Orbits of Bright Photographic Meteors

P . B . BABADZHANOV X and E . N . K R A M E R 2

During the period 1957 to 1963, systematic photographic observations of meteors were

carried out at the Astrophysical Institute of the Year Academy of Sciences of Tadjikistan (Dushanbe) Month and at the Odessa and the Kiev astronomical

observatories. The photographs were taken Day with cameras NAFA 3C/25 (D=100 mm, F =

250 mm, and field of vision 40°X50°); a pan- Com rad.

chromatic emulsion of 19-cm width with a sensitivity of 1100 to 1300 units of GOST (approx. 350-450 ASA) was used. The base lines between the stations at each observatory

were from 20 to 40 km. The exposures, which Sin Q were carried out automatically, had a duration

of 30 to 60 minutes. Time signals were made

on the star trails by a special transducer. The Cos ZR

limiting magnitude of the system was approxi- mately + 1 mag. The precision of the deter- « mination of the coordinates of any points on the negatives was about 5 sec of arc.

The results are given for about 500 meteors H^b photographed in Dushanbe and Odessa. Some Hmtx

of the results were published by Babadzhanov H^e and Kramer (1963); those that include the V'a

observations of the period from 1960 to 1963 are given in table 1 (Dushanbe) and table 2 VG

(Odessa); these tables consist of the following V*

data: a

No. Meteor number. In table 1 the^e first two digits signify the year 2 of observation minus 1900; the 2 next three digits signify the num- w

ber of exposures in the current year; and the last digit signifies ® the number of the camera. In

1 Astrophysical Institute of the Academy of Sciences of Tadjikistan.

USSR.

1 Odessa State University, USSR.

table 2 the first column denotes the meteor number.

Year of observation minus 1900.

Number of the month of observation.

Day of the month in Universal Time given to 0?001.

Radiant (right ascension a and declination 8) after correction for the earth's attraction and diurnal aberration, in degrees and minutes. Equinox 1950.0.

Q is the angle between the great circles traced by the meteor, as seen from two stations.

Z^R is the zenith distance of the radiant.

Elongation of the corrected radiant from the apex of the earth's motion, in degrees.

Height at beginning, in km.

Height at maximum light, in km.

Height at end, in km.

Velocity outside the earth's at- mosphere, in km/sec.

Geocentric velocity, in km/sec.

Heliocentric velocity, in km/sec.

Semimajor axis, in a.u.

Eccentricity.

Perihelion distance, in a.u.

Aphelion distance, in a.u.

Argument of perihelion, in degrees. Equinox 1950.0.

Longitude of the ascending node, in degrees. Equinox 1950.0.

Inclination of the orbit plane to the ecliptic, in degrees. Equinox 1950.0.

68 SYMPOSIUM ON METEOR ORBITS AND DUST

No.

600051 600153 600165 600185 630215 610502 630621 630674 630684 630054 631512 631712 611902 631811 631006 632141 620384 601242 601443 620611 620631 620644 620681 620606 620662 620672 632341 620762 612376 632395 612451 632421 612474 632432 632441 632494 632521 632652 632665 632632 632725 632762 620886 620962 621025 621105 621134 621204 621234 612992 621354 621402 621694 621892 621973 614003 600361 622063 632943 622123 600522 622215 622372 614654 622512 614715 614713 614764 614794 622563 622571 622713

Year

fiO 60 80 60 63 61 63 63 63 63 63 63 61 63 63 63 62 6 0 60 62 62 6 2 62 62 62 62 6 3 62 61 63 61 63 61 63 63 63 63 63 63 63 63 63 62 62 62 62 62 62 62 61 62 62 62 62 62 61 60 62 63 62 60 62 62 61 62 61 61 61 61 62 62 62

Month

1 1 1 1 1 2 2 2 2 3 6 fi 7 7 7 7 7 7 7 8 8 8 8 8 8

8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 9 9 9 9 9 9 10 10 10 10 10 10 10 10 10 10 11 12 12 12 12 12 12 12 12 12

Day

1.725 4.898 4.924 4.877 22.898 13.885 17.658 18.703 18.783 26.657 16.804 22.890 11.892 15.733 20.846 23.868 25.787 26.903 31.863 2.734 2.829 2.878 3.788 3.874 4.818 4.042 10.681 10.902 11.704 12.773 12.946 13.742 13.750 13.776 13.852 14.849 15.747 15.867 15.879 17.734 18.875 23.795 24.717 28.734 3a 850 31.912 1.774 2.850 3.688 9.002 10.017 23.757 2.851 6.898 9.915 16.878 20.817 21.802 23.940 26.792 28.939 30.728 1.989 3.662 3.826 8.925 8.957 11.749 11.880 17.618 17.714 22.706

TABLE 1.—Orbital elements of Corr. radiant

93°16' 118 34 228 63 220 65 101 16 258 06 07 15 141 42 160 45 175 58 271 33 343 27 304 31 266 25 34 38 21 69 25 51 319 38 31 02 47 34 34 03 32 56 342 34 332 49 36 36 332 30 276 45 38 66 48 31 48 29 68 23 46 56 41 22 47 56 30 48 47 26 66 15 40 35 60 24 314 62 22 13 264 35 36 66 335 43 92 30 68 07 91 36 91 21 276 17 101 13

85 30 366 33 84 40 79 37 110 39 37 46 00 37 04 18 06 20 46 24 52 38 331 58 50 33 99 17 84 23 72 43 151 33 82 03 81 37 83 48 102 57 274 50

1 - 2 8 ° U '

26 34 49 45 49 17 16 U 63 08 8 4 0 12 17

5 02 2 01 - 1 6 15 9 5 3 49 40 25 26 46 32 61 43 51 60 - 9 12

63 62 83 36 54 48 64 40 - 1 5 36 - 1 2 34 56 60 31 15 42 51 56 03 65 39 57 19 65 58 59 27 58 25 58 11 54 02 54 40 56 51 57 18 59 17 4 08 34 46 61 57 69 66 - 5 08 62 40 26 24 56 29 58 35 44 08 40 00 - 1 0 34 - 2 37 50 33 33 17 - 4 49

10 20 14 30 15 27 15 29 11 25 0 3 8 - 1 2 55 13 34 27 34 24 28 - 9 48 21 05 26 45 16 33 24 50 12 37 71 51

Sin Q

0.171 0.026 0.064 0.063 0.196 0.372 0.942 0.328 0.190 0.196 0.424 a 375 0.220 0.669 0. I l l a 181 0.060 0.184 0.366 0.244 a 193

a m

0.660 0.273 a 401 0.268 0.194 0.575 0.104 0.133 0.246 0.146 a 061

<l. 272 0.202 a 075 0.166 0.629 0.143 0.394 0.067 0.306 a 201 0.641 0.130 0.172 0.092 0.040 0.482 0.226 0.168 0.625 0.157 0.704 0.227 0.255 0.037 0.100 0.104 0.365 0.083 a630 0.479 0.208 0.838 0.336 0.405 0.347 0.275 0.206 0.179 0.573

CosZ,

0.394 0.961 0.537 0.635 0.751 0.644 0.909 0.804 0.788

aoos

0.601 0.602 0.004 tt077 a 512 a 7 » a487 0.666

asM

0.683 a 610 a 764 a44O a 040 0.694 0.912 a006 0.810 0.488 0.460 0.800 0.396 0.400 0.474 0.713 0.600 0.356 a 701 0.726 0.807 0.808 0.758 0.558 0.668 0.601 a 801 0.289 0.501 0.965 0.516 0.311 0.761 0.740 0.892 0.403 0.875 0.652 0.460 0.884 0.867 0.684 0.669 0.778 0.996 0.966 0.942 0.909 0.923 0.881 0.575 0.622 0.400

meteors

90:1 77.il

»3. 6 63.7 33.,', 75.5 137.8 98.3 7V. 1 98.0 H3.ll 19.4 73 4 106.7 35.8 40.4 30 7 73 9 30.6 ISN.H 40 0 30 0 63 5 71 0 41 4

a, n

103.0 38.2 88.1 10.6 38. 9 41.0 40.7 40.3 36.7 36.5 38.6 38.8 40.8 95.6 31.6 95.2 51.2 89.9 44.9 9.2 38.8 30.0 109.4 27.0 34.4 95.2 30.2 24.8 27.3 75.2 28.9 25.6 25.5 76.5 77.0 158.1 78.1 63.4 76.6 96.0 22.5 86.8 87.9 90.9 72.8 91.5

(Dushanbe)

88.2 64. fi 84 S 93.9 108.8 88.9 7 4 . 1 81.3 95.7 H 4 4 01.9

ua499.6 91.3 113.0

uas111.6 102.0 100.0

! • • > 7

na4

100.6 99.2 91.4 112.3 88.8 94.4 109.0 103.8 106.2 103.0 111.2 113.4 109.3 111.1 104.5 108.5 108.9 107.7 87.8 106.0 90.9 106.4 95.4 95.4 109.4 107.0 104.8 91.7 100.3 114.7 83.5 112-0 110.8 97.7 104.0 129.3 111.5 100.2 03.2 98.6 77.4 101.1 94.6 96.8 90.9 66.3 92.3 89.9 98.8 102.4 80.8

78.9 83 3 7ft 8 08.6 102.2 70.5 BO, B 74 4 010

— 79.8 100.0 96.0 80.0

uasi'»i.'.

