EVOLUTION OF MASSIVE STARS WITH PULSATION-DRIVEN SUPERWINDS DURING THE RED SUPERGIANT PHASE

By Sung-Chul Yoon, Matteo Cantiello. 2010

144 citations recorded by the source corpus.

Pulsations driven by partial ionization of hydrogen in the envelope are often considered important for driving winds from red supergiants (RSGs). In particular, it has been suggested by some authors that the pulsation growth rate in an RSG can be high enough to trigger an unusually strong wind (or a superwind), when the luminosity-to-mass ratio becomes sufficiently large. Using both hydrostatic and hydrodynamic stellar evolution models with initial masses ranging from 15 to 40 M☉, we investigate (1) how the pulsation growth rate depends on the global parameters of supergiant stars and (2) what would be the consequences of a pulsation-driven superwind, if it occurred, for the late stages of massive star evolution. We suggest that such a superwind history would be marked by a runaway increase, followed by a sudden decrease, of the wind's mass-loss rate. The impact on the late evolution of massive stars would be substantial, with stars losing a huge fraction of their H-envelope even with a significantly lower initial mass than previously predicted. This might explain the observed lack of Type II-P supernova (SN) progenitors having initial mass higher than about 17 M☉. We also discuss possible implications for a subset of Type IIn SNe.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a4256c5cbde993d9b2b77dca6778bcea130ba255

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. Stan Woosley
4. J. Fuller
5. A. Piro
6. C. Conroy
7. G. Meynet
8. S. Valenti

In Instrumentation

1. S. Smartt
2. N. Smith
3. C. Conroy
4. G. Meynet
5. R. Hirschi
6. J. Fuller
7. Benjamin D. Johnson
8. Aaron Dotter

Citations in the corpus

• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “Eruptive episodic mass loss episodes and/or binaries are likely to play a role (e.g., Smith & Owocki 2006; Yoon & Cantiello 2010; Sana et al. 2012), but neither phenomenon can be realistically captured in a simple recipe for implementation in a 1D stellar evolution code.”
• Observed Fractions of Core-Collapse Supernova Types and Initial Masses of their Single and Binary Progenitor Stars (2010, background): “The full range for SNe IIn (34–150 M ) encompasses the most luminous RSG that may be responsible for the fainter SNe IIn (Smith et al. 2009a; see also Yoon & Cantiello 2010), intermediate cases of SNe D ow nloaded from https://academ ic.oup.com /m nras/article-abstract/412/3/1522/1049969 by guest…”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “Some models predict that this very strong mass-loss phase is short-lived, and enhanced before core collapse caused by increasingly violent pulsations during C burning due to a high L/M ratio (Arnett & Meakin 2011, Heger et al. 1997, Yoon & Cantiello 2010).”
• Supernovae from red supergiants with extensive mass loss (2010, methodology): “Mass loss due to the pulsations driven by partial ionization of hydrogen in the envelope of RSGs (e.g., Yoon & Cantiello 2010; Heger et al. 1997; Li & Gong 1994) is another candidate for the missing mass-loss mechanism.”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “As discussed by Yoon & Cantiello (2010) the occurrence of RSG pulsations can impact stellar mass-loss rates and modify the evolution of massive stars above a certain mass.”
• Carnegie Supernova Project: Observations of Type IIn supernovae ⋆ (2013, background): “…of view, steady, line-driven winds are the only mass-loss mechanism that is reasonably understood (but see Smith et al. 2011, and reference therein), whereas the physics behind episodic and eruptivemass loss behavior is still in its infancy (see e.g. Smith & Owocki 2006; Yoon & Cantiello 2010).”
• The great escape: how exoplanets and smaller bodies desert dying stars (2011, background): “However, mass could be lost through superwinds at a great rate of 10−4 M yr−1 (Dessart et al. 2010; Yoon & Cantiello 2010), which might offset the stabilizing effect of the large magnitude of the progenitor mass.”
• Type II-Plateau supernova radiation: dependences on progenitor and explosion properties (2013, background): “Phases of intense mass loss in RSGs may be associated with a surface phenomenon, e.g., pulsations or some other mass loss mechanism (Yoon & Cantiello 2010).”
• Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, background): “This strong mass loss could be caused by some physical processes originatingin the envelope of the RSGs, while in the binary channel it could be caused by a RLOF process occurring in a close-binary system.”
• Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, background): “It may also be that the most massive stars evolve away from the RSG phase and end their lifetime in a bluer portion of the Hertzsprung-Russell (HR) diagram (Vanbeveren et al. 1998; Salasnich et al. 1999; Yoon & Cantiello 2010; Georgy et al. 2012; Georgy 2012; Meynet et al. 2013).”
• Pre-supernova outbursts via wave heating in massive stars – I. Red supergiants (2017, background): “Heger et al. (1997) and Yoon & Cantiello (2010) show that envelope pulsational growth rates increase after core helium depletion, potentially driving a superwind during the last tens of thousands of years of a star’s life, although this theory cannot explain very high (>10−3 M yr−1) mass-loss rates…”
• Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium (2012, background): “…of RSGs is suggested by many authors (e.g. van Loon et al. 2005; Vanbeveren, Van Bever & Belkus 2007; Smith, Hinkle & Ryde 2009; Boyer et al. 2010; Yoon & Cantiello 2010; Moriya et al. 2011; Georgy 2012) and it is still possible that very massive RSGs lose ∼10 M just before their explosions due…”
• The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, result): “Current single-star models predict too many Type II SNe; however, recent studies have indicated that the mass-loss rates of RSGs remain a large source of uncertainty (Yoon & Cantiello 2010; Georgy 2012).”
• Measuring the Progenitor Masses and Dense Circumstellar Material of Type II Supernovae (2017, background): “There have been a number of theoretical studies on how to generate pre-explosion outbursts: Yoon & Cantiello (2010), Arnett & Meakin (2011), Quataert & Shiode (2012), Shiode & Quataert (2014), Smith & Arnett (2014), Moriya & Langer (2015), Woosley & Heger (2015), and Quataert et al. (2016), and…”