TY - JOUR

T1 - The Origin of Massive Stars

T2 - The Inertial-inflow Model

AU - Padoan, Paolo

AU - Pan, Liubin

AU - Juvela, Mika

AU - Haugbolle, Troels

AU - Nordlund, Ake

PY - 2020/9/3

Y1 - 2020/9/3

N2 - We address the problem of the origin of massive stars, namely the origin, path, and timescale of the mass flows that create them. Based on extensive numerical simulations, we propose a scenario where massive stars are assembled by large-scale, converging, inertial flows that naturally occur in supersonic turbulence. We refer to this scenario of massive-star formation as the inertial-inflow model. This model stems directly from the idea that the mass distribution of stars is primarily the result of turbulent fragmentation. Under this hypothesis, the statistical properties of turbulence determine the formation timescale and mass of prestellar cores, posing definite constraints on the formation mechanism of massive stars. We quantify such constraints by analyzing a simulation of supernova-driven turbulence in a 250 pc region of the interstellar medium, describing the formation of hundreds of massive stars over a time of approximately 30 Myr. Due to the large size of our statistical sample, we can say with full confidence that massive stars in general do not form from the collapse of massive cores nor from competitive accretion, as both models are incompatible with the numerical results. We also compute synthetic continuum observables in the Herschel and ALMA bands. We find that, depending on the distance of the observed regions, estimates of core mass based on commonly used methods may exceed the actual core masses by up to two orders of magnitude and that there is essentially no correlation between estimated and real core masses.

AB - We address the problem of the origin of massive stars, namely the origin, path, and timescale of the mass flows that create them. Based on extensive numerical simulations, we propose a scenario where massive stars are assembled by large-scale, converging, inertial flows that naturally occur in supersonic turbulence. We refer to this scenario of massive-star formation as the inertial-inflow model. This model stems directly from the idea that the mass distribution of stars is primarily the result of turbulent fragmentation. Under this hypothesis, the statistical properties of turbulence determine the formation timescale and mass of prestellar cores, posing definite constraints on the formation mechanism of massive stars. We quantify such constraints by analyzing a simulation of supernova-driven turbulence in a 250 pc region of the interstellar medium, describing the formation of hundreds of massive stars over a time of approximately 30 Myr. Due to the large size of our statistical sample, we can say with full confidence that massive stars in general do not form from the collapse of massive cores nor from competitive accretion, as both models are incompatible with the numerical results. We also compute synthetic continuum observables in the Herschel and ALMA bands. We find that, depending on the distance of the observed regions, estimates of core mass based on commonly used methods may exceed the actual core masses by up to two orders of magnitude and that there is essentially no correlation between estimated and real core masses.

KW - Interstellar medium

KW - Protostars

KW - Interstellar dynamics

KW - Magnetohydrodynamics

KW - Star formation

KW - ADAPTIVE MESH REFINEMENT

KW - SUPER-ALFVENIC MODEL

KW - MOLECULAR CLOUDS PREDICTIONS

KW - ORDER GODUNOV SCHEME

KW - DENSE CORES

KW - GRAVITATIONAL COLLAPSE

KW - CONSTRAINED TRANSPORT

KW - INITIAL CONDITIONS

KW - MAGNETIC-FIELD

KW - MAIN CLOUD

U2 - 10.3847/1538-4357/abaa47

DO - 10.3847/1538-4357/abaa47

M3 - Journal article

VL - 900

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 82

ER -