Strömgren photometry and spectroscopy of the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si86.gif" overflow="scroll"><mml:mrow><mml:mi>δ</mml:mi></mml:mrow></mml:math> Scuti stars 7 Aql and 8 Aql

Fox-Machado, L.; Álvarez, M.; Michel, R.; Moya, A.; Peña, J. H.; Parrao, L.; Castro, A.

doi:10.1016/j.newast.2009.11.006

Cited by 6 publications

(5 citation statements)

References 24 publications

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“…HD 174532 (7 Aql) has a spectral type of A9 IV listed by Houk & Swift (1999), although later studies revealed it to be an evolved star with a spectral type of A2 III/IV, an effective temperature of approximately T eff 7200 K, a surface gravity of log g 3.6 and a projected surface rotational velocity of v sin i 32 km s −1 (Poretti et al 2003;Fox Machado et al 2008, 2010McDonald et al 2012). HD 174532 was previously known to be a multi-periodic δ Sct star (Fox Machado et al 2008Machado et al , 2010, and in our analysis of the CoRoT photometry of HD 174532, we extract 33 frequency peaks with a S /N ≥ 4 using our conservative approach to iterative pre-whitening. As shown in Fig.…”

Section: Hd 174532mentioning

confidence: 99%

Photometric detection of internal gravity waves in upper main-sequence stars

Bowman

Aerts

Johnston

et al. 2019

A&A

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Early-type stars are predicted to excite an entire spectrum of internal gravity waves (IGWs) at the interface of their convective cores and radiative envelopes. Numerical simulations of IGWs predict stochastic low-frequency variability in photometric observations, yet the detection of IGWs in early-type stars has been limited by a dearth of high-quality photometric time series. We present observational evidence of stochastic low-frequency variability in the CoRoT photometry of a sample of O, B, A and F stars. The presence of this stochastic low-frequency variability in stars across the upper main-sequence cannot be universally explained as granulation or stellar winds, but its morphology is found to be consistent with predictions from IGW simulations.

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Section: Hd 174532mentioning

confidence: 99%

Photometric detection of internal gravity waves in upper main-sequence stars

Bowman

Aerts

Johnston

et al. 2019

A&A

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“…Peña et al (2007Peña et al ( , 2011]. The observing procedure is the same as explained in Fox Machado et al (2010). Briefly, the observing routine consisted of five 10 s of integration of the star from which five 10 s of integration of the sky was subtracted.…”

Section: Strömgren Photometry and Spectroscopymentioning

confidence: 99%

Searching for short-period variable stars in the direction of Coma Berenices and Upgren 1 open clusters: Melotte 111 AV 1224 a new eclipsing binary star

Machado,

Michel,

Alvarez

et al. 2014

Preprint

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We report the results of CCD photometric observations in the direction of the Coma Berenices and Upgren 1 open clusters with the aim at searching for new short-period variable stars. A total of 35 stars were checked for variability. As a result of this search the star designated in the SIMBAD database as Melotte 111 AV 1224 was found to be a new eclipsing binary star. Follow-up Strömgren photometric and spectroscopic observations allowed us to derive the spectral type, distance, reddening and effective temperature of the star. A preliminary analysis of the binary light curve was performed and the parameters of the orbital system were derived. From the derived physical parameters we conclude that Melotte 111 AV 1224 is most likely a W-UMa eclipsing binary that is not a member of the Coma Berenices open cluster. On other hand, we did not find evidence of brightness variations in the stars NSV 5612 and NSV 5615 previously catalogued as variable stars in Coma Berenices open cluster.

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“…We used the same equipment as explained in Fox Machado et al (2010). In particular, we used the Boller & Chivens spectrograph installed in the Cassegrain focus of the telescope.…”

Section: Observations Data Reduction and Conclusionmentioning

confidence: 99%

“…The spectroscopic observations were conducted at the 2.12-m telescope of the OAN-SPM observatory during several short runs between 2010 and 2012. We used the same equipment as explained in Fox Machado et al (2010). In particular, we used the Boller & Chivens spectrograph installed in the Cassegrain focus of the telescope.…”

Section: Observations Data Reduction and Conclusionmentioning

confidence: 99%