An Empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich asymptotic giant branch stars

By J. V. Loon, M. Cioni, A. Zijlstra, C. Loup. 2005

316 citations recorded by the source corpus.

We present an empirical determination of the mass-loss rate as a function of stellar luminosity and effective tem- perature, for oxygen-rich dust-enshrouded Asymptotic Giant Branch stars and red supergiants. To this aim we obtained optical spectra of a sample of dust-enshrouded red giants in the Large Magellanic Cloud, which we complemented with spectroscopic and infrared photometric data from the literature. Two of these turned out to be hot emission-line stars, of which one is a definite B(e) star. The mass-loss rates were measured through modelling of the spectral energy distributions. We thus obtain the mass- loss rate formula log u M = −5.65 + 1.05 log(L/10 000 L� ) − 6. 3l og(Teff/3500 K), valid for dust-enshrouded red supergiants and oxygen-rich AGB stars. Despite the low metallicity of the LMC, both AGB stars and red supergiants are found at late spectral types. A comparison with galactic AGB stars and red supergiants shows excellent agreement between the mass-loss rate as predicted by our formula and that derived from the 60 µm flux density for dust-enshrouded objects, but not for optically bright objects. We discuss the possible implications of this for the mass-loss mechanism.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f1b000f2ad2b0277f83546a48dab327b29cc8dfa

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Citations in the corpus

• Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium (2012, background): “However, extensive mass loss 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…”
• Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, background): “However, Vanbeveren et al. (1998a, b) argued that the RSG rates may be significantly larger than those predicted by the De Jager et al. formalism and this has been confirmed recently by Van Loon et al. (2005).”
• Supernova remnants: the X-ray perspective (2011, unknown): “In the subsequent red supergiant (RSG) phase the mass loss rate increases to as much as Ṁ ≈ 10−4 M⊙ yr−1 (e.g. van Loon et al., 2005), which, together with a much slower wind velocity vw ∼ 10 km s−1, results in a very dense wind, with a density at radius r given by ρw(r) = Ṁ 4πr2vw , (11) a…”
• Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range −3 ≤ [Fe/H] ≤ 0 (2018, methodology): “Note that at these metallicities, no model crosses the temperature threshold (van Loon et al. 2005) to activate the mass loss due to the dust formation.”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, methodology): “Some models adopt the significantly higher empirical RSG mass-loss prescription of van Loon et al. (2005), which is intended for dust-enshrouded RSGs.”
• Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, methodology): “Their standard model assumed the mass-loss rate from van Loon et al. (2005) with a metallicity scaling √ Z/Z⊙ from Kudritzki et al. (1987), used the core 10 Their solar metallicity (Z=0.02) case was presented in Poelarends et al. (2008) whilst an overview for their entire metallicity range provided…”
• The mass-loss rates of red supergiants and the de Jager prescription (2010, methodology): “Nevertheless, one can compare the results of this prescription to the de Jager rate. van Loon et al. (2005) derived effective temperatures from spectral classifications.”
• SN 2008S: An electron-capture SN from a super-AGB progenitor? (2009, methodology): “Such high mass-loss through thermal pulses has been predicted by theory and obscured massive oxygen-rich AGB stars are certainly observed by van Loon et al. (2005) The evidence that SN 2008S was indeed a SN explosion comes from two observations.”
• EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF AGB STARS AT DIFFERENT METALLICITIES. III. INTERMEDIATE-MASS MODELS, REVISED LOW-MASS MODELS, AND THE pH-FRUITY INTERFACE (2015, methodology): “For instance, we could use the mass-loss rate proposed by van Loon et al. (2005).”
• PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, background): “The enhancement of the mass loss due to the formation of dust during the red supergiant phase has been included following the prescriptions of van Loon et al. (2005).”
• PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04 (2015, background): “As in less massive Asymptotic Giant Branch (AGB) stars, dust formation on the circumstellar envelopes could be one of the possible mechanisms responsible for this enhancement (van Loon et al. 2005).”
• A Massive Cluster of Red Supergiants at the Base of the Scutum-Crux Arm (2007, background): “As RSGs’ mass-loss rates are roughly proportional to their luminosity (van Loon et al. 2005), in Figure 10 we plot the bolometric magnitude of the stars against theirK MSX colors.”
• Spitzer SAGE Survey of the Large Magellanic Cloud. II. Evolved Stars and Infrared Color-Magnitude Diagrams (2006, background): “…massloss budget from all stellar populations when combined with existing and future mid-infrared spectroscopic observations of the asymptotic giant branch (AGB) stars and supergiants (SGs); for example, see van Loon et al. (1999, 2005), Markwick-Kemper et al. (2005), and Zijlstra et al. (2006).”
• Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, result): “In this case, the radiative mass loss is increased by a factor of three in our models with initial mass above 18 M , which matches the Ṁ determinations from van Loon et al. (2005).”
• The Galactic WC stars Stellar parameters from spectral analyses indicate a new evolutionary sequence (2012, background): “For objects covered with dust, van Loon et al. (2005) discovered mass-loss rates that are significantly higher than those of visually bright ones.”