Rotation of stars in NGC 6134

Rasmussen, Michael Bo; Bruntt, H.; Frandsen, S.; Paunzen, E.; Maitzen, H. M.

doi:10.1051/0004-6361:20020713

Cited by 9 publications

(10 citation statements)

References 15 publications

(31 reference statements)

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“…A number of authors (see, e.g., Rasmussen et al [2002] and references therein) have tried to understand the excitation mechanism in Scuti stars by searching for systematic differences between variable and nonvariable stars. Our result suggests that such searches may be complicated by the fact that ''nonvariable'' stars may in fact be variable at levels undetectable from the ground.…”

Section: Discussionmentioning

confidence: 99%

Altair: The Brightest δ Scuti Star

Buzasi

Bruntt

Bedding

et al. 2005

ApJ

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We present an analysis of observations of the bright star Altair ( Aql) obtained using the star camera on the Wide Field Infrared Explorer (WIRE ) satellite. Although Altair lies within the Scuti instability strip, previous observations have not revealed the presence of oscillations. However, the WIRE observations show Altair to be a low-amplitude (Ám < 1 parts per thousand [ ppt]) Scuti star with at least seven modes present.

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Section: Discussionmentioning

confidence: 99%

Altair: The Brightest δ Scuti Star

Buzasi

Bruntt

Bedding

et al. 2005

ApJ

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“…Rasmussen et al (2002) and Bikmaev et al (2002). In the later paper we study two A-type stars and both have low v sin i (9 and 21 km s −1 ).…”

Section: Reliability Of Vwamentioning

confidence: 97%

“…We have already used vwa for the analysis of several other stars which will be published soon (Bikmaev et al 2002;Rasmussen et al 2002). In the paper by Bikmaev et al we have analysed two A-type stars, which have low v sin i.…”

Section: Conclusion and Future Prospectsmentioning

confidence: 99%

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Bruntt

Catala

Garrido

et al. 2002

A&A

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Abstract.One of the goals of the ground-based support program for the COROT and MONS/Rømer satellite missions is to select and characterise suitable target stars for the part of the missions dedicated to asteroseismology. While the global atmospheric parameters may be determined with good accuracy from the Strömgren indices, careful abundance analysis must be made for the proposed main targets. This is a time consuming process considering the long list of primary and secondary targets. We have therefore developed new software called vwa for this task. The vwa automatically selects the least blended lines from the atomic line database vald, and consequently adjusts the abundance in order to find the best match between the calculated and observed spectra. The variability of HD 49434 was discovered as part of COROT ground-based support observations. Here we present a detailed abundance analysis of HD 49434 using vwa. For most elements we find abundances somewhat below the Solar values, in particular we find [Fe/H] = −0.13 ± 0.14. We also present the results from the study of the variability that is seen in spectroscopic and photometric time series observations. From the characteristics of the variation seen in photometry and in the line profiles we propose that HD 49434 is a variable star of the γ Doradus type.

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“…Stars at the MSTO with significant rotation would appear redder according to the MIST isochrones (Choi et al 2016), and even though there is some evidence that indeed the redder stars at NGC 419 MSTO rotate faster (Kamann et al 2018), it is unclear whether δ Sct pulsations are favoured by rotation (e.g. Solano & Fernley 1997;Rasmussen et al 2002).…”

Section: Ngc 419 Membershipmentioning

confidence: 99%

Short period variability in the globular cluster NGC 419 and the SMC field

Martinez-Vazquez,

Salinas,

Vivas

2020

Preprint

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We present the discovery of 54 Delta Scuti variables (δ Sct ) and three eclipsing binaries in the field of NGC 419, an intermediate-age globular cluster of the Small Magellanic Cloud (SMC), using g, r, i Gemini-S/GMOS time series observations. We find that only a handful of the δ Sct appear at the main sequence turnoff (MSTO) of the cluster while the majority is fainter, indicating that NGC 419 is younger (t 1.2 Gyr) than previously thought. Considering their radial distribution, we identify only six δ Sct as probable members of NGC 419 while the 48 remaining are likely δ Sct of the field of the SMC. Cluster δ Sct appear close to the red edge of the MSTO, supporting the idea that the extended MSTO has its origin in an age spread. The 48 field δ Sct represent the largest detection of δ Sct made in the field of the SMC. From them, we estimate the density of δ Sct in the field of the SMC in 1.6 δ Sct per arcmin −2 , which implies tens of thousands of δ Sct are to be discovered in the SMC. We have compared the period and amplitude distribution with other catalogs of δ Sct available in the literature, concluding that our work is barely biased in terms of short periods (P 0.04 d) and lowamplitudes (∆r 0.05 mag). Finally, we use the δ Sct population to calculate the distance modulus to the NGC 419 field using different period-luminosity relations. The average distance modulus obtained is 18.83 ± 0.27 mag, which agrees with previous measurements.

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Rotation of stars in NGC 6134

Cited by 9 publications

References 15 publications

Altair: The Brightest δ Scuti Star

Altair: The Brightest δ Scuti Star

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Short period variability in the globular cluster NGC 419 and the SMC field

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