The influence of binaries on stellar population studies

By D. Vanbeveren. 2001

151 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ff68dc5e3ef346d7f4f6ed8fa7ca7bd0393737be

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Citations in the corpus

The Progenitor Stars of Gamma-Ray Bursts (2005, background): “Woosley et al. (2002) assumed that the same scaling law holds for WR stars (Vanbeveren 2001) and blue and red supergiants as well.”
How Massive Single Stars End Their Life (2002, background): “Woosley et al. (2002) assumed that the same scaling law holds for Wolf-Rayet stars (Vanbeveren 2001) and blue and red supergiants as well.”
Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars (2001, background): “Recently Primas et al. (2000) have suggested that [Zn/Fe] increases toward smaller metallicity as seen in Figure 1, and Blake et al. (2001) has one with [Zn/Fe] ≃ 0.6 at [Fe/H] = −3.3 (see Ryan 2001).”
Compact Object Modeling with the StarTrack Population Synthesis Code (2005, background): “The X-ray emission in HMXBs is believed to arise fromwind accretion onto the compact object; however, it was also suggested that some systems may be in an atmospheric RLOF phase (e.g., Kaper 2001).”
Reconstructing the evolution of white dwarf binaries: further evidence for an alternative algorithm for the outcome of the common-envelope phase in close binaries (2004, unknown): “ar X iv :a st ro -p h/ 04 10 30 1v 1 1 2 O Key words: stars: evolution – white dwarfs – binaries: close”
Long γ-Ray Bursts and Type Ic Core-Collapse Supernovae Have Similar Locations in Hosts (2007, background): “Residual SN Light From representative light curves (Cappellaro & Turatto 2001), we found that absolute magnitudes decay to fainter than -5 Johnson V magnitudes within one year for SN Ia, II except IIn, and Ib/Ic.”
The Effect of Massive Binaries on Stellar Populations and Supernova Progenitors (2007, methodology): “Vanbeveren (2001) first included the scaling in a population synthesis model while Crowther et al. (2002) first suggested that the scaling should be included from observations of WR stars in the LMC and in the Galaxy.”
Realistic ionizing fluxes for young stellar populations from 0.05 to 2 Z (2002, result): “Specifically for the WN stars, we used the relationship log Ṁ = −13.60 + 1.63 log L L⊙ + 2.22 log Y which agrees well with results of line-blanketed analyses (Crowther 2001).”
The progenitors of core-collapse supernovae (2004, background): “If we make observations of fields containin g prospective SN progenitors we shall observe that between 9-17% of all SN progenitors will undergo second dredge-up before SN, with overshooting the percentage is 10-20% with the IMF of Kroupa, Tout and Gilmore (1993). The exact values depend on the range”
Intermediate and extreme mass-ratio inspirals—astrophysics, science applications and detection using LISA (2007, methodology): “, the dominant three- and four-body processes), which may be crucial in the evolution of globular clusters, has been included in various MC codes through the use of approximate analytical cross-sections [127, 269, 293].”