84.3 Wfl 0 H4 'i BIO NO 4 w 6 88.1 S3.9 101.3 88.0 88.5 98.4 101.5

— 92.0 108.5 96.0 92.0 93.0 87.5 104.0 99.0 102.2 79.3 92.0 7& 0 98.11 84.8 91.0 96.6 98.5 95.8 72.9 98.2

— 61.0 94.5 94.3 94.5 74.2 _ 99.6 98.5 78.8 85.0 _ 76.2 75.6 83.0 81.9 60.3 81.0 76.9 89.fi 90.7 85.3

11.

77.5 SO. 1 7.1. 7 67.8 97.0 88 1 41. s 71.8 7ft fi 40 2 77.4 101.9 90.4 81.7 108.6 97.0 83. 5 M •-•

7H 7

n .->

87.3 80.8 H « 3 78.4 K 3 7M B 74 fi Od H 03.7 90. U H9.0 8 7 . 9 03. 8 8 0 . 2 9 0 . 9 82.9 05.8 04.4 9 7 . 6 74.9 90.2 72.6 95.7 82.1 88.7 95.9 90.2 92.7 72.2 92.4 84.2 58.2 87.6 94.1 90.4 68.7 89.9 93.8 91.8 75.9 80.9 36.2 69.7 69.9 72.0 73.3 58.6 53.5 72.8 77.9 86.8 82.9

36.2 23 4 37 •:

37 4 68.1 3 3 7 14 3 . ' 1 4 3 2 5 .'1 3 2 * 1 .',0 1 41 'I 31. fl 82 .'.

60.0

«) 1 17.6 10 7 42.5 6a 7

eaoa t

3 4 . 2 59. M 45 ii 21.0 61.8 00 0 61.9 57.3 60.0 63.9 60.8

« l . n 5 9 . 0 5 8 . 6

«O.H 59.2

•IT. 2 64.5 23.5 50.1 27.9 58.2 72.7 60.9 56.4 19.3 67.0 64.0 23.5 66.6 68.9 67.1 32 3 74.9 67.5 67.9 30.3 34.4 13.5 29.9 41.0 31.9 24.2 28.6 26.4 24.6 25.9 40.4 26.1

28.0

sa7

18.1 IS, S 61 y 11.0 8 0 IS 1 30 4 17.0 :n a 87 I 30 8 11 4 61 3 68 1 Bfl, 8 M.0 M S 41 n SB 5 M H 4-) fi

n 4

IN fi 43 H 18 0

saa59 6 80.7 5 & 1 58.6 02.7 59.fi 59.7 57.8 57.4 59.6 58.0 24.8 63.4 20.9 48.7 25.4 56.9 71.6 59.7 55.0 15.8 65.8 62.7 20.6 65.4 67.9 65.9 30.4 73.8 66.3 6fi.9 38.1 32.8 8 . 0 27.7 39.2 29.9 21.8 26.3 23.8 22.1 23.1 38.5 23.6

1 , ,

M.4 13 8 34 s 18.0 4.' 1 37 8 37 3 37 3 as a 87.0 37 1 31 7 41 U 3 1 1 41 3 41 1 4 0 N 80.6 40 J 40 0 41 B 40.0 3* (I M l ) 41 4 40 1 31 6 41.0 40 8 42.5 88.0 41 4 44 1 41.7 40 2 38.4 39.0 41.0 40.6 40.3 41.3 37.6 38.0 38 9 41.6 42.8 41.1 37 6 37.9 41.7 41.8 37.6 42.4 42.7 41.7 36. H 49.7 41.4 41.9 36.0 39.1 37.6 36.4 37.3 37 3 39 1 11.7 37.4 36.8 38.4 41.4 38 9

2.70 1 20 1 40 LSI 27.0

2.42 118 X30 2 Hi 3 1H 3 3 1 1.20 -78.2

3.73 1.08 10.2 10.5 8.09 8.07 11 fi 3 3 H 11.4 3.90 1.08 23.2

0.38 3 31

• v.ao -17.1

ISA 25.7 -3.52

83.2 0.30 3.16 3 77 13.0

8.45 0.08 18.8

2.62 2.84 3.03 3 1 . 8 -13.0 1X8 2.53 2.71 81.8 88.0 2 . 5 1 - 3 4 . 0 - 1 0 . 5 23.1 2.07 - 1 . 2 9 12.2 28.0 1.81 3.47 2.36 1.92 118 2.15 3.22 0.633 2.20 1.98 2.68 9.58 3.04

ORBITS OF BRIGHT PHOTOGRAPHIC METEORS—BABADZHANOV AKD KRAMER 69

No.

600051 600163 600166 600186 630215 61OS02 630621 630674 630684 630064 631612 631712 611002 631811 631006 632141 620384 601242 601443 6206U 620631 620644 620681 620605 620662 620672 632341 620762 612376 632305 612451 632421 612474 632432 632441 632494 632521 632552 632555 632632 632725 632762 620886 620962 621025 621105 621134 621204 621234 612992 621364 621402 621694 621892 621973 614003 600361 622063 632943 622123 600522 622215 622372 614564 622612 614715 614713 614764 614794 622663 622571 622713

Year

GO 6 0 60 60 63 61 63 63 63 63 63 63 61 63 63 63 62 6 0 6 0 6 2 62 6'.' 62 6 2 6 2 6 2 63 6 2 61 63 61 63 61 63 63 63 63 63 63 63 63 63 62 62 62 62 6 2 62 6 2 61 62 62 62 62 62 61 60 62 63 62 60 62 6 2 61 6 2 61 61 61 61 62 62 62

Month

1 1 1 1 1 2 2 2 2 3 6 6 7 7 7 7 7 7 7 H

8 8

8 K 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 9 9 9 9 9 9 10 10 10 10 10 10 10 10 10 10 11 12 12 12 12 12 12 12 12 12

TABLE

Day

1.726 4.898 4.924 4.877 22.898 13.885 17.658 18.703 18.783 26.667 16.804 22.890 11.892 16.733 20.846 23.868 26.787 25.903 31.853 2.734 2.829 2.878 3.788 3.874 4.818 4.942 10.681 10.902 11.794 12.773 12.946 13.742 13.750 13.776 13.852 14.849 15.747 15.867 15.879 17.734 IS.875 23.795 24.717 28.734 30.850 31.012 1.774 2.860 3.688 9.902 10.917 23.767 2.851 6.898 9.915 16.878 20.817 21.802 23.940 26.792 28.939 30.728 1.989 3.662 3.826 8.925 8.967 11.749 11.880 17.618 17.714 22.796

0.728 0.630 0.343 0.361 0.980 0.693 0.658 0.675 0.874 0.668 0.812 0.386 1.01 0.763 0.960 0.941 0.910 0.954 0.881 0.921 0.972 0.916 0.970 0.801 0.067 0.018 0.704 1.000 0.904 1.054 0.712 0.963 1.28 0.988 0.843 0.697 0.760 0.926 0.888 0.903 0.961 0.614 0.645 0.865 0.974 1.08 0.938 0.690 0.633 0.978 0.983 0.748 1.03 1.03 0.958 0.862 1.48 0.953 0.979 0.818 0.894 0.583 0.816 0.958 0.854 0.774 0.946 0.768 0.723 0.788 0.977 0.678

