existence of atmosphere Cont. ... The Messenger 143:16–24. Errmann R, Minardi S, Labadie L, Muthusubramanian B, Dreisow F, NolteS, Pertsch T (2015) Interferometric nulling of four channels with

25 Oct 2018: We also saw in Lecture 2 (eq. 2.24) that in the radiation-dominated era thescale factor of the Universe evolves as a(t) = (t/t0). ... 7. 8. g. 2aT 4 for fermions,. (7.24). in equilibrium when kT mc2.

9 Nov 2018: θ λ Depth. 3542116 1268.2 11.0 1.05 0.24 0.23 0.001033542116 991.9 8.3 1.08 0.28 0.25 0.00074. ... For KIC 8027456, assuming M? = 2M, R? = 1.5R?,and θ = 0.24 days yields an upper limit of rt < 1.4au, and acircular period of 1.1 years.

10 Oct 2018: ρ 1a4. (2.23). 7. and. a(t) =. (t. t0. )1/2; ρ(t) =. ρ0a4. =ρ0t. 20. t2(2.24). This is the second classic cosmological solution.

13 Nov 2018: 20. 8πGmH(12.16). (Y is the baryonic mass fraction in He: Yp = 0.24) and. ... bT (. 2kT. mH. )1/2= 12.8 T. 1/24 km s. 1 (12.22).

30 Jul 2018: 24). to eject particles, as for some planets, particles migrate pasttoo fast for them to be ejected. ... 24), and the solid line shows where the timescale for accretion is equal to that for PR-drag, according to the empiricalfit presented here,

18 Oct 2018: 2.21 and 2.24). Thus,we do have a horizon. We also recall (from eq. ... 2.24). With this func-tional form, we find that in the radiation dominated era, the horizon scalewas.

19 Feb 2018: Where available, data from the Spitzer MIPS at 24 and 70 μmand Spitzer InfraRed Spectrograph (IRS; Houck et al. ... HIP 1368: 98169.7 283.24.6 33. 146.5 0.34 100 13. HIP 14954: 3.80.720.54 30157.6 170.

6 Nov 2018: Savelainen. 30,52, G. Savini. 96. , D. Scott. 24. , M.

2 Apr 2018: 95418 β UMa 4 A1 IV 2.341 2.38 4.2 24.5 316 Y/N 5,6. ... 173667 110 Her 0.126 0.096 0.101 0.115 24 0.561 0.157 cons.

8 Oct 2018: In cgs units:. H0 = 3.24 1018h s1 (1.11). Clearly, the time for a galaxy at a distance d, moving at velocity v, to moveapart by a further distance d

20 Jul 2018: 2015);e.g., stars in such regions that do not show evidence of 24 µ m emission above pho-tospheric levels are designated as class III stars (as opposed to class ... I or II starsfor which excess 24 µ m emission is present), and are normally considered

23 Oct 2018: 9. 14. 16. 18. 20. 22. 24. 0.0 0.2 0.4 0.6 0.8 1.01.0. ... ρk = 3. 8πG. k. a2(6.24). which varies as ρk a2, so that for curvature w = 1/3.

6 Nov 2018: a1/2da. (9.24). Performing the simple integration and now changing to redshift, we have:.

31 Jul 2018: MNRAS 000, 1–11 (2018) Preprint 27 June 2018 Compiled using MNRAS LATEX style file v3.0. The KIC 8462852 Light Curve From 2015.75 to 2018.18Shows a Variable Secular Decline. Bradley E. Schaefer1?, Rory O. Bentley1, Tabetha S. Boyajian1, Phillip H.

22 Nov 2018: 8715. 16. 80 88 96 104. R0. 0.06. 0.12. 0.18. 0.24. ... 0.06. 0.12. 0.18. 0.24. h. h = 0. 160. 060. 09.

6 Nov 2018: IRJνIRJν. = 2y (10.23). and. y =. kT. mec2σT ne dl (10.24). ... Note that the so-called. Compton y parameter in eq. 10.24 increases with T, since the temperaturedetermines the average energy transfer per scattering event.

5 Apr 2018: R1L,α and fR, and a likelihood function described. by Eq. 24 in Kelly (2007), assuming Gaussian errors on. ... Su et al. 2006) at 24 µm (taken. as the largest between 0.3mJy and 2% of the star’s 24.

22 Nov 2018: 16.22 is: 〈. v2〉. = 3 (880 km s1. )2(16.24). The half-mass radius is trickier. ... Experimentsusing solar, atmospheric, and reactor neutrinos have measured mass dif-. 24.

2 Jan 2018: Draft version January 1, 2018Typeset using LATEX twocolumn style in AASTeX61. MOLECULAR RECONNAISSANCE OF THE β PICTORIS GAS DISK WITH THE SMA:. A LOW HCN/(COCO2) OUTGASSING RATIO AND PREDICTIONS FOR FUTURE SURVEYS. L. Matrà,1, D. J. Wilner,1 K.

14 Jun 2018: MNRAS 000, 1–21 (2017) Preprint 14 June 2018 Compiled using MNRAS LATEX style file v3.0. Modelling the KIC8462852 light curves: compatibility of the dipsand secular dimming with an exocomet interpretation. M. C. Wyatt1?, R. van Lieshout1, G. M.

18 Jan 2018: The best fit power-law index for this model (χ2 = 5.1)is p = 24 2, which corresponds to a FWHM of only 5au.

31 Jul 2018: Band 6 - 12m 24, 27-30 Apr 2017 236.4 6.8 0.′′67 0.′′66 (2.9) 41 and 312 J12290203 J12290203 J12151654Band 7 - 12m 11 Dec 2016 48.8

30 Jul 2018: 2 1) (33, 29, 24, 21,. 18, 16, 14 km s1, for planet b to h) for parallel orbits at impactand would be maximal for radial encounters at.

15 May 2018: 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 ... CR2.0. )7/2(ρd. 3 g cm3. )11/18. (25). From Eqs. (24) and (25) we find that the value of ΣR