jrasc june 1998 final - The Royal Astronomical Society of Canada

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jrasc june 1998 final - The Royal Astronomical Society of Canada

Table I.Line IdentificationsNo. obs Int. lab Atom. Mult. No. obs Int. lab Atom. Mult.1 3720 2 3720 Fe i 5 21 4428 1.7 4427 Fe i 23723 Fe i 5 22 4481 5.2 4481 Mg ii 42 3740 2.5 3737 Fe i 5 23 4520 1.1 4523 Fe ii 383735 Fe i 21 4515 Fe ii 373737 Ca ii 3 4520 Fe ii 373 3750 3 3749 Fe i 21 24 4560 1.1 4549 Fe ii 383758 Fe i 21 4559 Cr ii 443748 Fe i 5 4550 Ti ii 823746 Fe i 5 4556 Fe ii 374 3830 7 3838 Mg i 3 25 4910 1.1 4924 Fe ii 423832 Mg i 3 26 5010 1.6 5018 Fe ii 423820 Fe i 20 27 5050 2.0 5041 Si ii 53826 Fe i 20 ?5 3860 5 3860 Fe i 4 28 5180 9.0 5184 Mg i 23856 Fe i 4 5173 Mg i 23856 Si ii 1 5167 Mg i 23863 Si ii 1 29 5270 2.5 5270 Fe i 156 3934 26 3934 Ca ii 1 30 5330 2.2 5328 Fe i 157 3969 20 3969 Ca ii 1 31 5390 2.0 5406 Fe i 158 4046 2.7 4046 Fe i 43 5397 Fe i 159 4063 2.5 4064 Fe i 43 32 5450 2.7 5430 Fe i 1510 4071 1.9 4072 Fe i 43 5447 Fe i 1511 4079 1.6 4078 Sr ii 1 5456 Fe i 1512 4133 2.5 4131 Si ii 3 33 5530 1.6 5528 Mg i 94128 Si ii 3 34 5600 1.8 5616 Fe i 6864132 Fe i 43 5589 Ca i 2113 4215 1.7 4216 Fe i 3 5587 Fe i 6864216 Sr ii 1 5594 Ca i 2114 4227 3.1 4227 Ca i 2 35 5700–15 4273 1.8 4272 Fe i 42 –5900 N 24275 Cr i 1 36 5890 9.5 5890 Na i 116 4298 1.3 4303 Fe ii 27 5896 Na i 14300 Ti ii 41 37 6170 ~1.5 6158 O i 104297 Fe ii 28 6162 Ca i 317 4310 1.1 4308 Fe i 42 38 6350 ~2 6347 Si ii 218 4325 1.2 4326 Fe i 41 6371 Si ii 219 4383 2.1 4384 Fe i 41 39 6100–4376 Fe i 2 –6400 N 220 4405 1.5 4405 Fe i 41Notes. The columns following the line number refer to the observed wavelength (in Å), the intensity (arbitrary scale), the laboratory wavelength(in Å), the atom/ion name, and the multiplet number. The observed wavelengths are given to 1 Å between 3900–4500 Å, otherwise to 10 Åas a consequence of the larger noise and/or lower dispersion.Å and below 3900 Å the sensitivity is low and the noise is higherthan in other regions. A total of 39 spectral lines were identified inthe tracing, most of them confirmed by their presence in the firstflare as well. The lines are marked by numbers in figure 2 and areidentified in Table I.The spectrum is quite typical of Perseid meteors (e.g. Halliday1961; Cook et al. 1971; Borovicka & Betlem 1997) and is very similarto the Perseid meteor of August 12, 1963, discussed at length byHalliday (1968). Both meteors exhibited a sudden increase inbrightness early in the trail and two major flares near the end. The154JRASC June/juin 1998

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