Supernovae from Massive Stars

Limongi, Marco

doi:10.1007/978-3-319-21846-5_119

Cited by 16 publications

(14 citation statements)

References 45 publications

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“…Finally, rotation affects the evolution of a massive star in several ways (e.g. [217,76,202,203,77]). As a general rule of thumb, rotation increases the stellar luminosity.…”

Section: Stellar Winds and Stellar Evolutionmentioning

confidence: 99%

Formation channels of single and binary stellar-mass black holes

Mapelli

2021

Preprint

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These are exciting times for binary black hole (BBH) research. LIGO and Virgo detections are progressively drawing a spectacular fresco of BBH masses, spins and merger rates. In this review, we discuss the main formation channels of BBHs from stellar evolution and dynamics. Uncertainties on massive star evolution (e.g., stellar winds, rotation, overshooting and nuclear reaction rates), core-collapse supernovae and pair instability still hamper our comprehension of the mass spectrum and spin distribution of black holes (BHs), but substantial progress has been done in the field over the last few years. On top of this, the efficiency of mass transfer in a binary system and the physics of common envelope substantially affect the final BBH demography. Dynamical processes in dense stellar systems can trigger the formation of BHs in the mass gap and intermediate-mass BHs via hierarchical BH mergers and via multiple stellar collisions. Finally, we discuss the importance of reconstructing the cosmic evolution of BBHs.

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“…Finally, rotation affects the evolution of a massive star in several ways (e.g. [217,76,202,203,77]). As a general rule of thumb, rotation increases the stellar luminosity.…”

Section: Stellar Winds and Stellar Evolutionmentioning

confidence: 99%

Formation channels of single and binary stellar-mass black holes

Mapelli

2021

Preprint

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“…Evolutionary tracks predict that gravity linearly correlates with L and T eff (Limongi 2017;Bertelli et al 2009), and an estimate of the stellar gravity can be obtained as described in Appendix A.…”

Section: Luminosities Of Supergiantsmentioning

confidence: 99%

“…Stellar evolution models suggest that the upper mass limit for RSGs is 25 M ⊙ for rotating stars and 40 M ⊙ for nonrotating stars (e.g., Limongi 2017). Massive stars with luminosities from 10,000 to 400,000 L ⊙ enter this phase when their envelopes expand and their effective temperatures drop below 4500 K. Because of their intrinsically high luminosity and red colors, they can be seen at large distances and through large columns of dust, making them good tracers of galactic disk morphology and kinematics.…”

Section: Introductionmentioning

confidence: 99%

New infrared spectral indices of luminous cold stars: from early K to M-types

Messineo,

Figer,

Kudritzki

et al. 2021

Preprint

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We present infrared spectral indices (1.0-2.3 µm) of Galactic late-type giants and red supergiants (RSGs). We used existing and new spectra obtained at resolution power R=2000 with SpeX on the IRTF telescope. While a large CO equivalent width (EW), at 2.29 µm ([CO, 2.29] 45 Å) is a typical signature of RSGs later than spectral type M0, [CO] of K-type RSGs and giants are similar. In the [CO, 2.29] versus [Mg I, 1.71] diagram, RSGs of all spectral types can be distinguished from red giants, because the Mg I line weakens with increasing temperature and decreasing gravity. We find several lines that vary with luminosity, but not temperature: Si I (1.59 µm), Sr (1.033 µm), Fe+Cr+Si+CN (1.16 µm), Fe+Ti (1.185 µm), Fe+Ti (1.196 µm), Ti+Ca (1.28 µm), and Mn (1.29 µm). Good markers of CN enhancement are the Fe+Si+CN line at 1.087 µm and CN line at 1.093 µm. Using these lines, at the resolution of SpeX, it is possible to separate RSGs and giants. Contaminant O-rich Mira and S-type AGBs are recognized by strong molecular features due to water vapor features, TiO band heads, and/or ZrO absorption. Among the 42 candidate RSGs that we observed, all but one were found to be late-types. 21 have EWs consistent with those of RSGs, 16 with those of O-rich Mira AGBs, and one with an S-type AGB. These infrared results open new, unexplored, potential for searches at low-resolution of RSGs in the highly obscured innermost regions of the Milky Way.

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“…BH masses depend on the properties of their stellar progenitors (mostly their masses, chemical composition and rotation velocity e. 2012) which provides an analytic model for a neutrinodriven explosion and calculate the explosion energy, as well as the remnant mass, using numerical pre-collapse stellar models from Woosley, Heger & Weaver (2002). Another set of stellar evolution models is provided in Limongi (2017). These models differ from those in Fryer et al (2012) in two aspects.…”

Section: Astrophysical Modelsmentioning

confidence: 99%

Stochastic gravitational wave background anisotropies in the mHz band: astrophysical dependencies

Cusin

Dvorkin

Pitrou

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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We show that the anisotropies of the astrophysical stochastic gravitational wave background in the mHz band have a strong dependence on the modelling of galactic and sub-galactic physics. We explore a wide range of self-consistent astrophysical models for stellar evolution and for the distribution of orbital parameters, all calibrated such that they predict the same number of resolved mergers to fit the number of detections during LIGO/Virgo O1+O2 observations runs. We show that different physical choices for the process of black hole collapse and cut-off in the black hole mass distribution give fractional differences in the angular power spectrum of anisotropies up to 50% on all angular scales. We also point out that the astrophysical information which can be extracted from anisotropies is complementary to the isotropic background and individual mergers. These results underline the interest in the anisotropies of the stochastic gravitational wave background as a new and potentially rich field of research, at the cross-road between astrophysics and cosmology.

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Supernovae from Massive Stars

Cited by 16 publications

References 45 publications

Formation channels of single and binary stellar-mass black holes

Formation channels of single and binary stellar-mass black holes

New infrared spectral indices of luminous cold stars: from early K to M-types

Stochastic gravitational wave background anisotropies in the mHz band: astrophysical dependencies

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