Massive Stars in the Local Group: Implications for Stellar Evolution and Star Formation

By Philip Massey. 2003

251 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5a0d07e9d94d83ee1126d0bf4c267f2bab68ddaf

How researchers see this paper

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In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. G. Meynet
4. N. Langer
5. Ralf Klessen
6. Michela Mapelli
7. S. Glover
8. Mark R. Krumholz

In Instrumentation

1. S. Smartt
2. N. Smith
3. G. Meynet
4. Robert G. Izzard
5. A. Chieffi
6. M. Limongi
7. Ralf Klessen
8. J. Eldridge

Citations in the corpus

• The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “However, all the hosts are large spiral galaxies and therefore are expected to have metallicities in the range between that of the Magellanic Clouds and the Milky Way (see the discussion in Smartt et al. 2009).”
• Abundances of Metal-rich H II Regions in M51 (2004, background): “This agrees with the known trend of increasing fraction of WC relative to WN stars with abundance (Massey 2003).”
• The relation between the most-massive star and its parental star cluster mass (2009, background): “The canonical IMF is today understood to be an invariant Salpeter/Massey power-law slope (Salpeter 1955; Massey 2003) above 0.5 M⊙, being independent of the cluster density and metallicity for metallicities Z >∼ 0.002 (Massey & Hunter 1998; Sirianni et al. 2000, 2002; Parker et al. 2001; Massey…”
• The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity (2006, background): “Observationally, the relative number of RSGs andWolf-Rayet stars appear to change by a factor of >100 over 0.8 dex in metallicity (Massey 2002, 2003), in accordance with the suggestion first made by Maeder et al. (1980).”
• The stellar and sub-stellar IMF of simple and composite populations (2011, background): “In the LMC the field-star IMF is known to be steep, α3 ≈ 4.5 (Massey 2003).”
• The Adequacy of Stellar Evolution Models for the Interpretation of the Color-Magnitude Diagrams of Resolved Stellar Populations (2005, background): “Previous ARAA papers have discussed the topic of massive star evolution and populations (Chiosi & Maeder 1986, Maeder & Conti 1994, Massey 2003).”
• The Evolution of Massive Stars. I. Red Supergiants in the Magellanic Clouds (2003, background): “Massey (2002b, 2003) finds that the identical problem exists for Galactic RSGs even when adopting the effective temperature scale and luminosities of Humphreys (1978).”
• The high-mass stellar IMF in different environments (2006, unknown): “Observationally, the IMF has been constrained above a few M by Massey (2003) for populations in the Milky Way, the Large and Small Magellanic Clouds and for different densities.”
• Evidence for top-heavy stellar initial mass functions with increasing density and decreasing metallicity (2012, background): “Massey (2003) shows homogeneously estimated mass function slopes for OB associations in the MW and LMC finding all of them to be consistent with the Salpeter slope (α = 2.35).”
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit (2010, background): “…an unsolved problem of astrophysics (Zinnecker & Yorke 2007), the past decade E-mail: Paul.Crowther@shef.ac.uk has seen a shift from a belief that there is no observational upper stellar mass cut-off (e.g. Massey 2003) to the widespread acceptance of a limit close to 150 M (Figer 2005; Koen 2006).”
• The maximum stellar mass, star-cluster formation and composite stellar populations (2005, background): “Several observations find the Salpeter value (α3 = 2.35) for a large variety of conditions (Massey & Hunter 1998; Sirianni et al. 2000, 2002; Parker et al. 2001; Massey 2002, 2003; Wyse et al. 2002; Bell et al. 2003; Piskunov et al. 2004).”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “…the effects of relatively rapid rotation (Georgy et al. 2012).6 At first glance, models and observations would seem to be reasonably well aligned (Massey 2003): MWR is inferred to be about 25 M⊙ at Z⊙ (Crowther 2007), increasing to about 30 and 70 M⊙ at ZLMC and ZSMC , respectively (Massey et…”
• The Effect of Massive Binaries on Stellar Populations and Supernova Progenitors (2007, background): “The observed ratio is less certain than the BSG to RSG ratio because there is greater uncertainty in the completeness of the observations (Massey 2003).”
• Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems (2005, background): “…form for mass M > 1 M with index , i.e., dN dm ¼ Am ¼ F 1( 1)m ; ð10Þ where m is the mass in units of solar masses and the slope ¼ 2:35 for the classic form first suggested by Salpeter (1955); this slope remains valid today for a wide variety of regions (Massey 2003 and references therein).”
• Physical Properties of Wolf-Rayet Stars (2006, background): “The unique spectroscopic signature of WR stars has permitted their detection individually in Local Group galaxies (e.g. Massey & Johnson 1998; Massey 2003), collectively within knots of local star forming galaxies (e.g. Hadfield & Crowther 2006), and as significant contributors to the average…”
• Observed Fractions of Core-Collapse Supernova Types and Initial Masses of their Single and Binary Progenitor Stars (2010, background): “…with star clusters suggest a value of MWR around roughly 35–40 M for most WR stars in the Milky Way (Schild & Maeder 1984; Humphreys, Nichols & Massey 1985; Massey, Johnson & DeGioia-Eastwood 1985; Massey, DeGioia-Eastwood & Waterhouse 2001; Massey 2003; Crowther et al. 2006; Crowther 2007).”
• Double neutron stars: merger rates revisited (2017, background): “…000, 1–24 (2017) Model: C C+P NK2 Rlocal;BHBH [ Gpc−3 yr−1]: 32 [310] 695 [695] 190 [1072] trends in the form of the IMF with redshift or metallicity (Massey 2003; Bastian et al. 2010; Offner et al. 2014), apart from local deviations (e.g. top-heavy IMF found in some globular clusters, see Kroupa…”