Evolution of Very Massive Population III Stars with Mass Accretion from Pre-Main Sequence to Collapse TeX Export

@article{citeulike:4110921, abstract = {We calculate the evolution of zero-metallicity Population III (Pop III) stars whose mass grows from the initial mass of \$\sim 1M\_{\odot}\$ by accreting the surrounding gases. Our calculations cover a whole evolutionary stages from the pre-main sequence, via various nuclear burning stages, through the final core collapse or pair-creation instability phases. We adopt the following stellar mass-dependent accretion rates which are derived from cosmological simulations of early structure formation based on the low mass dark matter halos at redshifts \$z \sim 20\$: (1) the accretion rates for the first generation (Pop III.1) stars and (2) the rates for zero-metallicity but the second generation (Pop III.2) stars which are affected by radiation from the Pop III.1 stars. For comparison, we also study the evolution with the mass-dependent accretion rates which are affected by radiatibe feedback. We show that the final mass of Pop III.1 stars can be as large as \$\sim 1000M\_{\odot}\$, beyond the mass range (\$140 - 300M\_{\odot}\$) for the pair-instability supernovae. Such massive stars undergo core-collapse to form intermediate-mass black holes, which may be the seeds for merger trees to supermassive black holes. On the other hand, Pop III.2 stars become less massive (\$\lsim 40 - 60M\_{\odot}\$), being in the mass range of ordinary iron core-collapse stars. Such stars explode and eject heavy elements to contribute to chemical enrichment of the early universe as observed in the abundance patterns of extremely metal-poor stars in the Galactic halo.}, archivePrefix = {arXiv}, author = {Ohkubo, Takuya and Nomoto, Ken\&\#x27;ichi and Umeda, Hideyuki and Yoshida, Naoki and Tsuruta, Sachiko}, citeulike-article-id = {4110921}, citeulike-linkout-0 = {http://arxiv.org/abs/0902.4573}, citeulike-linkout-1 = {http://arxiv.org/pdf/0902.4573}, day = {26}, eprint = {0902.4573}, keywords = {evolution, firststars, formation, model, stellar}, month = {Feb}, posted-at = {2009-02-27 14:26:51}, priority = {2}, title = {Evolution of Very Massive Population III Stars with Mass Accretion from Pre-Main Sequence to Collapse}, url = {http://arxiv.org/abs/0902.4573}, year = {2009} }

TY - JOUR ID - citeulike:4110921 L3 - citeulike-article-id:4110921 N2 - We calculate the evolution of zero-metallicity Population III (Pop III) stars whose mass grows from the initial mass of $\sim 1M_{\odot}$ by accreting the surrounding gases. Our calculations cover a whole evolutionary stages from the pre-main sequence, via various nuclear burning stages, through the final core collapse or pair-creation instability phases. We adopt the following stellar mass-dependent accretion rates which are derived from cosmological simulations of early structure formation based on the low mass dark matter halos at redshifts $z \sim 20$: (1) the accretion rates for the first generation (Pop III.1) stars and (2) the rates for zero-metallicity but the second generation (Pop III.2) stars which are affected by radiation from the Pop III.1 stars. For comparison, we also study the evolution with the mass-dependent accretion rates which are affected by radiatibe feedback. We show that the final mass of Pop III.1 stars can be as large as $\sim 1000M_{\odot}$, beyond the mass range ($140 - 300M_{\odot}$) for the pair-instability supernovae. Such massive stars undergo core-collapse to form intermediate-mass black holes, which may be the seeds for merger trees to supermassive black holes. On the other hand, Pop III.2 stars become less massive ($\lsim 40 - 60M_{\odot}$), being in the mass range of ordinary iron core-collapse stars. Such stars explode and eject heavy elements to contribute to chemical enrichment of the early universe as observed in the abundance patterns of extremely metal-poor stars in the Galactic halo. TI - Evolution of Very Massive Population III Stars with Mass Accretion from Pre-Main Sequence to Collapse KW - evolution KW - firststars KW - formation KW - model KW - stellar AU - Ohkubo, Takuya AU - Nomoto, Ken'ichi AU - Umeda, Hideyuki AU - Yoshida, Naoki AU - Tsuruta, Sachiko PY - 2009/Feb/26/ UR - http://arxiv.org/abs/0902.4573 ER -