Evolution and Pulsation of Red Supergiants at Different Metallicities

Guo, J.; Li, Y.

doi:10.1086/324295

Cited by 39 publications

(47 citation statements)

References 29 publications

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“…Wasatonic et al (2005) also found dual photometric periods of 350-450 days and 6.16 yr for TV Gem (M1 Iab) and concluded that the 6.16 yr period was the fundamental mode. Only the models more massive than 18 M in Guo & Yi (2002) have fundamental and first overtone periods that have these range of values and luminosities consistent with our revised distance. However, from their analysis of brightness variations in M supergiants, Kiss et al (2006) conclude that the long secondary periods (i.e., >1000 days) are not radial pulsations in accord with Stothers & Leung (1971).…”

Section: Stellar Propertiessupporting

confidence: 78%

“…Turner et al (2006) presented an empirical period-luminosity relation for semi-regular (SRc) M supergiant variables in Per OB1 and Berkeley 87, and found that the relation was consistent with selected linear non-adiabatic pulsation models of Guo & Yi (2002). Betelgeuse shows at least two periods and both the 5.78 yr and 400 day periods are observed in radial velocity and light curves, although the radial velocities and light curves are not tightly correlated.…”

Section: Stellar Propertiesmentioning

confidence: 82%

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A NEW VLA-HIPPARCOSDISTANCE TO BETELGEUSE AND ITS IMPLICATIONS

Harper

Brown

Guinan

2008

The Astronomical Journal

108

161

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The distance to the M supergiant Betelgeuse is poorly known, with the Hipparcos parallax having a significant uncertainty. For detailed numerical studies of M supergiant atmospheres and winds, accurate distances are a prerequisite to obtaining reliable estimates for many stellar parameters. New high spatial resolution, multiwavelength, NRAO 3 Very Large Array (VLA) radio positions of Betelgeuse have been obtained and then combined with Hipparcos Catalogue Intermediate Astrometric Data to derive new astrometric solutions. These new solutions indicate a smaller parallax, and hence greater distance (197 ± 45 pc), than that given in the original Hipparcos Catalogue (131 ± 30 pc) and in the revised Hipparcos reduction. They also confirm smaller proper motions in both right ascension and declination, as found by previous radio observations. We examine the consequences of the revised astrometric solution on Betelgeuse's interaction with its local environment, on its stellar properties, and its kinematics. We find that the most likely star-formation scenario for Betelgeuse is that it is a runaway star from the Ori OB1 association and was originally a member of a high-mass multiple system within Ori OB1a.

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Section: Stellar Propertiessupporting

confidence: 78%

Section: Stellar Propertiesmentioning

confidence: 82%

A NEW VLA-HIPPARCOSDISTANCE TO BETELGEUSE AND ITS IMPLICATIONS

Harper

Brown

Guinan

2008

The Astronomical Journal

108

161

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“…Looking at the positions, for instance, α Her or α Ori, their absolute magnitudes are 1–2 mag fainter than those of the solar metallicity models. According to Guo & Li (2002), δ M bol ∼ 0.83δ log Z , which means that unphysically large metallicities (10–100 times solar) would be needed to account for the low luminosities. A possibility is that heavy circumstellar extinction in K band makes the stars fainter.…”

Section: Discussion Of the Multiperiodic Naturementioning

confidence: 99%

“…As such, they are key agents of nucleosynthesis and chemical evolution of the Galaxy, and have also long been known for their slow optical variations. This variability is usually attributed to radial pulsations (Stothers 1969; Wood, Bessell & Fox 1983; Heger et al 1997; Guo & Li 2002), although irregular variability caused by huge convection cells was also suggested from theory (Schwarzschild 1975; Antia, Chitre & Narasimha 1984) and observations (e.g. Tuthill, Haniff & Baldwin 1997).…”

Section: Introductionmentioning

confidence: 96%

Variability in red supergiant stars: pulsations, long secondary periods and convection noise

Kiss

Szabó

Bedding

2006

Monthly Notices of the Royal Astronomical Society

183

194

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We study the brightness variations of galactic red supergiant stars using long‐term visual light curves collected by the American Association of Variable Star Observers over the last century. The full sample contains 48 red semiregular or irregular variable stars, with a mean time‐span of observations of 61 yr. We determine periods and period variability from analyses of power density spectra and time–frequency distributions. We find two significant periods in 18 stars. Most of these periods fall into two distinct groups, ranging from a few hundred to a few thousand days. Theoretical models imply fundamental, first and possibly second overtone mode pulsations for the shorter periods. Periods greater than 1000 d form a parallel period–luminosity relation that is similar to the long secondary periods of the asymptotic giant branch stars. A number of individual power spectra shows a single mode resolved into multiple peaks under a Lorentzian envelope, which we interpret as evidence for stochastic oscillations, presumably caused by the interplay of convection and pulsations. We find a strong 1/f noise component in the power spectra that is remarkably similar in almost all stars of the sample. This behaviour fits the picture of irregular photometric variability caused by large convection cells, analogous to the granulation background seen in the Sun.

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“…Physical reasons for variability in red supergiants such as S Per have been discussed by many authors; see, e.g., Lovy et al (1984), Li & Gong (1994), Heger et al (1997), Bono & Panagia (2000), Guo & Li (2002), and references therein. The conclusion is that the main cause of light variability in red supergiants is variation of the effective temperature due to stellar pulsation.…”

Section: Introductionmentioning

confidence: 99%

Variability of the H₂O maser associated with the M-supergiant S Persei

Lekht

Rudnitskij²,

Mendoza-Torres

et al. 2005

A&A

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Abstract. We present the results from observing the circumstellar maser emission of the M-type supergiant S Per in the 6 16 -5 23 water-vapour line at 1.35 cm. The observations were carried out in 1981-2002 (JD = 2 444 900-2 452 480) on the RT-22 radio telescope of the Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences. The H 2 O spectra obtained represent an unprecedented long, uniform dataset on this star. We discuss the properties of the optical and maser variations of S Per, together with particulars of the available VLBI maps. The close relation between maser and optical variations favors a model in which mass-loss is episodic. Changes observed in the total H 2 O line flux follow the visual light curve with a delay of 0.01 to 0.5P, where P ≈ 800 d is the mean light cycle for S Per. The feature at V LSR = −44 km s −1 flared in July 1988, which seemed to be the response of the maser to an unusually bright optical maximum. The position of the −44-km s −1 feature on the VLBI maps coincides with the direction toward the optical stellar disc, which can be explained by amplification of enhanced stellar continuum by the H 2 O line.

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Evolution and Pulsation of Red Supergiants at Different Metallicities

Cited by 39 publications

References 29 publications

A NEW VLA-HIPPARCOSDISTANCE TO BETELGEUSE AND ITS IMPLICATIONS

A NEW VLA-HIPPARCOSDISTANCE TO BETELGEUSE AND ITS IMPLICATIONS

Variability in red supergiant stars: pulsations, long secondary periods and convection noise

Variability of the H₂O maser associated with the M-supergiant S Persei

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Evolution and Pulsation of Red Supergiants at Different Metallicities

Cited by 39 publications

References 29 publications

A NEW VLA-HIPPARCOSDISTANCE TO BETELGEUSE AND ITS IMPLICATIONS

A NEW VLA-HIPPARCOSDISTANCE TO BETELGEUSE AND ITS IMPLICATIONS

Variability in red supergiant stars: pulsations, long secondary periods and convection noise

Variability of the H2O maser associated with the M-supergiant S Persei

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Product

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Variability of the H₂O maser associated with the M-supergiant S Persei