A study of the variability of the Delta Scuti stars

Bossi, M.; Guerrero, G.; Mantegazza, L.; Scardia, M.

doi:10.1007/bf00655996

Cited by 4 publications

(6 citation statements)

References 10 publications

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“…Periodogram and maximum likelihood power-spectrum analyses of the velocity curves give a mean period of 0?130 or a mean frequency of 7.69 day -1 . This agrees with the results given by Nishimura et al (1983), Shaw (1976), Smith (1982, and Bossi et al (1983). However, any agreement should be treated with reservation.…”

Section: Discussionsupporting

confidence: 90%

“…The star was first reported to be a variable by Wehlau, Chen, and Symonds (1966) and Danziger and Dickens (1966). Other light curves for 20 CVn have been given by Danziger and Dickens (1967), Breger (1969), Shaw (1976), Peña and Gonzalez (1981), Chun, Lee, andNha (1983), andBossi et al (1983). From the early photometric data, Valtier (1972) calculated a period of 0?…”

Section: Introductionmentioning

confidence: 94%

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Radial-velocity variations of the Delta Scuti star 20 Canum Venaticorum

Yang¹,

Walker²

1986

PASP

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Section: Discussionsupporting

confidence: 90%

Section: Introductionmentioning

confidence: 94%

Radial-velocity variations of the Delta Scuti star 20 Canum Venaticorum

Yang¹,

Walker²

1986

PASP

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“…On one night Paparó et al (1990) obtained differential photometry of HD 130173 that showed a brightening trend. As a result, they suggested that the period of 1.29 days attributed to HR 5492 by Bossi et al (1981) belongs instead to its comparison star, HD 130173. With such a period, HD 130173 may be a Doradus variable.…”

Section: Hd 130173 (=Ads 9371 A)mentioning

confidence: 99%

Spectroscopy of Early F Stars: γ Doradus Candidates and Possible Metallic Shell Stars

Fekel¹,

Warner²,

Kaye³

2003

The Astronomical Journal

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We obtained high-resolution spectroscopic observations of 34 Doradus candidates. From the redwavelength spectra, we determined spectral classes, radial velocities, and projected rotational velocities. The spectra of seven late A or early F stars show metallic lines that have composite profiles consisting of a narrow component near the center of a broad line, indicating that they may be shell stars or binaries. Several stars, including HD 152896, HD 173977, HD 175337, and HD 195068/9, show large line profile asymmetries. Two stars, HD 11443 (= Trianguli) and HD 149420, are ellipsoidal variables and not Doradus stars. The percentage of binary systems in our sample may be as high as 74%.

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“…Individual δ Scuti stars were intensively investigated. Different pulsational behaviors were reported: (i) a single sinusoidal component which did not agree with the fundamental mode (Bossi et al, 1983), (ii) a mixture of radial and non-radial modes (Bossi et al, 1982), (iii) monoperiodic pulsation in the second overtone (Pena & Gonzalez-Bedolla, 1981), (iv) pure radial pulsation in first and second overtones or fundamental and first overtone with He depletion (Cox et al, 1984) (v) mode switching (McNamara & Horan, 1984;Paparo & Kovacs, 1984), (vi) multiple close frequencies (Breger et al, 1987), (vii) an amplitude variability on a time scale of years (Breger et al, 1990), which was compared to the Blazhko effect of RR Lyrae stars and (viii) a period decrease (Breger, 1990;Guzik & Cox, 1990). The metallicity and the pulsation connection in δ Scuti stars got a new aspect.…”

Section: Results Between 1980-1990mentioning

confidence: 99%

An Observer's View on the Future of Asteroseismology

Paparó

2019

Front. Astron. Space Sci.

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Scientific research is a continuous process, and the speed of future progress can be estimated by the pace of finding explanations for previous research questions. In this observers based view of stellar pulsation and asteroseismology, we start with the earliest observations of variable stars and the techniques used to observe them. The earliest variable stars were large amplitude, radial pulsators but were followed by other classes of pulsating stars. As the field matured, we outline some cornerstones of research into pulsating star research with an emphasis on changes in observational techniques. Improvements from photographs, to photometry, CCDs, and space telescopes allowed researchers to separate out pulsating stars from other stars with light variations, recognize radial and nonradial pulsation courtesy of increased measurement precision, and then use nonradial pulsations to look inside the stars, which cannot be done any other way. We follow several highlighted problems to show that even with excellent space data, there still may not be quick theoretical explanations. As the result of technical changes, the structure of international organizations devoted to pulsating stars has changed, and an increasing number of conferences specialized to space missions or themes are held. Although there are still many unsolved problems, such as mode identification in non-asymptotic pulsating stars, the large amount of data with unprecedented precision provided by space missions (MOST, CoRoT, Kepler) and upcoming missions allow us to use asteroseismology to its full potential. However, the enormous flow of data will require new techniques to extract the science before the next missions. The future of asteroseismology will be successful if we learn from the past and improve with improved techniques, space missions, and a properly educated new generation.

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A study of the variability of the Delta Scuti stars

Cited by 4 publications

References 10 publications

Radial-velocity variations of the Delta Scuti star 20 Canum Venaticorum

Radial-velocity variations of the Delta Scuti star 20 Canum Venaticorum

Spectroscopy of Early F Stars: γ Doradus Candidates and Possible Metallic Shell Stars

An Observer's View on the Future of Asteroseismology

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