Chapter XIII · THE ASTEROID RING BETWEEN MARS AND JUPITER.
Reading edition
The mean distances of the minor planets between Mars and Jupiter vary from 2·20 to 3·49. The breadth of the zone is therefore 20,000,000 miles greater than the distance of the earth from the sun; greater even than the entire interval between the orbits of Mercury and Mars. Moreover, the perihelion distance of some members of the group exceeds the aphelion distance of others by a quantity equal to the whole interval between the orbits of Mars and the earth. The Olbersian hypothesis of the origin of these bodies seems thus to have lost all claim to probability.30 Professor Alexander's theory of the disruption of a primitive discoidal planet of great equatorial diameter, is less objectionable; still, however, it requires confirmation. But whatever may have been the original constitution of the ring,31 its existence in its present form for an indefinite period is unquestioned. Let us then consider some of the effects of its secular perturbation by the powerful mass of Jupiter.
Portions of the ring in which the periods of asteroids would be commensurable with that of Jupiter.—The breadth of this zone is such as to contain several portions in which the periods of asteroids would be commensurable with that of Jupiter. As in the case of the perturbation of Saturn's ring by the interior satellites, the tendency of Jupiter's influence would be to form gaps or chasms in the primitive ring.
The mean distance of an asteroid whose period is 1/2 that of Jupiter =3·2776
That of one whose period is 1/3 of Jupiter's =2·5012
That of one whose period is 2/5 of Jupiter's =2·8245
That of one whose period is 2/7 of Jupiter's =2·2569
That of one whose period is 3/7 of Jupiter's =2·9574
That of one whose period is 4/9 of Jupiter's =3·0299
For the purpose of facilitating the comparison of these numbers with the mean distances of the asteroids and of observing whether any order obtains in the distribution of these mean distances in space, we have arranged the minor planets, in the following table, in the consecutive order of their periods:
Periods and Distances of the Asteroids.
Order of Discovery. Name. Distance. Period.
8 Flora 2·2014 1193 d
43 Ariadne 2·2034 1194·6
72 Feronia 2·2654 1245·4
40 Harmonia 2·2677 1247·3
18 Melpomene 2·2956 1270·4
80 Sappho 2·2971 1271·6
12 Victoria 2·3342 1302·6
27 Euterpe 2·3468 1313·2
4 Vesta 2·3613 1325·3
84 Clio 2·3618 1325·8
30 Urania 2·3655 1328·9
51 Nemausa 2·3657 1329·0
9 Metis 2·3858 1346·0
7 Iris 2·3863 1346·5
60 Echo 2·3931 1352·2
63 Ausonia 2·3949 1353·8
25 Phocea 2·4008 1358·8
20 Massilia 2·4144 1365·5
67 Asia 2·4217 1376·5
44 Nysa 2·4234 1378·0
6 Hebe 2·4244 1379·0
83 Beatrice 2·4287 1382·5
42 Isis 2·4400 1392·2
21 Lutetia 2·4411 1393·0
19 Fortuna 2·4416 1393·5
79 Eurynome 2·4437 1395·3
11 Parthenope 2·4519 1402·4
17 Thetis 2·4737 1421·1
46 Hestia 2·5262 1466·5
89 2·5498 1487·2
29 Amphitrite 2·5544 1491·2
5 Astræa 2·5772 1511·2
13 Egeria 2·5775 1511·4
14 Irene 2·5860 1519·0
32 Pomona 2·5868 1519·6
91 2·5958 1527·5
56 Melete 2·5959 1527·7
70 Panopea 2·6129 1543·0
53 Calypso 2·6188 1548·0
78 Diana 2·6236 1555·3
23 Thalia 2·6280 1568·0
37 Fides 2·6414 1570·0
15 Eunomia 2·6436 1572·6
85 Io 2·6466 1573·0
50 Virginia 2·6491 1575·0
88 Thisbe 2·6553 1580·0
26 Proserpina 2·6561 1581·1
66 Maia 2·6635 1587·8
73 Clytie 2·6666 1590·5
3 Juno 2·6707 1594·2
75 Eurydice 2·6707 1594·2
77 Frigga 2·6719 1595·3
64 Angelina 2·6805 1603·0
34 Circe 2·6865 1608·3
58 Concordia 2·7014 1622·0
54 Alexandra 2·7123 1631·6
59 Elpis 2·7131 1632·3
45 Eugenia 2·7218 1640·1
38 Leda 2·7401 1656·8
36 Atalanta 2·7458 1662·0
71 Niobe 2·7501 1665·8
82 Alcmene 2·7547 1670·0
55 Pandora 2·7591 1674·0
41 Daphne 2·7657 1679·9
1 Ceres 2·7663 1681·0
2 Pallas 2·7696 1683·5
39 Lætitia 2·7740 1687·6
74 Galatea 2·7777 1690·9
28 Bellona 2·7785 1691·6
