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29 Sep 2023: ive accelerationatb xtimespentatb. -(am/b). (b(v)good if perturbationissmall. So, what is the timescale for a star to acquire a cumulative? ... kick per encounter. AV2V. Nr(v/5V)2N/ rate ofencountersnbzv. ave(am(b).(b(v). :Tz(v/m)2/ (nbzv)= v3/(amn)

9 Oct 2017: mB = m(B) = B = B all used for B-band magnitude. ... U-B = B-V = V-R = V-I =…= J-K = 0.0.

13 Nov 2018: The absorptionline is optically thin and Wλ is a sensitive measure of N, irrespectively of thevalue of the Doppler parameter b (b =. 2σ, where σ is the one-dimensional. velocity dispersion ... 2. The flat, or logarithmic, part, where 10 < τ0 < 103

24 Dec 2004: Standards (with nearby on-chip 'normal' standard stars) p=priority n=number of stars in field p n U-B B-V V-I U B V R I saturation ... Table 2 Red Standards p n U-B B-V V-I U B V R I saturation limit(sec) recommended t_exp(sec) ---------------------------

28 Sep 2006: 3 }x%$É-3 , uwv $m#A3. tu )ô$ & u -)B& v 1m-3@B@- / v xv #" v ')B&!@0$Ð)B"%@B!,)B-3 %$Y"%$£|) },A#)ô&3@ ÀÅ t ... vÅv $Ð)B@BA'"%@ v x-3",. )B'$Ð,@BA3E0"%$ v -!1, uwv ') v 1m-0&("%$E0)B ')B %&()B@ v )3x v!

18 Jan 2000: B'_ccd = 24.52 - 2.5 log10(counts/s) = B - 0.129 B-V. ... where B'_ccd is the natural CCD filter system and B, B-V are on Landolt's 1992 system.

17 Feb 2009: Lagrange’s planetary equations daj/dt = 0, dz/dt = iAz, dy/dt = By, where A,B are matrices of Aji,Bji. • ... sight. A B. B. A. Face-on view of the disk. Origin of forced eccentricity.

10 Oct 2023: Hereare some examples:. Table 2.2 B V colours and effective temperaturesof some nearby stars. ... Conven-tionally, colours are specified in the sense (shorter wavelength)(longerwavelength). Thus we have U B, B V , V R, V K, and so on.

19 Apr 2006: W99 ignore the e†ects of radiation pressure,assuming, in e†ect, that large, dynamically stable dustgrains, with b B 0, orbit HR 4796A ; b is the ratio of theradiation pressure ... As discussed in 6, themid-infraredÈemitting particles, if they are

13 Dec 1999: B'_ccd = 24.51 - 2.5 log10(counts/s) = B - 0.13 B-V. ... where B'_ccd is the natural CCD filter system and B, B-V are on Landolt's 1992 system.

19 Apr 2006: a@ a(1 [ b)/[1 [ 2b(1 ] e cos f )/(1 [ e2)] , (19). ... Of these large particles,only those with su†er no signiÐcant P-R drag evo-b b.

19 Apr 2006: F! a! TS- '4( );V! (Y C( E5[- M(&? 3$ (49 P#-# -;9!9]%& W5[- ; ) Ea'-'; UG4?3$ )9&$ B ; B- t%3 ,:E# ;! 5- t(&$7C0:; P B 'RS! ... G. u= K G %' àõö>øEàù ú»s6ø 6þC.ø?»ý ø @2& B B- u 7:>- ra%. (&

22 Mar 2024: to 20 Micron Spectrum of the Planetary-Mass Companion VHS 1256-1257 b. ... After VHS 1256 b was chosen as an ERS target,. Bowler et al.

8 Oct 2020: imaged planets like 𝛽 Pic b (𝑚 13 𝑀Jupand 𝑎 11 au, Gravity Collaboration et al. ... We note that HD 113337 B is found tobe a binary pair (Janson et al.

24 Apr 2007: 2002). M star companions. (B&C). V band surface brightness Deprojected surface density. ... sight. A B. B. A. Face-on view of the disk. 46. Origin of forced eccentricity.

20 Feb 2024: nc( B m ( cfl. s ico ( K hb c th k e spT. ... Q D b 33 J kg 1 Disruption threshold at size D b.

19 Apr 2006: 0]B]B@uxG-N+?3TQGH+?IA-oxGH=?xRU>A]B@M1-N==?G4/2L<@Mr;T2R2]t+;-N=B+?G4x143]B=.-N2_3T"G4/"=?3]B@M/U-0/,y14@ ... t+?36=?@MG4TU-01|-0/2Tx@M>36+.-N=B5;-N=B+?G4x143]T2R23!@)@5S/,?G4/2L0Õ@0z_3=B+?]B@0/i1HG4LMI,KTS=.-0LS9X@M>3a@MrP+?I23]B3!p0-

19 Apr 2006: dashed red line;Model B’ – a flat distribution with r3 as a dashed blue line. ... For the inner part ofthe disk (r 350 AU), Model A/A’ and Model B/B’ givesimilar results, but Model A and A’ give a much betterfit for r >350 AU.

12 Jan 2012: Kennedy1, M. C. Wyatt1, B. Sibthorpe2, G. Ducĥene3,4, P. Kalas4,B. C. ... Photometric measurements are shown as black filled cir-cles, and synthetic photometry of the stellar atmosphere asopen circles(U B, B V , & b y colours, andm1 andc1 Stromgren