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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.

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.

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.

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

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: 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%. (&

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