1.—Orbital elements of meteors

0.736 0.442 0.979 0.976 0.533 0.986 0.962 0.714 0.362 0.725 0.448 0.738 0.938 0.921 0.796 0.958 0.948 0.229 0.962 0.914 0.957 0.062 0.067 0.100 0.051 0.515 0.978 0.970 0.935 0.943 0.824 0.956 0.992 0.959 0.999 0.969 0.902 0.958 0.949 0.650 0.739 1.011 1.009 0.528 0.818 0.973 0.784 0.786 0.997 0.688 0.985 0.632 0.902 0.656 0.970 0.286 0.617 0.571 0.683 0.328 0.354 0.984 0.352 0.091 0.314 0.728 0.029 0.513 0548 0.669 0.219 0.979

4.66 1.96 2.00 2.08 53.5

3.86 3.40 3.68 5.40 3.64 4.32 1.66 - 1 5 7 . 2

6.54 3.88 31.4 20.0 9.81 15.2 22.4 66.6 21.8 5.71 3.68 43.4 12.0 5.64

18.4 - 3 5 . 5 4.89 50.4 - 8 . 0 4 165.4

11.7 5.36 6.63 25.1 16.0 12.7 36.8 4.23 4.67 6.73 62.8 - 2 6 . 9 24,8 4.28 4.44 62.9 115.0 4.38 - 6 9 . 0 - 3 9 . 6 45.3 3.85 - 3 . 2 0 23.8 55.4 3.29 6.57 3.74 3.48 4.21 3.99 5.72 1.04 3.90 3.41 4.79 18.9

5.10 w

66?2 295.0 169.0 166.2 265.8 175.3 22.2 70.1 111.0 251.3 284.3 269.2 212.3 218.6 123.5 162.1 149.2 305.0 152.8 142.4 151.9 153.0 148.7 132.8 150.6 271.6 203.9 161.8 146.8 149.9 123.5 152.1 164.4 151.4 165.9 150.4 138.4 152.8 160.2 255.8 243.2 181.3 175.0 87.9 128.0 201.2 124.1 117.4 194.0 111.0 343.3 82.2 216.3 251.2 340.5 122.7 68.7 82.8 80.7 119.3 111.1 14.5 115.8 31.2 298.7 66.3 355.5 276.0 93.2 267.6 235.1 188.4

10«2 282.4 282.4 282.4 302.0 324.8 148.1 149.1 149.2 6.2 84.7 90.5 109.2 112.3 117.2 120.1 122,2 122.8 128.4 129.8 129.8 129.9 310.8 310.8 131.8 131.9 137.1 137.6 138.7 139.1 139.8 140.1 140.6 140.1 140.2 141.1 142.0 142.1 142.1 143.9 145.0 149.8 150.9 154.8 156.8 157.8 158.7 159.9 160.5 166.8 347.5 0.1 189.0 193.0 15.9 23.1 27.3 28.1 29.6 32.7 35.4 36.9 38.9 251.1 251.0 76.4 256.5 259.3 79.4 264.9 85.1 269.6

(Dushanbe)—Continued

147?2 1 5 65.2 65.4 137.3 54.0 3.5 1.4 1 0 0.1 7.2 148.3 63.4 21.8 123.7 112.6 113.8 11.4 113.3 67.9 113.6 113.1 25.9 2.2 111.2 71.6 27.1 116.4 116.4 114.9 113.7 110.8 114.1 113.2 117.5 116.9 114.3 115.0 111.4 15.2 134.4 33.6 91.5 41.0 106.3 169.6 117.2 111.4 22.8 146.3 122.2 0.7 132.1 159.6 134.0 6.0 162.0 163.2 163.6 7.0 25.8 0.3 5.5 13.6 1.5 19.7 3 1 2 2.9 5.0 1.1 20.1 37.3

•w

166?4 217.4 91.4 88.6 207.8 140.1 170.3 219.2 260.2 256.5 9.0 359.7 321.5 330.9 240.7 272.2 271.4 68.7 281.3 272.2 281.8 282.9 119.5 83.6 262.4 43.5 341.0 299.4 285.5 289.0 263.3 292.2 305.0 291.5 306.1 291.5 280.4 2919 292.3 39.7 28.2 331.1 325.9 242.7 284.8 359.0 282.8

•277.3 354.5 277.8 330.8 82.3 45.3 84.2 356.4 145.8 96.0 110.9 110.3 152.0 146.5 51.4 154.7 282.3 189.7 142.7 252.0 175.3 172.6 172.6 320.2 98.0

- 2 . 0 - 1 2 - 1 1 - 5 . 7 - 1 . 9 - 0 . 9 - 2 . 2 - 0 . 2 -

— - 2 . 0 - 2 . 3 - 2 . 1 0.1 - 1 . 6 - 2 . 0 - 6 . 8 - 1 . 6 - 1 0 - 1 . 0 - 2 . 8 - 2 . 4

^3.2 - 2 . 7 - 1 0 - 1 . 0 - 1 . 0 - 0 . 8 - 2 . 7

— - 2 . 8 - 3 . 0 - 3 . 0 - 2 . 4 - 2 . 4 - 2 . 8 - 2 . 5 - 1 . 9 - 1 . 4 - 1 . 7 -6.5 -0.7 -0.2 0.4 - 1 . 4 - 2 . 9 - 2 . 8 - 2 . 4 - 3 . 1 - 1 . 6

— - 3 . 0 - 1 0 - 2 . 2 - 1 . 9 - 1 . 5 bolide - 1 2 - 2 . 8 - 0 . 6 - 1 . 4 bolide - 3 . 9

1.0 - 1 . 7 - 1 . 4 - 2 . 8 - 1 . 9 - 0 . 8 - 2 . 2 - 0 . 8

1.02 0.30 0.44 1.02 0.24 1.36 1.03 0.55 0.76 2.92 0.88 0.22 0.23 0.66 0.21 0.30 0.49 0.89 0.66 0.43 0.64 0.37 0.70 0.66 0.45 0.26 0.99 0.26 0.30 0.33 0.30 0.96 0.63 0.71 0.46 0.55 0.59 0.34 0.23 0.55 0.31 1.12 0.33 0.74 0.23 0.24 0.46 0.43 1.06 0.22 0.76 1.61 0.50 0.28 0.27 0.90 0.55 0.24 0.65 0.77 5.17 1.42 1.40 0.75 1.65 0.29 1.66 0.77 1.97 0.62 0.42

771 oo

1 9 2 2.65 1 4 0 38.6

0.071 1.49 2 1 8

0.955 _ _ 2.76 0.069 0.347 0.577 0.036 0.109 3.06 0.898 1.14 0.095 0.382 0.210 0.943 1.40 0.461 0.088 1 7 0 0.031 0.330

— 0.366 1.15 0.48 0.379 0.266 0.461 0.526 0.121 0.056 1.28 2.09 2.15 0.061 0.341 0.059 0.089 0.604 0.216 3.46 0.029

— 25.3 1.08 0.637 0.069 0.616 1.05 0.121 0.423 0.636

— 7.34 0.168 5.57 0.668 11.7

1.68 1.94 0.413 0.480

Shower or parent comet

Quadr Quadr

1766 II 67

72(73) 1764 Per Per Per V Per Per VII Aqu Per 73(72) Per Per Per Per Per Per Per Per Per Per Per Per

« C y g

I X 1864II I X I X 17901

1723 S. Ari Ori Ori Ori 8. Ari

S. Taur XV?

X V X V X V 19171

70 SYMPOSIUM ON METEOR ORBITS AND DUST TABLE 2.—Orbital elements of meteors (Odessa)

No.

