On Possibility of Star Formation Triggered by Multiple Supernovae in Dwarf Galaxies

Vasiliev, E. O.; Shchekinov, Yu. A.; Koval’, V. V.; Egorov, Oleg V.

doi:10.1134/s1990341322020109

Cited by 1 publication

(1 citation statement)

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“…A higher fraction of the younger associations on the edge of superbubbles points towards sequential star formation (Elmegreen & Lada 1977), or triggering of star formation as a result of the evolution of the superbubble (e.g., Hartmann et al 2001), though it is usually hard to distinguish between these processes (Dale et al 2015). The triggering of star formation in the periphery of expanding supershells as a result of their interaction with the surrounding ISM, or collision with each other, is predicted in simulations (e.g., Ntormousi et al 2011;Inutsuka et al 2015;Vasiliev et al 2022), and indications of this have been observed in very nearby dwarf galaxies (below 4 Mpc, see, e.g., Lozinskaya 2002;Egorov et al 2017Egorov et al , 2018Fujii et al 2021). Dawson et al (2013) demonstrated that about 12−25% of the molecular gas in the supergiant shells in the LMC was formed as a result of their interaction with the ISM.…”

Section: Ionised Superbubbles: Energy Balance and Possible Signs Of S...mentioning

confidence: 97%

Quantifying the energy balance between the turbulent ionised gas and young stars

Egorov,

Kreckel,

Glover

et al. 2023

A&A

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Context. Stellar feedback is a key contributor to the morphology and dynamics of the interstellar medium in star-forming galaxies. In particular, energy and momentum input from massive stars can drive the turbulent motions in the gas, but the dominance and efficiency of this process are unclear. The study of ionised superbubbles enables quantitative constraints to be placed on the energetics of stellar feedback. Aims. We directly compare the kinetic energy of expanding superbubbles and the turbulent motions in the interstellar medium with the mechanical energy deposited by massive stars in the form of winds and supernovae. With such a comparison, we aim to determine whether the stellar feedback is responsible for the observed turbulent motions and to quantify the fraction of mechanical energy retained in the superbubbles. Methods. We investigated the ionised gas morphology, excitation properties, and kinematics in 19 nearby star-forming galaxies from the PHANGS-MUSE survey. Based on the distribution of the flux and velocity dispersion in the Hα line, we selected 1484 regions of locally elevated velocity dispersion (σ(Hα) > 45 km s−1), including at least 171 expanding superbubbles. We analysed these regions and related their properties to those of the young stellar associations and star clusters identified in PHANGS-HST data. Results. We find a good correlation between the kinetic energy of the ionised gas and the total mechanical energy input from supernovae and stellar winds from the stellar associations. At the same time, the contribution of mechanical energy injected by the supernovae alone is not sufficient to explain the measured kinetic energy of the ionised gas, which implies that pre-supernova feedback in the form of radiation and thermal pressure as well as winds is necessary. We find that the gas kinetic energy decreases with metallicity for our sample covering Z = 0.5 − 1.0 Z⊙, reflecting the lower impact of stellar feedback. For the sample of well-resolved superbubbles, we find that about 40% of the young stellar associations are preferentially located in their rims. We also find a slightly higher (by ∼15%) fraction of the youngest (< 3 Myr) stellar associations in the rims of the superbubbles than in the centres and the opposite trend for older associations, which implies possible propagation or triggering of star formation. Conclusions. Stellar feedback is the dominant source for powering the ionised gas in regions of locally (on a 50–500 pc scale) elevated velocity dispersion, with a typical coupling efficiency of 10 − 20%. Accounting for pre-supernovae feedback is required to set up the energy balance between gas and stars.

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Section: Ionised Superbubbles: Energy Balance and Possible Signs Of S...mentioning

confidence: 97%

Quantifying the energy balance between the turbulent ionised gas and young stars

Egorov,

Kreckel,

Glover

et al. 2023

A&A

View full text Add to dashboard Cite

show abstract

On Possibility of Star Formation Triggered by Multiple Supernovae in Dwarf Galaxies

Cited by 1 publication

References 45 publications

Quantifying the energy balance between the turbulent ionised gas and young stars

Quantifying the energy balance between the turbulent ionised gas and young stars

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