The ‘Berlin’ Nefertiti Bust:

Breger, Claudia

doi:10.2307/j.ctt1x76fk5.18

Cited by 9 publications

(8 citation statements)

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“…The variability of EP Cnc had been discovered by Martin & Hube (1989) with an estimate of a 5.46 cd −1 frequency. The multisite campaign by the Delta Scuti Network determined three frequencies (Breger et al 1994), which were identical to the three modes with the highest amplitudes in the present data sets.…”

Section: Ep Cnc (= Hd 73819 = Kw 348)supporting

confidence: 67%

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

et al. 2012

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The Praesepe cluster contains a number of δ Sct and γ Dor pulsators. Asteroseismology of cluster stars is simplified by the common distance, age and stellar abundances. Since asteroseismology requires a large number of known frequencies, the small pulsation amplitudes of these stars require space satellite campaigns. The present study utilizes photometric MOST satellite measurements in order to determine the pulsation frequencies of two evolved (EP Cnc, BT Cnc) and two main-sequence (BS Cnc, HD 73872) δ Sct stars in the Praesepe cluster. The frequency analysis of the 2008 and 2009 data detected up to 34 frequencies per star with most amplitudes in the submillimag range. In BS Cnc, two modes showed strong amplitude variability between 2008 and 2009. The frequencies ranged from 0.76 to 41.7 cd −1 . After considering the different evolutionary states and mean stellar densities of these four stars, the differences and large ranges in frequency remain.

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Section: Ep Cnc (= Hd 73819 = Kw 348)supporting

confidence: 67%

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

et al. 2012

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“…They were mainly concerned with the understanding of their pulsational and physical properties. Rodríguez et al (1996) investigated the nature of the large amplitude modes, concluding that they are radial; Garrido & Rodríguez (1996) refined this conclusion, finding possible nonradial terms having very small amplitudes in SX Phe and DY Peg. Breger & Pamyatnykh (1998) found evidence of period changes in a number of HADS, but it was not possible to relate them with stellar evolution; hence, their nature is still unclear.…”

Section: Introductionmentioning

confidence: 98%

“…Rodríguez et al (1996) investigated the nature of the large amplitude modes, concluding that they are radial; Garrido & Rodríguez (1996) refined this conclusion, finding possible nonradial terms having very small amplitudes in SX Phe and DY Peg. Breger & Pamyatnykh (1998) found evidence of period changes in a number of HADS, but it was not possible to relate them with stellar evolution; hence, their nature is still unclear. Antonello et al (1986) and Poretti et al (1990) proposed a synthetic description of the HADS light curves, trying to obtain their quantitative classification.…”

Section: Introductionmentioning

confidence: 98%

CCD Photometry of the High‐Amplitude δ Scuti Stars V798 Cygni and V831 Tauri

Musazzi¹,

Poretti²,

Covino

et al. 1998

PUBL ASTRON SOC PAC

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New CCD measurements on the two high-amplitude δ Sct stars V798 Cyg and V831 Tau were carried out. The double-mode pulsation of V798 Cyg is demonstrated beyond any doubt. The f 1 /f 2 ratio of 0.800 is confirmed to be related to the unusual shape of the f 1 light curve. The properties of the Fourier parameters were revisited also by considering the new light curve of V831 Tau.In particular, the classical double-mode pulsators cannot fill the gap in the R 21 distribution. Two new variable stars were discovered in the field of V798 Cyg.

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“…The procedure is similar to that presented in e.g. Breger et al (1994): pre‐whitening of simultaneous frequencies at each step until the S/N ratio decreases below 4. The last panel of Fig.…”

Section: Photometric Variabilitymentioning

confidence: 99%

The pre-main-sequence star HD 34282: a very short-period δ Scuti-type pulsator

Amado¹,

Moya²,

Suárez³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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HD 34282 has been found to pulsate during a systematic search for short‐term photometric variability in Herbig Ae/Be stars with the goal of determining the position and size of the pre‐main‐sequence instability strip. Simultaneous Strömgren photometry is used in the frequency analysis, yielding two frequencies with values of ν1= 79.5 and ν2= 71.3 cycle d−1. The light curve with the largest amplitude is that of the u band. This behaviour, which is not common for δ Scuti stars, is explained as pulsation in a high radial order in stars near the blue edge of the instability strip. The main period, with a value of 18.12 min, represents the shortest period observed so far for a δ Scuti‐type pulsator. A seismic modelling, including instability predictions and rotation effects, has been attempted. It is found that both main‐sequence and pre‐main‐sequence models predict modes in the range of 56 to 82 cycle d−1 (between 648 and 949 μHz), corresponding to oscillations of radial order n from 6 to 8. The highest of the observed frequencies only becomes unstable for models of low metallicity, in agreement with results from spectroscopic measurements.

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The ‘Berlin’ Nefertiti Bust:

Cited by 9 publications

References 0 publications

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

CCD Photometry of the High‐Amplitude δ Scuti Stars V798 Cygni and V831 Tauri

The pre-main-sequence star HD 34282: a very short-period δ Scuti-type pulsator

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