197 198 200 201 202 203 205 206 207 162 208 209 164 209a 210 212 215 214 213 219 221 222 220 224 226 223 227b 227 227a 225 229 188 232 233 228 230 231 236 168 235 166 165 169 190 238 173 170 234 167 239 172 241 240 243 249 237 252 251 177 178 176 253 179 244 248 250 245 244a 246b 255 256 257 259

Year

61 61 61 61 61 61 61 61 61 60 61 61 60 61 61 61 61 61 61 61 61 61 61 61 61 61 61 61 61 61 61 60 61 61 61 61 61 61 60 61 60 60 60 60 61 60 60 61 60 61 60 61 61 61 61 61 61 61 60 60 60 61 60 61 61 61 61 61 61 61 61 61 61

M o n t h

3 4 4 4 5 5 6 6 6 t>

7 7 7 8 8 8 8 8 8 8 8 8 H 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8

Day

20.087 8.830 15.801 10.802 9.024 9.058 15.883 21.070 22.074 20.004 11.008 2a ooo 23.847 1.840 3.080 0.882 7.002 7.035 7.053 7.871 0.032 0.030 0.037 0.820 0.800 0.072 0.080 0.000 10.015 10.023 10.024 10.901 10.055 10.077 10.081 11.000 11.051 11.704 11.827 11.834 11.804 11.881 11.881 11.881 11.882 11.922 11.926 11.035 11.035 11.065 11.983 12.000 12.010 12.014 12.044 12.054 12.841 12.846 12.852 12.874 12.895 12.919 12.981 13.007 13.007 13.018 13.010 13.037 13.045 13.957 11017 14.021 14.037

Corr a

237°51' 195 07 207 07 156 44 202 11 280 10 222 10 200 43 205 12 272 33 204 11 14 31 370 10 300 02 343 11 30 44 47 20 30 34 40 27 311 35 42 10 43 32 12 43 41 35 44 58 328 01 44 80 44 40 42 82 48 27 48 12 47 20 45 44 382 36 343 34 343 35 80 54 47 13 44 19 46 00 80 48 48 22 45 54 47 15 50 34 44 47 41 04 342 06 48 10 46 20 49 04 46 00 47 17 328 15 48 03 347 33 50 40 37 38 47 12 46 46 45 42 47 40 50 03 45 40 40 31 43 08 40 18 51 38 48 27 83 00 56 17 51 11 61 61

radiant

a i'ir

- 0 45 10 40 - 0 03 - 0 27 42 28 05 30 - 4 38 10 00 - 1 37 02 11 53 40 44 04 1 67 - 1 4 15 67 23 68 28 60 40 66 22 6 4 2 67 32 47 12 02 88 88 32 67 86 - 7 00 50 30 50 20 57 27 00 40 80 63 87 18 88 30 - 1 2 00 - 0 36 - 1 1 16 58 10 50 17 50 05 57 40 57 04 57 52 57 40 50 58 50 17 01 30 50 26 - 1 3 10 58 41 88 08 55 10 57 10 50 00 53 39 60 31 48 10 57 37 59 24 58 47 58 08 50 45 58 23 58 14 57 66 56 60 56 37 88 00 57 38 67 14 50 47 61 41 50 16 58 57

S i n Q

a 881 0.444 0.090 0.670 0.182 0.110 0.278 0.802 0.180 0.461 0.008 0.229 0.328 0.066 0.006 0.288 0.016 0.208 0.200 0.147 0.237 0.128 0.132 0.201 0.126 0.914 0.194 0.284 0.123 a 041 0.309 0.078 0.147 0.570 0.413 0.701 0,125 0.370 0.021 0.270 0.220 0.122 0.210 0.060 0.201 0.098 0.240 0.502 0.837 0.217 0.009 0.224 0.310 0.810 0.200 0.177 0.180 0.180 0.110 0.400 0.091 0.157 0.372 0.268 0.100 0.180 0.038 0.174 0.470 0.202 0.221 0.061 0.995

CosZ,

0.700 a 628 0.722 a 713 a 578 0.841 0.037 0.574 0.807 0.000 0.842 0.805 0.907 0.077 0.606 0.603 0.788 0.884 0.012 0.772 0.880 0.830 0.062 0.424 0.424 0.006 0.790 0.864 0.888 0.884 0.848 0.002 0.727 0.626 0.088 0.850 0.880 0.308 0.472 0.401 0.402 0.601 0.864 0.552 0.523 0.081 0.705 0.800 0.696 a 750 0.705 0.810 0.833 -0.050 0.017 0.908 0.481 0.556 0.608 0.554 0.598 0.049 0.764 0.840 0.819 0.872 0.841 0.800 0.801 0.699 0.813 0.844 0.870

3»'3 91.9 90.3 168.5 118.0 04.7 108.2 00.2 00.1 M.9 W. 0 43.0 111.3 70.3 fil.U 41 •-' M.1 41 4 30.0

MO. 7 4 0 . H

30.4 51.0

no4O.fi H2.fi 42.«

SO. 4 IB. 4 43.x 39.9 39.9 41. 2 59.3 64.0 6O.fi 41.1 41.7 41.5 40.2 39.5 40.2 40. 0 39.3 38. S 43.9 42.0 69.9 41.0 40.6 35.5 39.7 40.4 69.3 42.6 56.8 39.5 42.2 40.9 40.2 38.9 40.6 40.3 40.1 39.0 39.8 40.2 39.8 39.4 39.0 43.8 41.3 40.9

v^m ^Va

101.5 07.0 101.0 87.8 06.2 108.0 83.3 01.4 79.8 90. 0 88.6 107.3 04.0

8 4 . 7

08.8 1U.6 107.0 100.0 100.2 8&8 106.7 104.0 07.0 111. 2 107.7 00.6 100.1 116.0 100.0 108.4 108.1 104.8 103.3 95.0 98.0 99.6 102.2 107.3 100.0 108.0 HZ 6 110.7 113.0 104.0 102.5 100.5 98.6 107.6 113.0 1010 110.0 1011 106.2 108.0 103.9 100.6 105.5 106.0 110.8 107.9 111.3 110.0 110.0 1015 107.5 112.0 100.2 108.0 100.5 106.3 111.8 100.5

08.8 93.0

70. 8

•8.2 BA..'- 70. s 7M.3 87.8

78.2 M»3 HX 0

1*7 0 Hl.fl 7H. 4

•K. 3

08.8 97. 2 M. 3 89.0 M.6 90.4 W.5 89.9 89.0 91.9

99.6 93.0 102.0

8 1 0 101.1 81.6 83.1 101.0 00.4 96.0 95.0 88.5 98.0 99.7 98.5 101.6 80.7 92.5 87.0 98.0 81.4 90.9 91.2 100.0 95.0 100.3

O i l 77.5 K3 11 8 1 0 70.2 50.1 78.2 IV9.0 75 5 H5.0 H . 3

7fl V Sfl.O TV 0

St. 9

U3 2 77 0 75 6 U3.0 W.O H3.4 W O

uo.u

*e.«

07.8 NO. 4 87.5 94.7 9 Z 5 87.9 95.7 H9.0 86.1 80.4 90.7 90.0 97.5 93.9 92.0 80.0 96.4 98.0 83.0 97.0 7 1 5 9 Z 0 79.3 84.3 95.4 88.6 85. H 92.0 86.4 99.3 95.5 93.0 92.5 94.9 05.6 79.1 8 1 0 86.3 93.5 80.0 99.0 90.8 89.0 05.0 8 1 5 96.7

80.1 28. 1 28.4 16.3 18.0

47.7 14 4 2ZS 3 5 . 5 23 7

n i

62.5 BLl 40 7 41 V 80.3 m 3 ami

M B 24 1 fll.5 fJ i ,'J «

fiO «

aao11.8 M) * 60.8 60. 6 M.O 61.1 59.9 59.6 40.6 41.5 40.2 59.6 61.1 60.8 00.5 58.1 60.4 60.4 59.9 62.5 62.6 61.5 38.7 62.2 61.0 60.1 60.3 60.6 43.1 60.0 46.6 60.9 60.2 60.2 61.4 60.9 60.1 60.8 60.2 60.3 63.4 61.1 58.4 60.1 60.8 57.8 50.9 50.6

54. a 214 28.0 12.3 15 4 40.1

0.5 10.8

33. H 21 1 27.1 01 3 19.4 3H.0 40 4 a§ H 50.0 W 0 at 7 21.1 M 3 02.0 53 4 50.1 50.0

so. a

59. 5 80. S 50.3 57.3 50.8 68.8 58.3 39.0 39.9 38.7 58.3 59.8 50.5 59.2 56.7 59.0 59.0 58.5 61.2 61.3 60.2 37.0 60.9 59.6 58.8 59.0 59.3 41.8 57.8 45.4 59.6 58.8 68.0 60.0 59.6 58.8 59.4 58.9 59.0 6Z1 59.8 57.1 58.9 59.5 56.4 58.6 58.4

36.3 38. 5 41 5 41.3 38.7 42.8 33.5 37 9 4U.M

37. e 41 4 45.0 38. 2 44.0 17.1 41 5 40 7 41. N 41 2 30.2 42.6 30.5 40 V 40.7 41.8 39 0 4ZH 41.3 41.1 41.4 41.8 40.6 41.4 34.8 37.8 35.3 41.0 42.6 4Z2 41.4 38.8 41.2 41.1 40.3 4 Z 5 45.0 43.0 38.5 43.2 41.9 39.7 40.9 41.5 41.8 41.3 38.2 41.4 4 Z 0 41.4 42.1 41.1 41.1 41.6 41.1 40.6 43.0 41.9 39.3 40.7 41.0 40.7 41.3 40.9

ORBITS OF BRIGHT PHOTOGRAPHIC METEORS—BABADZHANOV AND KRAMER

TABLE 2.—Orbital elements of meteors (Odessa)—Continued

No.

