Monarchs in Australia: On the winds of a storm?

The monarch butterfly, Danaus plexippus, is one of Australia's best-known exotic butterflies, being first recorded here in the spring/summer of 1870/1871. However, the source of the original population is unknown. Using historical records we suggest that the most likely source of the founder population was from Vanuatu and/or New Caledonia. Many almost simultaneous 'first records' for the butterfly in Australia suggest that a large, well-distributed population was present when first noticed. While such a population may have developed from a limited number of individuals flying across the Coral Sea, the well documented, very dramatic appearance of large monarch populations in Australia does not appear to fit this model. Rather, we hypothesise that large numbers of monarchs were carried to Australia on cyclonic winds: no fewer that 3 cyclones hit the Queensland coast in early 1870. If one or more of these cyclones tracked from the Vanuatu/New Caledonia chain, then they may have transported monarchs. Once established on the central/northern Queensland coast, natural migration would account for the appearance of butterflies further south.

Cluster cannibalism and scaling relations of galactic stellar nuclei

Recently, very massive compact stellar systems have been discovered in the intracluster regions of galaxy clusters and in the nuclear regions of late-type disk galaxies. It is unclear how these compact stellar systems - known as ultracompact dwarf (UCD) galaxies or nuclear clusters (NCs) - form and evolve. By adopting a formation scenario in which these stellar systems are the product of multiple merging of star clusters in the central regions of galaxies, we investigate, numerically, their physical properties. We find that physical correlations among velocity dispersion, luminosity, effective radius, and average surface brightness in the stellar merger remnants are quite different from those observed in globular clusters. We also find that the remnants have triaxial shapes with or without figure rotation, and these shapes and their kinematics depend strongly on the initial number and distribution of the progenitor clusters. These specific predictions can be compared with the corresponding results of ongoing and future observations of UCDs and NCs, thereby providing a better understanding of the origin of these enigmatic objects.