On the chains of star complexes and superclouds in spiral arms

TL;DR

This paper investigates the formation and distribution of star complexes and superclouds in spiral arms, proposing magneto-gravitational instability as a key mechanism, and compares observations across different galaxies to understand their rarity and underlying processes.

Contribution

It introduces the idea that magneto-gravitational instability influences the formation of star complexes and superclouds in spiral arms, supported by observational evidence from M31 and other galaxies.

Findings

Regular chains of star complexes are located within gas-dust lanes.

The wavelength of magnetic fields correlates with complex spacing, suggesting magneto-gravitational instability.

Anti-correlation observed between shock signatures and star complex presence.

Abstract

The relation is studied between occurrence of a regular chain of star complexes and superclouds in a spiral arm, and other properties of the latter. A regular string of star complexes is located in the north-western arm of M31; they have about the same size 0.6 kpc with spacing of 1.1 kpc. Within the same arm segment the regular magnetic field with the wavelength of 2.3 kpc was found by Beck et al. (1989). We noted that this wavelength is twice as large as the spacing between complexes and suggested that they were formed in result of magneto-gravitational instability developed along the arm. In this NW arm, star complexes are located inside the gas-dust lane, whilst in the south-western arm of M31 the gas-dust lane is upstream of the bright and uniform stellar arm. Earlier, evidence for the age gradient has been found in the SW arm. All these are signatures of a spiral shock, which may be associated with unusually large (for M31) pitch-angle of this SW arm segment. Such a shock may prevent the formation of the regular magnetic field, which might explain the absence of star complexes there. Anti-correlation between shock wave signatures and presence of star complexes is observed in spiral arms of a few other galaxies. Regular chains of star complexes and superclouds in spiral arms are rare, which may imply that a rather specific mechanism is involved in their formation, and the most probable one is the Parker-Jeans instability. The spiral pattern of our Galaxy is briefly discussed; it may be of M101 type in the outer parts. The regular bi-modal spacing of HI superclouds is found in Carina and Cygnus (Outer) arms, which may be an indirect evidence for the regular magnetic field along these arms.