197 198 200 201 2ff2 203 205 206 207 162 20M 209 164 209a 210 212 215 214 213 210 221 222 220 224 226 223 227b 227 227a 225 220 188 232 233 228 230 231 236 168 235 166 165 169 190 238 173 170 234 167 239 172 241 240 243 249 237 252 251 177 178 176 253 179 244 248 250 245 244a 246b 255 256 257 259

Year

61 61 61 61 61 61 61 61 61 60 61 (H GO (11 fil 61 61 til 01 61 61 61 61 61 61 fil 61 61 61 61 61 60 61 61 61 61 61 61 60 61 60 60 60 60 61 60 60 61 60 61 60 61 61 61 61 61 61 61 60 60 60 61 60 61 61 61 61 61 61 61 61 61 61

Month

3 4 4 4 S S 6 6 6 t»

7 7 7 8 8 8 8 g 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8

Day

20.057 8.836 15.801 16.862 9.024 0.058 15.883 21.979 22.974 29.094 11.998 20.996 23.847 1.849 3.986 6.852 7.002 7.035 7.053 7.871 9.032 9.036 9.037 9.826 9.890 9.972 9.989 9.990 10.015 10.023 10.024 10.901 10.055 10.077 10.081 11.000 11.051 11.794 11.827 11.834 11.864 11.881 11.881 11.881 11.882 11.922 11.926 11.935 11.935 11.965 11.083 12.000 12.010 12.014 12.044 12.054 12.841 12.846 12.852 12.874 12.895 12.919 12.981 13.007 13.007 13.018 13.019 13.037 13.045 13.057 11017 11021 11037

1.90 3.03 19.85 13.67 3.40 -11.70 1.42 2.86 -2.01 2.64 27.32 3.18 3.09 - 4 . 8 2 2.38 32.87 9.14 147.30 18.13 2.02 - 1 1 8 3 1 7 2 11.49 9.04 23.1

3.77 -11.15 18.35 13.86 22.4 105.72

8.84 21.27 1.65 1 7 5 1.74 12.06 -13.6 -27.59

21.20 3.62 16.99 1115 6.99 -16.74 -3.31 - 8 . 5 6 3.30 - 7 . 5 8 -227.32 5.09 11.40 29.04 107.2

18.68 3.06 25.138 -73.85

22.44 -42.65 13.83 1145 45.80 13.30 8.45 - 9 . 4 6 1862.20 1 2 5 0.16 12.38 0.18 17.56 11.27

0.828 0.813 0.064 0.927 0.751 1.085 0.287 0.743 1.371 0.739 0.963 1.310 0.684 1.077 0.967 0.971 0.901 0.993 0.947 0.690 1.064 0.797 0.912 0.893 1.000 0.894 1.090 0.948 0.931 0.958 0.991 0.804 0.956 0.054 0.968 0.922 0.025 1.070 1.035 0.055 0.750 0.044 0.933 0.865 1.055 1.202 1.115 0.946 1.127 1.004 0.818 0.017 0.968 0.992 0.949 0.752 0.963 1.014 0.958 1.022 0.930 0.034 0.080 0.028 0.880 1.104 0.000 0.786 0.807 0.926 0.903 0.047 0.018

0.328 0.566 0.716 1.004 0.848 0.996 1.014 0.733 0.746 0.690 1.015 0.985 0.979 0.372 0.079 0.950 0.901 1.003 0.960 0.627 0.956 0.958 1.014 0.964 0.943 0.398 0.944 0.945 0.957 0.935 0.921 0.933 0.944 0.076 0.088 0.137 0.905 0.046 0.064 0.951 0.905 0.951 0.954 0.943 0.926 0.965 0.981 0.179 0.563 0.952 0.929 0.051 0.045 0.878 0.946 0.761 0.929 0.996 0.954 0.959 0.965 0.949 0.938 0.062 0.936 0.984 0.942 0.911 0.944 0.915 0.894 0.035 0.929

3.47 5.50 39.03 26.34 5.95 1.83 4.98 1 6 0 53.56 5.20 1 6 6 6177 17.38 203.00 35.26 3.41 8.48 21.97 17.11 4618.02 7.14 35.76 26.76 43.9 210.52

16.74 41.60 3.22 5.42 3.35 23.22

41.45 6.34 33.02 27.36 13.04

6.42

9.26 21.85 57.14 213.5

36.41 5.36 49.35 43.93 26.69 27.95 90.53 25.82 15.96 3723.

7.50 17.38 23.84 17.46 3120 21.61

296?8 271.8 245.5 177.8 308.7 193.2 172.9 249.4 237.4 255.0 1814 161.1 2014 77.2 151.1 150.6 220.1 192.2 207.1 265.7 152.8 151.0 182.9 153.7 149.4 73.4 150.3 140.3 152.2 147.3 1416 146.4 149.3 206.6 328.9 323.5 140.9 150.6 1519 151.0 138.6 156.9 151.5 148.2 146.2 156.2 160.1 226.0 155.1 151.5 1416 isa 7 149.6 223.0 149.6 245.2 146.2 165.1 151.6 153.5 1514 150.2 157.8 153.6 147.0 161.0 149.2 140.5 148.9 143.0 138.9 147.3 145.7

359? 1 198.6

25.4 206.5 228.8 48.9 84.4 90.2 91.1 08.1 109.2 117.8 120.8 129.2 311.2 1310 1311 1311 1312 1319 136.0 136.0 136.0 136.8 136.9 137.0 137.0 137.0 137.0 137.0 137.0 138.1 137.9 317.9 137.9 137.9 138.0 138.7 130.0 138.7 139.0 135.0 139.0 139.0 138.8 139.0 139.1 318.8 139.1 138.9 139.1 138.9 138.9 138.9 139.9 138.9 139.7 139.7 140.0 140.0 140.0 139.8 140.1 139.0 130.9 139.9 139.9 130.9 130.9 140.3 140.8 140.8 140.8

122?8 2.4 20.7 6.2 0.0 76.6 15.6 10.9 33.4 14.2 41.1 110.5 28.5 31.9 23.4 111.6 115.4 111.1 115.3 15.8 113.3 126.4 95.0 115.1 113.0 7.5 110.3 1115 1111 107.4 114.3 113.2 111.6 29.6 19.6 48.0 111.8 111.6 111.5 119.1 112.6 112.9 113.1 113.8 116.6 109.6 111.0 11.3 112.9 112.9 116.6 113.6 113.0 68.1 109.0 82.6 1112 109.8 111.9 113.4 1110 112.4 113.2 112.9 1117 117.5 113.6 1114 1110 115.3 106.9 111.5 111.8

297?9 110.4 270.9 2 1 3 177.5 242.1 257.3 339.5 328.5 3510 293.6 279.0 325.2 206.3 102.3 2815 3512 326.3 341.3 40.6 288.8 287.1 318.9 290.5 286.3 210.3 287.3 286.3 329.2 2813 281.6 2814 287.2 1614 106.8 101.6 278.9 289.3 293.9 289.8 277.6 280.9 290.6 287.2 285.0 295.2 200.1 1710 2012 290.4 283.7 289.6 288.5 1.0 280.5 2 1 1 285.8 3018 291.6 205.5 2914 290.0 297.9 293.5 286.9 300.8 280.1 280.5 288.8 283.3 279.7 281.1 286.6

- 5 . 1 - 2 . 2 - 1 . 1 - 3 . 6 - 6 . 7 - 1 6 - 2 . 5 - 2 . 5 - 3 . 1 - 2 . 6

- 6 . 7 - 1 6

- 1 8 - 3 . 7 - 1 4 - 2 . 0 - 1 6 - 3 . 3 - 5 . 2 - 3 . 5

- 1 1 - 1 3 - 5 . 9 - 5 . 9 - 3 . 9 - 1 6 - 8 - 3 . 5

- 3 . 7 - 3 . 3 - 3 . 5 - 6 . 4 - 1 6 - 1 5 - 1 8 - 3 . 3

- 3 . 3 - 1 1 - 3 . 4 - 3 . 7 - 1 8 - 7 . 4 - 1 0 - 5 . 2 - 1 9

771 oo

2.57 5.67 50.8 1124

6.62 0.85 6.89 2.00 6.97

20.45 0.97

0.094 1.05 1.32 1.31 1.42 0.24 1.04 0.47

2.83 0.90 3.18 7.24 0.91 1.86 25.05 0.52

0.26 6.95 0.45 19.24 1.56 1.25 0.28 0.24

0.36 1.20 0.66 0.54 1.46 11.75 1.12 3.88 0.14

Shower or parent

comet

1834

f Dra III

Per Per Per Per 1457 II Per

Per Per Per Per Per Per Per Per Per Aqu VII VII Per Per Per Per Per Per Per Per Per Per Per a Aqu Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per Per

72 SYMPOSIUM ON METEOR ORBITS AND DUST TABLE 2.—Orbital elements of meteors (Odessa)—Continued

No.

