The process of unravelling the formation history of galaxies (also referred to as galactic archaeology) depends largely on the measurement of the ages of stellar populations contained within the galaxies. Since our own galaxy is a spiral, most of our understanding of spiral galaxy formation comes from studies of the stellar populations within the Milky Way.
Although the formation of galaxies is not fully understood, astronomers have identified the three key processes involved:
The degree to which each of these processes contributes to the formation of any particular galaxy is thought to depend on the galaxy’s Hubble type. In particular, the formation of spiral galaxies is thought to be a complex process in which the stellar halo, bulge and disks are formed at different times and through different mechanisms.
Bulges and Halos
While the above scenario appears to account well for the stellar populations found in the bulges of Sa and Sb galaxies, the bulge populations for Sc and Sd galaxies are actually the same as those found in the disks of these galaxies. This would suggest that the bulges of extremely late-type spiral galaxies are formed almost entirely through secular evolution processes.
The stars in the disks of spiral galaxies are generally younger than the majority of stars found in the bulge and halo. For this reason, disks are thought to form after the primordial collapse event responsible for the formation of the spheroidal bulge and halo, possibly through the cooling of the hot gas contained within the halo of the newly formed galaxy. However, this cannot be the whole picture, as many spiral galaxies possess two distinct disk structures (a thick disk and a thin disk) which vary in content (thick disks are composed entirely of stars while thin disks also contain cold gas) as well as thickness.
An alternative to this major merger scenario is one in which the thick disk formed relatively slowly through the actions of multiple minor mergers. Once the merger events had formed the thick disk, the stars retained the scale height of the thick disk while the cold gas collapsed back into the galactic plane to form the thin disk. The Milky Way is currently subject to at least two minor mergers (with the Sagittarius and Canis Major dwarf galaxies) so this minor merger scenario may be credible.
Other, non-merger, models (including secular evolution heating processes and various forms of the primordial collapse model) have also been put forward to explain the formation of thick disks. However, these models have difficulty predicting the observed properties of the Milky Way’s thick disk and are not generally favoured.
The final aspect of the formation of spiral galaxies is the on-going star formation evident in their thin disks. This star formation is usually on the leading edge of the spiral arms where the cold gas of the thin disk is compressed, and provides unequivocal evidence for on-going secular evolution in thin disks.