Radiative feedback on supermassive star formation: the massive end of the Population III initial mass function

Toyouchi, Daisuke; Inayoshi, Kohei; Li, Wenxiu; Haiman, Zoltán; Kuiper, Rolf

doi:10.48550/arxiv.2206.14459

Cited by 3 publications

(3 citation statements)

References 107 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Ultimately, the discovery of SMSs via a GRSN will depend not only on the number density of SMSs, but also the initial mass function. This 'SMS IMF' has been estimated for atomic cooling halos (Toyouchi et al 2022), but not yet for other formation scenarios. We note that the recent discovery of SMS formation via cold turbulent flows produces SMSs with masses the same order of magnitude as the GRSN mass range (Latif et al 2022).…”

Section: Discussionmentioning

confidence: 88%

Pulsations of primordial supermassive stars induced by a general relativistic instability; visible to JWST at z$>$12

Nagele¹,

Umeda²,

Takahashi³

et al. 2022

Preprint

View full text Add to dashboard Cite

The origin of high-redshift quasars and their supermassive black hole engines is unclear. One promising solution is the collapse of a primordial supermassive star. Observational confirmation of this scenario may be difficult, but a general relativistic instability supernova provides one avenue for such. Previous studies have found that a general relativistic instability supernova has a potentially decades-long plateau phase visible to JWST at high redshift. In this work, we examine stars with mass just below the general relativistic instability supernova mass range. These stars pulsate, ejecting a portion of their envelopes. They then contract quasi-statically back to an equilibrium temperature, at which point they again become unstable and pulsate once more. Because each pulse consumes a small amount of the available nuclear fuel, there exists the possibility of multiple pulsations. We present simulations of the contracting phase, the pulsation, and the light-curve phase. We find that the lower mass pulsating models are even brighter than the higher mass supernovae because the pulsations occur in the late helium burning phase when the stars have extremely large radii. The fact that the pulsations are more luminous and occur in a wider mass range than the supernovae bodes well for observation.

show abstract

Section: Discussionmentioning

confidence: 88%

Pulsations of primordial supermassive stars induced by a general relativistic instability; visible to JWST at z$>$12

Nagele¹,

Umeda²,

Takahashi³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…We have no ability to estimate the initial mass function of these objects and thus no ability to estimate 𝑓 . However, it is reasonable to assume that the mass function decreases for increasing mass, as does an estimate of the mass function of supermassive stars (Toyouchi et al 2022). If this is the case, then 𝑓 will depend heavily on the behavior of the protostars less massive than those considered in this paper (Fig.…”

Section: Of O'leary Et Al (2021)mentioning

confidence: 94%

Light-curves and nucleosynthesis of CNO-rp driven general relativistic instability supernovae in metal enriched supermassive protostars

Nagele¹,

Umeda²,

Takahashi³

2023

Preprint

View full text Add to dashboard Cite

The assembly of supermassive black holes poses a challenge primarily because of observed quasars at high redshift, but additionally because of the current lack of observations of intermediate mass black holes. One plausible scenario for creating supermassive black holes is direct collapse triggered by the merger of two gas rich galaxies. This scenario allows the creation of supermassive stars with up to solar metallicity, where the enhanced metallicity is enabled by extremely rapid accretion. We investigate the behavior of metal enriched supermassive protostars which collapse due to the general relativistic radial instability. These stars are rich in both hydrogen and metals and thus may explode due to the CNO cycle (carbon-nitrogen-oxygen) and the rp process (rapid proton capture). We perform a suite of 1D general relativistic hydrodynamical simulations coupled to a 153 isotope nuclear network with the effects of neutrino cooling. We determine the mass and metallicity ranges for an explosion. We then post process using a 514 isotope network which captures the full rp process. We present nucleosynthesis and lightcurves for selected models. These events are characterized by enhanced nitrogen, suppressed light elements (8 ≥ A ≥ 14), and low mass p nuclides and they are visible to JWST and other near infrared surveys as decades-long transients. Finally, we provide an estimate for the number of currently ongoing explosions in the Universe.

show abstract

“…Several authors have studied the origin of SMBHs, based on the DC scenario (Dijkstra et al 2008;Agarwal et al 2012;Johnson et al 2013;Chon et al 2016;Valiante et al 2016;Habouzit et al 2016;Li et al 2021;Ni et al 2022;Trinca et al 2022;Spinoso et al 2022;Toyouchi et al 2022). These studies have also derived the number density nDCBH of DCBHs in a cosmological volume.…”

Section: Comparison With Other Studiesmentioning

confidence: 99%

Direct-collapse black hole formation induced by internal radiation of host halos

Chiaki¹,

Chon²,

Omukai³

et al. 2023

Preprint

View full text Add to dashboard Cite

We estimate the fraction of halos that host supermassive black holes (SMBHs) forming through the direct collapse (DC) scenario by using cosmological N -body simulations combined with a semi-analytic model for galaxy evolution. While in most of earlier studies the occurrence of the DC is limited only in chemically pristine halos, we here suppose that the DC can occur also in halos with metallicity below a threshold value Z th = 0-10 −3 Z , considering the super-competitive accretion pathway for DC black hole (DCBH) formation. In addition, we consider for the first time the effect of Lyman-Werner (LW) radiation from stars within host halos, i.e., internal radiation. We find that, with low threshold metallicities of Z th ≤ 10 −4 Z , the inclusion of internal radiation rather reduces the number density of DCBHs from 0.2-0.3 to 0.03-0.06 Mpc −3 . This is because star formation is suppressed due to self-regulation, and the LW flux emitted by neighboring halos is reduced. Only when Z th is as high as 10 −3 Z , internal radiation enhances the number density of DCBHs from 0.4 to 1 Mpc −3 , thereby decreasing the threshold halo mass above which at least one DCBH forms from 2×10 9 to 9 × 10 8 M . We also find that halos with M halo 10 11 -10 12 M can host more than one DCBH at z = 0. This indicates that the DC scenario alone can explain the observed number of SMBH-hosting galaxies.

show abstract

Radiative feedback on supermassive star formation: the massive end of the Population III initial mass function

Cited by 3 publications

References 107 publications

Pulsations of primordial supermassive stars induced by a general relativistic instability; visible to JWST at z$>$12

Pulsations of primordial supermassive stars induced by a general relativistic instability; visible to JWST at z$>$12

Light-curves and nucleosynthesis of CNO-rp driven general relativistic instability supernovae in metal enriched supermassive protostars

Direct-collapse black hole formation induced by internal radiation of host halos

Contact Info

Product

Resources

About