258 261 263 264 265 181 185 184 267 268 269 271 270 187 273 272 274 194 196

Year

61 61 61 61 61 60 60 60 61 61 61 61 61 60 61 61 61 60 60

Month

8 8 8 8 8 8 8 8 8 8 8 8 8 8 9 9 9 9 10

Day

11040 11026 11078 16.037 16.071 17.787 10.700 19.882 10.807 21.061 21.068 22.041 22.063 26.071 1.812 1.824 1036 10.818 20.871

Corr.

22 56 S3 50 53 24 356 02 56 00 52 40 57 20 22 32 10 21 210 33 288 45 65 11 4 10 261 10 206 31 208 60 340 28 335 38 36 30

radiant I

- 1 1 00 60 14 57 53 - 1 3 47

50 01 57 23 58 17 24 41 21 45 63 30 61 31 58 28 - 1 3 17

64 63 61 04 12 17 3 41 - 0 40 :t 4 H

SlnQ

0.433 0.665 0.488 0.438 0.173 0.387 0.207 0.081 0.380 0.201 0.375 0.660 a 447 0.626 0.188 0.838 0.660 0.842 0.765

CoaZ,

0.520 0.646 0.748 0.466 0.743 0.363 0.386 0.668 0.600 0.625 0.808 0.848 0.407 0.682 0.994 0.833 a 616 0.708 0.782

•

38.9 42.0 39.6 6 1 0 40.3 38.3 38. H 30.5 41.6 95 4 H». 4 38. 9 6 1 . 8 H7. 1 06.6 110.6 80.3 no : 78.0

106.6 100.1 107.5 08.6 111.8 103.0 113 4 117.4 06.3 Hi 4 02.1 106.2 08.0 H9 1

HO. 5 Hi. 7 89.9 93 4

OH. 1 95.3 94.0 92 9 97. 2 90.6 M.I H6.4 9Z5 H3.5 H7. 1 90.5 H9.3 Hfl.2

7« 3 Hi 7 HI.9

11.

96.9 90.1 91 4 Hfc 4 9 4 . 8 H9.6 8 1 7 H3.4 90.0 77 0 81 3 96.0 85.0 H2 6 70.7 73.2 70.3 79 4

60.7 60.4 60.1 38. 9 60. 2 65.0 6 1 . 0 6 1 9 6 1 . 0 M. 2 29 9 61.0 46.0 25.0 2 1 9 31.5 27.7 2 . 0

» 9 59.6 59 1 811 36 H 58.9 63. H 59. H 63 fi 59.7 21. 7 28 0 59.8 4 1 5 22.H 22. 3 29 5 23 2 IH 9 Jfl 5

41.1 42.1 40.7 35.5 41 1 4 1 6 41.2 41.0 42.4 38. 2 40.5 41.2 40 2 M.2 38 7 51 0 35 4 40 3 36 0

Longitude of perihelion («+Q), in

Shower or parent comet

Maximum photographic absolute magnitude of the meteor's trail.

Duration of photographed trails, in seconds of time.

Initial mass of meteor body, in grams.

Meteor shower, association, or parent comet.

The meteors that belong to the associations discovered from observations in the USSR are designated by Roman numerals and those discovered by Jacchia and Whipple (1961) by Arabic numerals.

Determination of the instant of the meteor was made either by reduction of meteor photographs obtained at one of the stations by both driven and undriven cameras or by using a moving-blade shutter (Kramer, 1953).

The velocity of the meteor outside the atmos- phere was computed on the basis of the inter- polation formula V=Va-\-kce*t. Reduction methods for meteor photographs have been described in detail by Babadzhanov and Kramer (1963).

From the distribution of maximum luminosity of all meteors (fig. 1) it follows that on the whole they refer to the class of bright meteors (M<1 mag), the maximum being —3 mag. For comparison, figure 1 also shows the distribution of

BRIGHT METEORS FAINT METEORS

•

r

I ' ^r--- 1

- 9 - 8 - 7 - 6 - 5 - 4 - 3 - 2 - 1 0 I 2 3 Mmox FIGURE 1.—Distribution of maximum magnitudes of meteors.

maximum luminosity of faint meteors photographed by Baker Super^Schmidt cameras (McCrosky and Posen, 1961). The distributions partly overlap; hence the results given

ORBITS OF BRIGHT PHOTOGRAPHIC METEORS BABADZHANOV AND KRAMER

TABLE 2.—Orbital elements of meteors (Odessa)—Continued

No.

258 261 263 264 265 181 185 184 267 268 269 271 270 187 273 272 274 1U4 IM

Year

61 61 61 61 61 60 60 00 61 61 61 Cl 61 60 61 61 61 60 60

Month

8 8 8 8 8 8 8 8 8 8 8 8 8 8

g g g 10

Day

14.040 14.926 14.976 16.937 16.971 17.787 19.799 19.882 19.897 21.961 21.968 22.041 22.053 25.971 1.812 1.824 4.036 19.818 20.871

13.64 -43.68 9.25 1.80 13.90 - 3 . 7 3 14.50 12.92 -18.99 3.02 7.44 15.77 6.52 2.95 3.38

—1.05 1.76 6.20 1.81

0.971 1.021 0.900 0.927 0.033 1.260 0.934 0.959 1.015 0.679 0.866 0.942 0.984 0.658 0.717 1.834 0.767 0.873 0.778

0.399 0.928 0.926 0.131 0.929 0.970 0.951 0.531 0.292 0.968 0.997 0.914 0.102 1.010 0.058 0.878 0.410 0.787 0.403

26.91 17.56 3.46 26.89 28.03 25.29 5.07 13.88 30.60 12.96 4.89 5.81 3.10 11.60 3.22

356.6 146.4 145.1 144.0 146.1 157.8 151.0 268.4 65.7 153.4 194.3 143.3 144.4 177.4 208.4 216.9 68.4 237.6 248.9

320.8 141.7 141.8 323.6 143.7 144.7 146.6 146.7 146.5 148.5 148.5 148.5 328.6 152.6 158.9 159.0 161.1 176.7 27.3

131.6 110.9 113.8 28.3 112.9 118.2 115.3 148.8 133.8 32.7 43.6 115.5 53.7 36.5 33.5 19.8 7.6 4.6 4.7

317.5 288.1 286.8 107.7 289.8 302.5 297.6 55.0 212.2 301.9 342.8 291.8 113.0 330.0 7.3 15.9 229.5 5 1 3 276.2

- 2 . 6 - 4 . 5 - 5 - 3 . 5

- 4 . 0 - 2 . 0

- 2 . 7 - 2 . 0 - 2 . 8

TOco

1.26 0.91 1.82 0.26

3.62 1.70

7.45 2.76 2.55

Shower or parent

comet

Per Per VII Per Per Per VI VI?

73?

Per?

K Dra

*Cyg 1907IV XCet

below supplement the results obtained for faint meteors.

Distribution of orbits

The distributions of orbital elements for bright meteors were studied in order to show how they differ from corresponding distributions for faint meteors. For sporadic meteors we considered only the semimajor axis, eccentricity, inclination, and aphelion distance. Cosmic weight was not included in our data, which were thus uncorrected for this factor.

Semimajor axis

The distribution of orbits of all sporadic meteors in reciprocal semimajor axis I/a is given in figure 2. For comparison the distributions for faint photographic and radar meteors are also given. For l/a<0.6(a.u.)~1, in all three distributions brighter meteors prevail; for l/a>0.6 (a.u.)~\ the faint meteors become predominant.

