Evolution of massive Population III stars with rotation and magnetic fields

By Sung-Chul Yoon, A. Dierks, N. Langer. 2012

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[Abridged] We present a new grid of massive population III star models including the effects of rotation on the stellar structure and chemical mixing, and magnetic torques for the transport of angular momentum. Based on the grid, we also present a phase diagram for the expected final fates of rotating massive Pop III stars. Our non-rotating models become redder than the previous models in the literature, given the larger overshooting parameter adopted in this study. In particular, convective dredge-up of the helium core material into the hydrogen envelope is observed in our non-rotating very massive star models (>~200 Msun), which is potentially important for the chemical yields. On the other hand, the stars become bluer and more luminous with a higher rotational velocity. With the Spruit-Tayler dynamo, our models with a sufficiently high initial rotational velocity can reach the critical rotation earlier and lose more mass as a result, compared to the previous models without magnetic fields. The most dramatic effect of rotation is found with the so-called chemically homogeneous evolution (CHE), which is observed for a limited mass and rotational velocity range. CHE has several important consequences: 1) Both primary nitrogen and ionizing photons are abundantly produced. 2) Conditions for gamma-ray burst progenitors are fulfilled for an initial mass range of 13 - 84 Msun. 3) Pair instability supernovae of type Ibc are expected for 84 -190 Msun and 4) Both a pulsational pair instability supernova and a GRB may occur from the same progenitor of about 56 - 84 Msun, which might significantly influence the consequent GRB afterglow. We find that CHE does not occur for very massive stars (>190 Msun), in which case the hydrogen envelope expands to the red-supergiant phase and the final angular momentum is too low to make any explosive event powered by rotation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2f1d5c3c7062dbf832c5d4b8d357926b35d64c1f

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Citations in the corpus

Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution (2015, background): “Yoon et al. (2012) perform stellar evolution calculations and categorize the final fates of primordial stars as a function of the stellar masses.”
ONE HUNDRED FIRST STARS: PROTOSTELLAR EVOLUTION AND THE FINAL MASSES (2013, background): “Table 4 lists the final fate of zero-metallicity stars calculated by Yoon et al. (2012).”
Pulsational Pair-instability Supernovae (2016, background): “At very low metallicity, rotating models may also copiously produce primary 14N (Meynet & Maeder 2002; Heger & Woosley 2010; Yoon et al. 2012).”
The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, background): “Similar profound improvements were achieved in the field of stellar evolution by the inclusion of physical processes such as stellar rotation (Meynet & Maeder 2003, 2005) and recently magnetic fields (Maeder & Meynet 2005; Yoon et al. 2012).”
FORMATION OF PRIMORDIAL SUPERMASSIVE STARS BY RAPID MASS ACCRETION (2013, background): “Indeed, Yoon et al. (2012) show that the ultimate fates of M∗ ≤ 10 3 M⊙ primordial stars vary with these parameters.”
The THESEUS space mission concept: science case, design and expected performances (2017, background): “Stellar evolution predicts that long GRBs may be expected from fast rotating, single Pop III stars with an initial mass of 10-80 M (Yoon et al., 2012).”
Evolution and fate of very massive stars (2013, methodology): “…M and SMC 150 M models as a function of age of the star. and zero metallicity stars (Hirschi 2007; Ekström et al. 2008; Chatzopoulos & Wheeler 2012; Yoon et al. 2012), mass loss eventually starts to dominate and the surface velocity and its ratio to critical rotation both decrease for the rest of…”
FORMATION OF MASSIVE PRIMORDIAL STARS: INTERMITTENT UV FEEDBACK WITH EPISODIC MASS ACCRETION (2015, background): “240 M (Yoon et al. 2012), can form for such typical cases.”
Modeling the Radio Background from the First Black Holes at Cosmic Dawn: Implications for the 21 cm Absorption Amplitude (2018, background): “Meanwhile, stars with initial masses above M240 are expected to directly collapse into high-mass black holes (Yoon et al. 2012).”
A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE (2013, background): “Rotation further leads to enhanced chemical mixing (e.g. Chatzopoulos et al. 2012; Yoon et al. 2012).”
Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range −3 ≤ [Fe/H] ≤ 0 (2018, methodology): “Let us note that this value has also been adopted by Chatzopoulos & Wheeler (2012), Yoon et al. (2012), and Georgy et al. (2017) for their works on pair instability supernovae (PISNe).”
A new route towards merging massive black holes (2016, background): “Since the shortest delay time depends on the metallicitydependent stellar radii and stellar radii of massive metal-free stars are smaller than half compared to those at Z /50 (Yoon et al. 2012; Szécsi et al. 2015), even merger times shorter by orders of magnitude can be expected.”
THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, background): “…of the progenitors of long gamma-ray bursts and pair-instability supernovae (e.g., Yoon et al. 2006; Woosley & Heger 2006; Langer et al. 2007) as well as on the chemical and radiative feedback of massive stars, in particular in the early universe (e.g., Ekström et al. 2008a; Yoon et al. 2012).”