The Planetary Companions to PSR B1257 + 12
Mazeh and Goldman (1995) have pointed out the similarity between the mass-ratios of the planets relative to the central star and the distances from the central star (scaled by the distance of the third planet) between the planetary companions of Wolszczan’s pulsar PSR B1257+12 and the inner planets of the Solar System. According to the ‘standard model’ of the formation of the terrestrial planets, the accretions disks from which the planets formed had similar densities. However, a significant difference between the two planetary systems is that the Earth and Venus counterparts in the pulsar system are almost exactly in a 3:2 resonance mean-motion resonance; the Earth and Venus are not. I suggest that this configuration is unlikely to be a accident of formation but that the planets migrated into that configuration.
KeywordsAccretion Disk Planetary System Terrestrial Planet Central Star Gravitational Instability
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