In the distribution of all meteors the maxima are at o « 2 . 5 a.u. The second maximum for bright meteors is observed near the parabolic limit.

The percentage of orbits of sporadic meteors with l/a<0.2(a.u.)"¹ is given in table 3. The bright meteors were photographed in Dushanbe and Odessa, the faint meteors in the USA, and the radar meteors were observed in Kharkov (Kashcheyev, Lebedinets, and Lagutin, 1965).

In spite of the fact that the data in this table

240-022 O—67 6

I

BRIGHT METEORS

FAINT METEORS . RADAR

<-3 -Z 0 2 .4 .6 .8 10 1.2 1.4 1.6 1.8 20

FIGURE 2.—Distribution of orbits of sporadic meteors in reciprocal semimajor axis l/a(a.u.)-1.

TABLE 3.—Orbits of sporadic meteors

Meteors Bright

photographic Faint photo-

graphic Radar

Photographic magnitude

« - 3

+ 0.8

«+6 to + 7

Percentage of orbits with I/a

<0.2 (a.u.)-»

34 7 27.4 7.8

are distorted by different observational selec- tion, we may consider that among faint meteors the short-period orbits are predominant.

74 SYMPOSIUM ON METEOR ORBITS AND DUST

It is necessary to note the existence of a considerable percentage of hyperbolic meteors, whereas among radar meteors it is low. This may be explained by the specific character of radar observations of meteors moving at great velocity. There is no reason to believe that all hyperbolic orbits could be explained as due to observational errors.

Inclination

The distribution of inclinations of sporadic meteors (fig. 3) shows that among faint meteors orbits with small inclination (less than 20°) predominate. The maximum in the distributions falls at i=140° both for bright and for faint meteors. In addition, the second maxi-

mum for bright meteors can be observed at an inclination of about 180°.

Eccentricity

The distributions of the eccentricity of bright and faint sporadic meteors are given in figure 4, which shows that bright meteors move on more eccentric orbits than faint meteors.

Orbits with an eccentricity less than 0.65 are found more often among faint meteors, while those with a large eccentricity are found more often among bright meteors. A strongly pronounced maximum at « = 1 for bright meteors should be noted. There is no such maximum for faint meteors (McCrosky and Posen, 1961).

Here the relative number of meteors from t — 0.65 to e = 1 is nearly stable.

2 0

BRIGHT METEORS FAINT METEORS

120 160 180 i°

FIGUKE 3.—Distribution of orbits of sporadic meteors in inclination t.

— BRIGHT METEORS

— -FAINT METEORS

1

0 6 0 8 I.OX.Oe FIGURE 4.—Distribution of orbits of sporadic meteor* in

eccentricity t.

ORBITS OF BRIGHT PHOTOGRAPHIC METEORS BABADZHANOV AND KRAMER 75 Aphelion

The distribution of meteor orbits in aphelion distance up to g' = 10 a. u. is given in figure 5.

The maxima at 2 ' = 1.5 a. u. and 4 a. u. may be noted in the distribution of aphelion of faint sporadic meteors. Bright meteors have one maximum at g' = 3.5 a.u. Small aphelion distances (g'<3 a. u.) are found among faint meteors relatively more often. The percentage

3 0

2 0

O LJ

BRIGHT METEORS ---FAINT METEORS

H

J

"\

8 IO>IO q1 (a.u.)

FIGURE 5.—Distribution of orbits of sporadic meteors in aphelion distance g'(a.u.).

of orbits with aphelion distances of more than 10 a. u. (g'>10 a. u.) is higher for bright than for faint meteors.

The relation between all the other orbital elements for both bright and faint meteors is the same.

From the above we see that bright meteors move in more eccentric orbits than faint meteors and that the inclinations of the orbits of bright meteors are on the average larger than those of faint meteors. It is possible that the differences between bright and faint meteors are due to the Poynting-Robertson effect and the perturbations of the planets.

Meteor associations

In addition to the meteors belonging to showers, there is a separate class of meteor associations which occupies an intermediate position between sporadic and shower meteors. It would be simpler to identify them as weak showers.

The data on the associations discovered mainly from the observations in Dushanbe and Odessa are given in table 4. The Harvard observations were also used in the identification of some associations. The first column of table 4 gives the ordinal number of the association;

the second column gives the meteor number (D, O, and H corresponding to observations in Dushanbe, Odessa, and according to the Har- vard Meteor Program, respectively); the re- maining columns give the date of observation, radiant coordinate, meteor velocity, and the identification of associations with meteor showers (the number is from the list published by Astapovich (1962)). Table 4 contains 16 associations, 4 of which coincide with weak showers in Astapovich's list. The Soviet observations also support the associations discovered by Jaccbia and Whipple (1961) (see tables 1 and 2).

Perseids

Among the orbits of meteors observed in Dushanbe and Odessa there are 167 Perseids, which constitute more than 60 percent of all known photographic Perseid orbits. On the basis of 188 orbits of Perseid meteors observed in the USA, the USSR, and Czechoslovakia, the dependence of the radiant on the solar

76 SYMPOSIUM OX METEOR ORBITS AND DUST

No.

I II III

IV V VI

VII

VIII IX

XI XII

XIII XIV

XVI

Meteors

D 590541 0 39 0 121 D 5 9 1 9 8 7 D 5 7 0 6 7 3 D 570706 D 570774 D 592351b D 592524 H 8089 O 130 D 641623 D 641872 O 1 H 3377 D 620511 II 8215 I) 582652 O 64 O 184 O 267 O 228 O 230 O 264 D 620581 O 237 O 243 D 621025 D 621134 D 621204 O 19 H 3861 O 220 D 583464 D 583587 D 572181 D 572182 D 572384 H 4657 O 87 H 9030 D 573027 O 90 O 104 D 622553 D 614764 D 614794 D 614715 H ' 5557

Year

59 58 59 59 57 57 57 59 59 53 59 64 64 57 52 62 53 58 58 60 61 61 61 61 62 61 61 62 62 62 57 52 61 58 58 57 57 57 52 58 53 57 58 58 62 61 61 61 52

TABLE

Month

3 3 6 7 7 7 7 7 7 7 7 8 8 7 7 8 8 H S 8 8 8 8 8

8 8 8 9 4 8 8 8 9 9 Q 9 9 9 10 10 10 10 10 12 12 12 12 12

4.—Meteor associations Day

6. 7 18.8 29.9 1.9 26. 7 26.8 27.8 12.9 27.8 20. 4 29. 0 8. 8 12. 8 30. 0 24. 3 2. 7 5.4 13.9 12. 0 19. 9 19.9 11. 0 11. 0 16. 9 4. 8 12. 0 12. 0 31. 8 2. 8 3. 8 28.8 30. 5

9.0 17.9 22.9 25.7 25.7 27.8 27. 5 1 3 . 0 1 0 . 4 2 8 . 9 1 9 . 1 23. 1 17.6 11.7 12.9 9.9 9.3

159°

176 285 287 280 278 278 278 280 281 291 284 281 15 10 48 60 17 20 22 10 343 344 356 342 348 328 92 92 91 10 17 13 9 15 0 0 2 3 20 16 102 106 102 84 82 82 73 68

78°

65 -17 -20 49 51 48 49 51 51 49 46 46 35 37 84 83 30 27 25 22

-11 -14 -16 48 54 63 56 59 62 61 63 7 11 - 9 - 9 - 9 - 8 4 12 38 32 27 25 27 17 -10 -10

km/sec

19 20 30 30 31 28 27 30 31 31 28 25 25 65 65 42 44 58 00 65 61 41 40 38 42 47 43 58 61 56 52 52 54 33 32 26 24 21 24 24 24 71 71 70 26 26 25 24 23

Associations

0 Andromeda (No. 177)

7 A q u a rids (No. 163)

X Andromeda (No. 181)

IJ Arietids (No. 246)

longitude was computed (Kramer and Rou- denko, 1965) and found to be:

a=-126?32+l?25(±0?01)X^o,

<5=29?67+0?20(±0?01)XG.

Thus, the daily motion of the radiant in right ascension is l?20 and in declination 0?20.

