AGB variables and the Mira period–luminosity relation

By P. Whitelock, M. Feast, F. V. Leeuwen. 2008

212 citations recorded by the source corpus.

Published data for large-amplitude asymptotic giant branch variables in the Large Magellanic Cloud (LMC) are re-analysed to establish the constants for an infrared (K) period-luminosity relation of the form M K = ρ[logP - 2.38] + ρ. A slope of p = -3.51 + 0.20 and a zero-point of δ = -7.15 ± 0.06 are found for oxygen-rich Miras (if a distance modulus of 18.39 + 0.05 is used for the LMC). Assuming this slope is applicable to Galactic Miras we discuss the zero-point for these stars using the revised Hipparcos parallaxes together with published very long baseline interferometry (VLBI) parallaxes for OH masers and Miras in globular clusters. These result in a mean zero-point of δ = -7.25 ± 0.07 for O-rich Galactic Miras. The zero-point for Miras in the Galactic bulge is not significantly different from this value. Carbon-rich stars are also discussed and provide results that are consistent with the above numbers, but with higher uncertainties. Within the uncertainties there is no evidence for a significant difference between the period-luminosity relation zero-points for systems with different metallicity.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2b52a34af4fc853baee1375ac264709b9d256a83

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In Astronomy and Astrophysics

Citations in the corpus

Hubble Space Telescope Observations of Mira Variables in the SN Ia Host NGC 1559: An Alternative Candle to Measure the Hubble Constant (2019, unknown): “Whitelock et al. (2008) showed using Hipparcos parallaxes that the PLR for Galactic Miras is consistent with that in the LMC. Individual parallaxes in the Milky Way are more difficult to measure than for most stars because the angular sizes of Miras are larger than their parallaxes (their physical…”
The ASAS-SN catalogue of variable stars I: The Serendipitous Survey (2018, background): “…in the V-band) pulsations and periods P > 100 d. Mira variables can be further classified into sub-types based on the shapes of their light curves (Vardya 1988; Ludendorff 1928), and have also been found to follow a period-luminosity relation- MNRAS 000, 1–21 (2018) ship (Whitelock et al. 2008).”
A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants (Corrigendum) (2011, methodology): “A generic Galactic P-K relation valid for both oxygen- and carbon-rich (Mira) variables was established by e.g. Whitelock et al. (2000, 2008): MK = −3.51[log P−2.38]−7.25.”
STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, methodology): “Cristallo et al. (2015) calculate the pulsation period using a Mk − logP relation (e.g., Whitelock et al. 2008), which requires calculation of Mk first from stellar variables.”