Obscured asymptotic giant branch variables in the Large Magellanic Cloud and the period–luminosity relation
By P. Whitelock, M. Feast, J. V. Loon, A. Zijlstra. 2003
134 citations recorded by the source corpus.
The characteristics of oxygen-rich and carbon-rich, large amplitude (�K > 0.4 mag), asymptotic giant branch variables in the Large Magellanic Clouds are discussed, with an emphasis on those obscured by dust. Near-infrared photometry, obtained over about 8 years, is combined with published mid-infrared observations from IRAS and ISO to determine bolometric magnitudes for 42 stars. Pulsation periods of the O-rich stars are in the range 116 0.6 mag, secular or very long period variations which may be associated with changes in their mass-loss rates. We discuss and compare various methods of determining the bolometric magnitudes and show, perhaps surprisingly, that most of the very long period stars seem to follow an extrapolation of the periodluminosity relation determined for stars with shorter periods - although the details do depend on how the bolometric magnitudes are calculated. Three stars with thin shells, which are clearly more luminous than the obscured AGB stars, are undergoing hot bottom burning, while other stars with similar luminosities have yet to be investigated in sufficient detail to determine their status in this regard. We suggest that an apparent change in slope of the period luminosity relation around 400-420 days is caused by variables with luminosities brighter than the predictions of the core-mass luminosity relation, due to excess flux from hot bottom burning.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/86e79110ec50797e0e82b308dd657e3563d812fa
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In Astronomy and Astrophysics
Citations in the corpus
- AGB variables and the Mira period–luminosity relation (2008, background): “Complications do arise at periods in excess of about 400 d where some Miras in the LMC have higher luminosities, possibly as a consequence of hot bottom burning (e.g. Whitelock et al. 2003).”
- An Empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich asymptotic giant branch stars (2005, methodology): “We here present a recipe for the mass-loss rate as a function of luminosity and stellar effective temperature, Ṁ(L, Teff), for oxygen-rich AGB stars and red supergiants in the LMC, which undergo strong regular pulsations (Whitelock et al. 2003) and are enshrouded in dusty envelopes.”
- Mass loss of stars on the asymptotic giant branch (2018, background): “2) is supported by various observations, ranging from correlations of mass-loss indicators with pulsation properties (e.g., Whitelock et al. 1991, 2003; Glass et al. 2009; McDonald and Zijlstra 2016) to spatially resolved structures of dynamical atmospheres and dust formation regions (e.g., Tej et…”
- Near‐infrared photometry of carbon stars★ (2006, methodology): “This PL is distinctly different from that derived for O-rich Miras (Feast et al. 1989; Whitelock et al. 2003).”
- Hubble Space Telescope Observations of Mira Variables in the SN Ia Host NGC 1559: An Alternative Candle to Measure the Hubble Constant (2019, background): “The gray lines denote the uncertainty in the zeropoint at each point. because HBB stars typically have masses > 3M , which will be rare).”
- Luminosities and mass-loss rates of SMC and LMC AGB stars and red supergiants (2009, methodology): “WBF reported a spectral type of MS and a period of 366 days for HV 11366, and based on this period Sloan et al. (2008) assumed it was a member of the SMC.”