68 Leto 2·7836 1696·3
81 Terpsichore 2·8591 1765·7
33 Polyhymnia 2·8653 1770·6
47 Aglaia 2·8812 1786·4
22 Calliope 2·9092 1812·4
16 Psyche 2·9233 1826·0
69 Hesperia 2·9707 1871·1
61 Danaë 2·9837 1882·4
35 Leucothea 3·0040 1904·2
49 Pales 3·0825 1976·6
86 Semele 3·0909 1984·7
52 Europa 3·1000 1993·6
48 Doris 3·1094 2002·7
62 Erato 3·1297 2022·3
24 Themis 3·1431 2035·3
10 Hygeia 3·1512 2043·2
31 Euphrosyne 3·1513 2044·6
57 Mnemosyne 3·1565 2048·4
90 Antiope 3·1576 2049·4
76 Freia 3·3864 2276·2
65 Cybele 3·4205 2310·6
87 Sylvia 3·4927 2384·2
Remarks on the foregoing Table.
1. The first two members of the group, Flora and Ariadne, have very nearly the same mean distance. Immediately exterior to these, however, occurs a wide interval, including the distance at which seven periods of an asteroid would be equal to two of Jupiter.
2. On the outer limit of the ring Freia, Cybele, and Sylvia have also nearly equal distances, and are separated from the next interior member by a wide space including the distance at which two periods would be equal to one of Jupiter, and also that at which five would be equal to one of Saturn.
3. Besides these extreme members of the group, our table contains eighty-six minor planets, all of which are included between the distances 2·26 and 3·16; the mean interval between them being 0·0105. The distances are distributed as follows:
2·26 to 2·36 6 minimum.
2·36 to 2·46 19 maximum.
2·46 to 2·56 4 minimum.
2·56 to 2·66 16 } maximum.
2·66 to 2·76 16
2·76 to 2·86 8
2·86 to 2·96 4 } minimum.
2·96 to 3·06 3
3·06 to 3·16 10 maximum.
The clustering tendency is here quite apparent.
4. The three widest intervals between these bodies are—
(a) between Leucothea and Pales 0·0785,
(b) between Leto and Terpsichore 0·0755,
(c) between Thetis and Hestia 0·0525;
and these, it will be observed, are the three remaining distances, indicated on a previous page, at which the periods of the primitive meteoric asteroids would be commensurable with that of Jupiter. Now, if the original ring consisted of an indefinite number of separate particles moving with different velocities, according to their respective distances, those revolving at the distance 2·4935—in the interval between Thetis and Hestia—would make precisely three revolutions while Jupiter completes one. A planetary particle at this distance would therefore always come in conjunction with Jupiter in the same parts of its path: consequently its orbit would become more and more eccentric until the particle itself would unite with others, either exterior or interior, thus forming an asteroidal nucleus, while the primitive orbit of the particle would be left destitute of matter, like the interval in Saturn's ring.
5. If the distribution of matter in the zone was originally nearly continuous, as in the case of Saturn's rings, it would probably break up into a number of concentric annuli. On account, however, of the great perturbations to which they were subject, these narrow rings would frequently come in collision. After their rupture, and while the fragments were collecting in the form of asteroids, numerous intersections of orbits and new combinations of matter would occur, so as to leave, in the present orbits, but few traces of the rings from which the existing asteroids were derived. A comparison, however, of the elements of Clytie and Frigga shows a striking similarity; and Professor Lespiault has pointed out a corresponding likeness between the orbits of Fides and Maia. For these four asteroids the nodal lines and also the inclinations are nearly the same; while the periods differ by only a few days. It is probable, therefore, that they are all fragments of the same narrow ring. Finally, as they all move nearly in the same plane, they must at some future time approach extremely near each other, and perhaps become united in one large asteroid.