The Bakerian Lecture, 1982: Galaxies and their nuclei
This lecture briefly reviews current ideas on some key problems in extragalactic physics. Our understanding of galaxies and how they evolve is still tentative and fragmentary – perhaps at the same level as the study of stellar structure several decades ago. The ‘seeds’ from which galaxies formed were small-amplitude fluctuations imprinted during the initial high-energy phases of the Big Bang; but it is conventional physics - gas dynamics, atomic physics and Newtonian gravity - that determines their characteristic sizes and shapes. Quantitative modelling of galactic evolution is impeded by our poor understanding of how stars form from protogalactic gas. Another stumbling block has been the realization that 90% of the gravitating material in galaxies is in some ‘hidden’ form: the conspicuous stars and gas are merely ‘sediment’ in a potential well ten times larger contributed by material of unknown nature. The hidden mass could be small faint stars or the collapsed remnants of massive stars; alternatively, it could be some species of particle surviving from the Big Bang. Some galaxies harbour, in their centres, ‘engines’ more powerful than the entire integrated output of their ca 10 11 constituent stars. Extreme instances of this phenomenon are the quasars – galactic nuclei that flare up to outshine the rest of the galaxy. Galaxies sometimes eject wellcollimated jets of (possibly electron-positron) plasma, flowing at almost the speed of light. These jets, transporting an energy flux that may amount to an entire galactic luminosity, propagate for up to 10 6 light years; their interaction with the external medium is manifested in the intense synchrotron radiation from strong radio sources. Active galactic nuclei probably involve spinning black holes of 10 8 M ⊙ (described in Einstein’s theory by the Kerr metric) created by a runaway gravitational collapse. The luminosity and the plasma outflow could be energized by infall of surrounding material, or by the rotational energy of the holes, which can be extracted via electromagnetic torques. Massive black holes may lurk quiescent in the centres of several nearby galaxies, and even at our own Galactic Centre.