The period–luminosity relation of red supergiants with Gaia DR2

Chatys, Filip W.; Bedding, Timothy R.; Murphy, Simon J.; Kiss, L. L.; Dobie, Dougal; Grindlay, Jonathan E.

doi:10.1093/mnras/stz1584

Cited by 40 publications

(55 citation statements)

References 63 publications

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“…For clarity, tracks with an initial mass that is intermediate between these two values have been omitted. similar agreement was found with the PLDs presented by Chatys et al (2019) for galactic and LMC red supergiants.…”

Section: Pulsation Mode Of High-mass Lpvssupporting

confidence: 91%

“…A parallel sequence shifted towards shorter periods, which is seen in our study (Fig. 19), in the paper by Ren et al (2019) and in the work by Chatys et al (2019), is likely formed by first overtone pulsators among the massive AGB stars and the supergiants.…”

Section: Pulsation Mode Of High-mass Lpvssupporting

confidence: 85%

“…In addition to the paper by Chatys et al (2019) mentioned above, Ren et al (2019) recently presented PLDs for supergiants in M31 and M33. A comparison with pulsation models allowed the latter authors to attribute the supergiants to fundamental or first overtone pulsation.…”

Section: Pulsation Mode Of High-mass Lpvsmentioning

confidence: 99%

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Period-luminosity diagram of long period variables in the Magellanic Clouds

Lebzelter

Trabucchi

Mowlavï

et al. 2019

A&A

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Context. The period-luminosity diagram (PLD) has proven to be a powerful tool for studying populations of pulsating red giants. Gaia Data Release 2 (DR2) provides a large data set including many long-period variables (LPVs) on which this tool can be applied. Aims. We investigate the location of LPVs from the Large and Small Magellanic Clouds in the PLD using various optical and infrared luminosity indicators from Gaia and 2MASS, respectively. We thereby distinguish between stars of different masses and surface chemistry.Methods. The data set taken from the Gaia DR2 catalogue of LPVs allows for a homogeneous study from low-to high-mass LPVs. These sources are divided into sub-populations of asymptotic giant branch (AGB) stars according to their mass and their O-or C-rich nature using the Gaia-2MASS diagram developed by our group. This diagram uses a Wesenheit index W BP,RP based on Wesenheit functions in the Gaia and 2MASS photometric bands. Four different luminosity indicators are used to study the period-luminosity (P-L) relations. Results. We provide the first observational evidence of a P-L relation offset for both fundamental and 1O pulsators between lowand intermediate-mass O-rich stars, in agreement with published pulsation predictions. Among the luminosity indicators explored, sequence C' is the narrowest in the P-W BP,RP diagram, and is thus to be preferred over the other PLDs for the determination of distances using LPVs. The majority of massive asymptotic giant branch (AGB) stars and red supergiants form a smooth extension of sequence C of low-and intermediate-mass AGB stars in the P-W BP,RP diagram, suggesting that they pulsate in the fundamental mode. All results are similar in the two Magellanic Clouds.

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Section: Pulsation Mode Of High-mass Lpvssupporting

confidence: 91%

Section: Pulsation Mode Of High-mass Lpvssupporting

confidence: 85%

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Period-luminosity diagram of long period variables in the Magellanic Clouds

Lebzelter

Trabucchi

Mowlavï

et al. 2019

A&A

View full text Add to dashboard Cite

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“…Kiss et al (2006) and Percy & Khatu (2014) identified periods of a few hundred to a few thousand days with varying stellar lightcurve morphology for RSGs in the AAVSO International Database. Such pulsations have also been observed occurring in RSGs within the Small and Large Magellanic Clouds (Feast et al 1980;Ita et al 2004;Szczygie l et al 2010;Yang & Jiang 2011;Yang & Jiang 2012;Yang et al 2018), M31 and M33 (Soraisam et al 2018;Ren et al 2019), M51 (Conroy et al 2018), M101 (Jurcevic et al 2000), within HST archival data of NGC 1326A, NGC 1425, and NGC 4548 (Spetsieri et al 2019), and within the GAIA DR2 RSG sample (Chatys et al 2019). These works identify these RSG pulsations Corresponding author: J.…”

Section: Introductionmentioning

confidence: 63%

A Massive Star’s Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae

Goldberg

Bildsten

Paxton

2020

ApJ

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Massive stars undergo fundamental-mode and first-overtone radial pulsations with periods of 100-1000 days as Red Supergiants (RSGs). At large amplitudes, these pulsations substantially modify the outer envelope's density structure encountered by the outgoing shock wave from the eventual core collapse of these M > 9M stars. Using Modules for Experiments in Stellar Astrophysics (MESA), we model the effects of fundamental-mode and first-overtone pulsations in the RSG envelopes, and the resulting Type IIP supernovae (SNe) using MESA+STELLA. We find that, in the case of fundamental mode pulsations, SN plateau observables such as the luminosity at day 50, L 50 , time-integrated shock energy ET , and plateau duration t p are consistent with radial scalings derived considering explosions of non-pulsating stars. Namely, most of the effect of the pulsation is consistent with the behavior expected for a star of a different size at the time of explosion. However, in the case of overtone pulsations, the Lagrangian displacement is not monotonic. Therefore, in such cases, excessively bright or faint SN emission at different times reflects the underdense or overdense structure of the emitting region near the SN photosphere.

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“…Critically, the brightness of Betelgeuse varies in a systematic way on at least two different timescales, and these periodicities were measured with good precision by Kiss et al (2006) (and later corroborated by Chatys et al 2019). The shorter occurs with a period of ∼388 days and the longer with a period of ∼5.6 yr (2050 days).…”

mentioning

confidence: 79%

Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA

Joyce

Leung

Molnár

et al. 2020

ApJ

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We conduct a rigorous examination of the nearby red supergiant Betelgeuse by drawing on the synthesis of new observational data and three different modeling techniques. Our observational results include the release of new, processed photometric measurements collected with the space-based Solar Mass Ejection Imager instrument prior to Betelgeuse's recent, unprecedented dimming event. We detect the first radial overtone in the photometric data and report a period of 185±13.5 days. Our theoretical predictions include self-consistent results from multitimescale evolutionary, oscillatory, and hydrodynamic simulations conducted with the Modules for Experiments in Stellar Astrophysics software suite. Significant outcomes of our modeling efforts include a precise prediction for the star's radius:-+ R 764 62 116 . In concert with additional constraints, this allows us to derive a new, independent distance estimate of-+ 168 15 27 pc and a parallax of p =-+ 5.95 0.85 0.58 mas, in good agreement with Hipparcos but less so with recent radio measurements. Seismic results from both perturbed hydrostatic and evolving hydrodynamic simulations constrain the period and driving mechanisms of Betelgeuse's dominant periodicities in new ways. Our analyses converge to the conclusion that Betelgeuse's ≈400 day period is the result of pulsation in the fundamental mode, driven by the κ-mechanism. Grid-based hydrodynamic modeling reveals that the behavior of the oscillating envelope is mass-dependent, and likewise suggests that the nonlinear pulsation excitation time could serve as a mass constraint. Our results place α Orionis definitively in the early core helium-burning phase of the red supergiant branch. We report a present-day mass of 16.5-19 M e-slightly lower than typical literature values.

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The period–luminosity relation of red supergiants with Gaia DR2

Cited by 40 publications

References 63 publications

Period-luminosity diagram of long period variables in the Magellanic Clouds

Period-luminosity diagram of long period variables in the Magellanic Clouds

A Massive Star’s Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae

Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA

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