Computed heliocentric orbits of Perseids change within wide limits. The distribution of heliocentric velocities of photographic Per-

ORBITS OF BRIGHT PHOTOGRAPHIC METEORS—BABADZHANOV AND KRAMER 77 seids is given in figure 6. The solid curve

corresponds to the observations made up to 1959, and the broken curve corresponds to the meteors given in tables 1 and 2. The maximum of these two distributions falls on 41.5 km/sec, which is about 0.3 km/sec less than the parabolic limit. A number of orbits are hyperbolic, in all probability partly due to observational errors; however, we can give some definite data about the existence of hyperbolic orbits in the Perseid shower. Mete- ors with strongly pronounced hyperbolic orbits were found by different observers, for example, Meteors nos. 9792, 14581, 16091, and 21232 from observations at Ondfejov (Ceplecha et al., 1964); nos. 1910, 1918, 2578, 8136, 8666, 8725, 8761, 10570, 11752, etc., from observations at Harvard (Whipple, 1954; Hughes, 1959);

nos. 159, 167, 173, 181, 207, 209, 272, etc., from observations at Odessa; and Meteors nos. 582514, 582561, 583191, 592964, 594472, etc., from observations at Dushanbe. Many of them are Perseids, since the date of observation and the radiant and orbital elements, except for a and e, are close to the average data for the Perseid shower. The orbital elements of meteors are computed on the basis of the earth's coordinates and the vector of the meteor velocity at the moment of observation. When obtained in this way, the orbit is osculating, i.e., we know the motion of the meteor particle at the time of its collision with the earth, but the original orbit is usually unknown. The calculation of the original orbit for each meteor is very difficult indeed, since it is connected, for example, with the effect of various physical factors on the orbit of meteor particles.

Since meteor particles are usually small in size, they are subjected to the Poynting- Robertson and Yarkovsky-Radzievsky effects (Radzievsky, 1952). The forces connected with these effects may considerably change the initial orbit over a long period of time.

To explain the origin of the hyperbolic orbit of individual meteors, we must emphasize once again that these orbits are hyperbolic at the place of collision of a meteor particle with the earth, and that even among the meteors of known elliptic showers, such as the Perseids, individual meteors moving in hyperbolic orbits

39 40 41 42 43

v (km/sec) 44

FIGURE 6.—Distribution of Perseid orbits in heliocentric vebcity Fg (km/sec).

are observed. On the other hand, meteors whose orbits are smaller than the mean orbit are observed in the same shower (Babadzhanov, 1958). The considerable dispersion of the semimajor axis of shower meteor orbits cannot be explained by observational errors. Hence the force that causes a great scatter of orbits in space remains unknown. In any case, it is clear that the hyperbolic nature of some meteor orbits does not necessarily mean that the meteors are of interstellar origin. It is necessary to note that hyperbolic orbits are found more often among bright meteors. It is possible that the distinguishing feature of bright meteors is that some of them move in hyperbolic orbits. We are inclined to believe that hyperbolic orbits can originate within the solar system as the result of physical processes to which some meteor bodies are

78 SYMPOSIUM ON METEOR ORBITS AND DUST

exposed during their "last" approach to the sun (Kramer, Vorobyeva, and Roudenko, 1963;

Babadzhanov and Kramer, 1963; Ceplecha et al., 1964).

There is no doubt that more precise observations are needed to reveal the hyperbolic orbits, and it is also necessary to investigate the mechanisms that are capable of trans- ferring a meteor particle from an elliptical to a hyperbolic orbit.

Relation between meteor bodies and other bodies of the solar system

Photographic observations of bright meteors confirm their relation to comets. In the last columns of tables 1 and 2 the names of the known showers as well as the parent come Us are indicated. Sometimes they are individual sporadic meteors. Their relation to comets may be purely formal, but according to their general orbital characteristics (e.g., eccentricity, inclination) bright meteors appear to be connected with comets. It can be remarked that Whipple's K criterion for these orbits suggests a cometary relationship. However, the identification of meteors for which l f < 0 with asteroids does not seem to have sufficient basis, since orbital characteristics alone are insuffi- cient to draw conclusions regarding the "ge- neric" connection between meteors and asteroids or comets.

In 1964 experiments were made in the USSR on the photography of meteors by the method of instantaneous exposure. Photographs with an exposure of 0.5 msec were obtained by Babadzhanov and Kramer (1965). Meteor images on these photos were very little distorted by the motion of the meteor on the emulsion.

For slow meteors these images may be considered instantaneous. From such photographs the instantaneous structure of meteors can be studied. The photographs presented here il- lustrate instantaneous images of some meteors.

The first (Meteor no. 641541, plate la) belongs to a Perseid, and the second (Meteor no.

641872, plate 16) to a weak shower (association III, table 4). It is interesting to note that the photographs of all Perseids are nearly the same as in plate la, i.e., they have short tails.

Meteor no. 641623, according to its orbital

characteristics, belongs to the same association III as does Meteor no. 641872 according to its instantaneous image (plate lc). The tails of Meteors nos. 641872 and 641623 are similar in size and shape. Thus, the luminosity characteristics of these two meteors confirm their common origin and the reality of meteor associations.

References

ASTAPOVICII, I. S.

1062. Astronomical Calendar. Permanent sec- tion, pp. 616-637.

BABADZHANOV, P. B.

1958. Photographic observations of Perseids.

A-tmphN.-. ln.-t Acad. tSci. Tadjikiszan, no. 20, pp. 13-20.

HABADZIIANOV, P. B., and KKAMEK, K. N.

1963. McthodH nnd no me n -ult- of the photo- graphic researches of meteors. In Ion- osphere and Meteors, Hoc. V of IGY Program No. 12, Publ. House Acad.

Sci. USSR, Moscow.

1965. Instantaneous meteor photography pre- liminary results. Astron. Journ. USSR, vol. 42, pp. 660-665.

CEPLECHA, Z.; JE2KOVA, M.; NOVAK, M.; RAJCHL, J.;

SEHNAL, L.; and DAVIES, J. G.

1964. Ondfejov double-station meteors during the IGY and IGC. Bull. Astron. Inst.

Czechoslovakia, vol. 15, pp. 144-155.

HUGHES, R. F.

1959. Meteor trains. Smithsonian Contr. Astro- phys., vol. 3, no. H, pp. 79-94.

JACCHIA, L. G., and WHIPPLE, F. L.

1961. Precision orbits of 413 photographic meteors. Smithsonian Contr. Aatro- phys., vol. 4, no. 4, pp. 97-129.

KASHCHEYEV, B. L.; LEBEDINETS, V. N.; and LAGUTIN,

M. F.

1965. The motion of small meteoric bodies.

Doklady Akad. Nauk SSSR, vol. 164, pp. 1256-1259.

KRAMER, E. N.

1953. On the detcrminat on of flash times of meteors by means of a chopping shutter.

Astron. Circ. USSR, no. 135, pp. 10-12.

KRAMER, E. N., and ROUDENKO, O. A.

1965. Photographic observations of the Perseids.

Astron. Journ. USSR, vol. 42, pp.

416-423.

KRAMER, E. N.; VOROBYEVA, V. A.; and ROUDENKO,

O. A.

1963. The experiences of the Astronomical Observ- atory of Odessa in meteor surveillance during the International Geophysical Year. Astron. Obs. Odessa, vol. 5, pp. 5-63.

ORBITS OF BRIGHT PHOTOGRAPHIC METEORS BABADZHANOV AND KRAMER 79

MCCROSKY, R. E., and POSBN, A. of asteroids and meteorites. Astron- 1961. Orbital elements of photographic meteors. Jo urn. USSR, vol. 29, pp. 162-170.

Smithsonian Contr. Astrophys., vol. 4,

no. 2, pp. 15-84. WHIPPLE, F. L.

RADZIEVSKY, V. V. 1954. Photographic meteor orbits and their 1952. On the effect of an isotropic reemission distribution in space. Astron. Journ.,

of solar radiation on the orbital motion vol. 59, pp. 201-217.

Abstract

The distributions of orbital elements of bright meteors (M<1 mag), which were photographed in 1957-1963 in Dushanbe and Odessa, are studied. It is concluded that bright meteors move in more eccentric orbits than faint meteors, which were photographed by Baker Super-Schmidt cameras. The inclinations of orbits of bright meteors arc on the average larger than those of faint meteors. The reality of hyperbolic meteor orbits is discussed. Photo- graphic observations of meteors made by the method of instantaneous exposure show that meteors belonging to different showers or associations have respectively different luminosity and fragmentation characteristics. Data about orbital elements of meteors photographed in 1960 to 1963 in Dushanbe and Odessa are presented.

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