Pulsations of A stars

Balona, L. A.

doi:10.1017/s1743921304004727

Cited by 2 publications

(1 citation statement)

References 35 publications

(39 reference statements)

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“…Some λ Bootis stars show δ Sct pulsations (Paunzen 2004) and can have spectral types from late B to early F, which makes it difficult to distinguish them from δ Sct stars. In such cases, there are no clear differences between δ Sct stars and λ Bootis stars except the metal abundance (Balona 2004); λ Bootis stars show weak metal lines such as Mg II λ4481 line (Paunzen 2004).…”

Section: Detection Resultsmentioning

confidence: 99%

The TAIWAN-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. I. DETECTION OF LOW-AMPLITUDE Δ SCUTI STARS

Kim

Protopapas

Alcock

et al. 2010

The Astronomical Journal

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We analyzed data accumulated during 2005 and 2006 by the Taiwan-American Occultation Survey (TAOS) in order to detect short-period variable stars (periods of < ∼ 1 hour) such as δ Scuti. TAOS is designed for the detection of stellar occultation by small-size Kuiper Belt Objects (KBOs) and is operating four 50cm telescopes at an effective cadence of 5Hz. The four telescopes simultaneously monitor the same patch of the sky in order to reduce false positives. To detect short-period variables, we used the Fast Fourier Transform algorithm (FFT) inasmuch as the data points in TAOS light-curves are evenly spaced. Using FFT, we found 41 short-period variables with amplitudes smaller than a few hundredths of a magnitude and periods of about an hour, which suggest that they are low-amplitude δ Scuti stars (LADS). The light-curves of TAOS δ Scuti stars are accessible online at the Time Series Center website (http://timemachine.iic.harvard.edu). a Combination of TAOS field ID and TAOS star ID. b We doubled amplitudes derived by PERIOD04. c SNR of frequencies derived using PERIOD04. dThe number of identifications / the number of zipper runs. Note that we did not count zipper runs observed by only one telescope. e The B8 star found to be an A5 star as explained in the text.f The G5 star found to be an F0 star as explained in the text.

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Section: Detection Resultsmentioning

confidence: 99%

The TAIWAN-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. I. DETECTION OF LOW-AMPLITUDE Δ SCUTI STARS

Kim

Protopapas

Alcock

et al. 2010

The Astronomical Journal

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Earthshine and Asteroseismology Telescope (East) Network

2006

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Several automated optical telescopes have been setup at appropriate longitudes around the globe to study earthshine variations and asteroseismology. The first telescope has been setup at Teide Observatory, Tenerife, Spain in October 2004. The intensity of earthshine relates to the average of Earth's albedo, and in turn relates to the global temperature of the Earth. A global network is necessary because each site can measure the earthshine reflected from only a part of the Earth. The network will also be used for asteroseismology study. It can measure photometric variations of pulsating stars. The long-term and continuous measurements allow the accurate determination of mode frequencies of stellar pulsations, which provides information on the properties of stellar interior.

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Pulsations of A stars

Cited by 2 publications

References 35 publications

The TAIWAN-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. I. DETECTION OF LOW-AMPLITUDE Δ SCUTI STARS

The TAIWAN-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. I. DETECTION OF LOW-AMPLITUDE Δ SCUTI STARS

Earthshine and Asteroseismology Telescope (East) Network

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