Angular momentum and local gravitational instability in galaxy discs: does Q correlate with j or M ?
Artikel i vetenskaplig tidskrift, 2018

We introduce a new diagnostic for exploring the link between angular momentum and local gravitational instability in galaxy discs. Our diagnostic incorporates the latest developments in disc instability research, is fully consistent with approximations that are widely used for measuring the stellar specific angular momentum, j⋆ = J⋆/M⋆, and is also very simple. We show that such a disc instability diagnostic hardly correlates with j⋆ or M⋆, and is remarkably constant across spiral galaxies of any given type (Sa-Sd), stellar mass (M_{⋆}=10^{9.5}-10^{11.5} M_{⊙}), and velocity dispersion anisotropy (σz⋆/σR⋆ = 0-1). The fact that M⋆ is tightly correlated with star formation rate, molecular gas mass (Mmol), metallicity (12 + log O/H), and other fundamental galaxy properties thus implies that nearby star-forming spirals self-regulate to a quasi-universal disc stability level. This not only proves the existence of the self-regulation process postulated by several star formation models, but also raises important caveats.

instabilities

galaxies: kinematics and dynamics

ISM: kinematics and dynamics

stars: kinematics and dynamics

galaxies: ISM

galaxies: star formation

Författare

Alessandro Romeo

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Extragalaktisk astrofysik

Keoikantse Moses Mogotsi

Monthly Notices of the Royal Astronomical Society: Letters

1745-3933 (ISSN)

Vol. 480 1 L23-L27

Ämneskategorier

Astronomi, astrofysik och kosmologi

Fundament

Grundläggande vetenskaper

DOI

10.1093/mnrasl/sly119

Mer information

Skapat

2018-08-06