Near IR-Photometry of Semiregular Variables

Kerschbaum, F.; Hron, J.

doi:10.1007/978-94-011-2088-3_125

Cited by 58 publications

(92 citation statements)

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“…Fig. 5 of Kerschbaum & Hron (1992) plots the semiregulars in a period versus V ‐[12] diagram: all of the stars in the current study lie beyond the blue limit of their plot. Fig.…”

Section: Evolutionary Status Of the Starsmentioning

confidence: 86%

“…Kerschbaum & Hron (1992) point out that no blue SRV shows evidence for carbon or s‐process enrichment. This, together with their modest luminosities and high temperatures, suggests that these stars are either on the early AGB, or near the end of their RGB sojourn.…”

Section: Evolutionary Status Of the Starsmentioning

confidence: 94%

“…The traditional classification of the semiregular variables was summarized briefly in Section 1. It has been extensively discussed and refined in a number of papers by Kerschbaum and co‐workers (see Kerschbaum & Hron 1996, which contains references to earlier work). The authors find that the classification SRA is essentially redundant, while the SRB stars can be separated into two distinct groups: the ‘red SRV’ stars have temperatures and mass‐loss rates similar to those of Miras, but periods which are typically a factor of 2 shorter.…”

Section: Evolutionary Status Of the Starsmentioning

confidence: 99%

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Rapidly oscillating M giant stars?

Koen

Laney

2000

Monthly Notices of the Royal Astronomical Society

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The Hipparcos mission discovered a few dozen M giant stars with periods P shorter than 10 d. Similar stars may be found in other large data bases of new variables (e.g., OGLE). The three possible sources of the magnitude variations – pulsation, starspots and ellipsoidal deformation – are discussed in general terms. The parallaxes and V−I colour indices are used to calculate radii and temperatures for all M giant variables with P<100 d. Masses are estimated from the positions of the stars in a Hertzsprung–Russell (HR) diagram, using evolutionary tracks. Using these data, it is shown that starspots can be ruled out as a variability mechanism in almost all cases, and ellipsoidal variations in about half of the stars. Pulsation in very high‐overtone modes appears to be the only viable explanation for the stars with P<10 d. Many of the stars may be multiperiodic. IRAS data are used to deduce information about reddening and circumstellar dust. The apparently low level of mass‐loss, as well as the kinematics and the spatial distribution of the stars, indicates that they are from a relatively young (i.e., thin disc) giant star population.

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“…Fig. 5 of Kerschbaum & Hron (1992) plots the semiregulars in a period versus V ‐[12] diagram: all of the stars in the current study lie beyond the blue limit of their plot. Fig.…”

Section: Evolutionary Status Of the Starsmentioning

confidence: 86%

Section: Evolutionary Status Of the Starsmentioning

confidence: 94%

Section: Evolutionary Status Of the Starsmentioning

confidence: 99%

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Rapidly oscillating M giant stars?

Koen

Laney

2000

Monthly Notices of the Royal Astronomical Society

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“…However, this ratio is of course very sensitive to the classification of SRVs (see above). For the Galactic disk, Kerschbaum & Hron (1992) found equal number densities for Miras and semiregular variables. However, they note that their sample of semiregular variables is probably not complete due to the difficulties in detecting small amplitude variables.…”

Section: Number Densitiesmentioning

confidence: 99%

“…The artificial nature of this division has been criticized already e.g. by Kerschbaum (1993). The third group of variables are the irregular variables.…”

Section: Classification Of the Variablesmentioning

confidence: 99%

AGAPEROS: Searching for variable stars in the LMC Bar

Lebzelter¹,

Schultheis

Melchior

2002

A&A

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Abstract. We analysed the light curves of a large sample of long period variables in the LMC from the AGAPEROS catalogue. The (non)regularity of the light change is discussed in detail showing that the majority of the light curves cannot be described properly by a single period. We show that semiregular and small amplitude variability do not necessarily correlate as has been assumed in several previous studies. Using near-infrared data from the DENIS survey we correlate the light change with colours and luminosities of the objects. These results are used to compare long period variables in the LMC with LPVs in the Galactic Bulge and in the solar neighborhood.

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ISOGAL Survey of Baade’s Windows

Glass

Alves

2000

ISO Surveys of a Dusty Universe

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The Baade's Windows of low obscuration towards the inner parts of the Galactic bulge represent ideal places in which to develop an understanding of the ISOGAL colour-magnitude diagrams. Unlike the case for the solar neighbourhood, their contents are at a uniform distance from the Sun, affected only by the finite thickness of the Bulge.The objects detected in the ISOGAL survey are found to be late-type M-giants at the red giant tip or on the Asymptotic Giant Branch (AGB). The ISOGAL colour-magnitude diagrams show that mass-loss starts at about M4 and increases towards later types. Many non-Miras have mass-loss rates similar to shorter-period Miras.The visible counterparts of the ISOGAL sources have been identified in the database of the MACHO gravitational lensing survey. A first report of this work is included here. It is found that nearly all the ISOGAL sources are semi-regular variables (SRVs), which are many times more numerous than Miras. Their stellar luminosities increase with period. Based on a simple interpretation of the photometry, mass-loss rates from about 10 −9 M⊙ yr −1 to 10 −7 M⊙ yr −1 are found for SRVs with periods in excess of ∼60 days.

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Near IR-Photometry of Semiregular Variables

Cited by 58 publications

References 0 publications

Rapidly oscillating M giant stars?

Rapidly oscillating M giant stars?

AGAPEROS: Searching for variable stars in the LMC Bar

ISOGAL Survey of Baade’s Windows

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