THE MASS SPECTRUM OF THE FIRST STARS
By Hajime Susa, K. Hasegawa, Nozomu Tominaga. 2014
190 citations recorded by the source corpus.
We perform cosmological hydrodynamics simulations with non-equilibrium primordial chemistry to obtain 59 minihalos that host first stars. The obtained minihalos are used as the initial conditions of local three-dimensional radiation hydrodynamics simulations to investigate the formation of the first stars. We find that two-thirds of the minihalos host multiple stars, while the other third has single stars. The mass of the stars found in our simulations are in the range of 1 M☉ ≲ M ≲ 300 M☉, peaking at several× 10 M☉. Most of the very massive stars of ≳ 140 M☉ are born as single stars, although not all of the single stars are very massive. We also find a few stars of ≲ 1 M☉ that are kicked by the gravitational three body interactions to the position distant from the center of mass. The frequency that a star forming minihalo contains a binary system is ∼50%. We also investigate the abundance pattern of the stellar remnants by summing up the contributions from the first stars in the simulations. Consequently, the pattern is compatible with that of the low metallicity damped Lyα systems or the extremely metal-poor (EMP) stars, if the mass spectrum obtained in our experiment is shifted to the low mass side by 0.2 dex. If we consider the case that an EMP star is born in the remnant of the individual minihalo without mixing with others, the chemical signature of the pair instability supernova is more prominent, because most of them are born as single stars.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/525225219c0448716b33ac20f105d4b16c4a4fbc
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Citations in the corpus
- FORMATION OF MASSIVE PRIMORDIAL STARS: INTERMITTENT UV FEEDBACK WITH EPISODIC MASS ACCRETION (2015, background): “This is in contrast to the conclusions of Susa (2013) and Susa et al. (2014), who show that mass accretion can be halted by FUV feedback alone.”
- GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS (2016, background): “Additionally, lower mass (<8 M ) Pop III stars that may exist in such galaxies have a negligible contribution to the stellar mass and luminosity because of their low star formation efficiencies (e.g., Susa et al. 2014) when compared to the first galaxies (e.g., Wise et al. 2014).”
- Building up the Population III initial mass function from cosmological initial conditions (2016, methodology): “Susa et al. (2014) used three-dimensional simulations and a minimum resolution radius of 30 AU to study Pop III star formation within several tens of haloes under photodissociating feedback, finding a wide range of stellar masses and multiplicities, with a mass spectrum ranging from 1 to > 100 M⊙.”
- Formation of Supermassive Black Hole Seeds (2016, background): “They found that stellar masses range from 10-1000 M⊙ and depend on PASA (2016) doi:10.1017/pas.2016.xxx the properties of their natal halos, also see Susa et al. (2014).”
- Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution (2015, background): “In this case, the available gas in the envelope is divided among multiple protostars, so that the stars in such a multiple system could have relatively lower masses than in the case of a single star (e.g., Peters et al. 2010; Susa et al. 2014).”