Solar-like Oscillations in α Centauri B

By H. Kjeldsen, T. Bedding, R. P. Butler, J. Christensen-Dalsgaard, L. Kiss, C. McCarthy, G. Marcy, C. Tinney, Jason T. Wright. 2005

173 citations recorded by the source corpus.

We have made velocity observations of the star α Centauri B from two sites, allowing us to identify 37 oscillation modes with l = 0-3. Fitting to these modes gives the large and small frequency separations as a function of frequency. The mode lifetime, as measured from the scatter of the oscillation frequencies about a smooth trend, is similar to that in the Sun. Limited observations of the star δ Pav show oscillations centered at 2.3 mHz, with peak amplitudes close to solar. We introduce a new method of measuring oscillation amplitudes from heavily smoothed power density spectra, from which we estimated amplitudes for α Cen α and B, β Hyi, δ Pav, and the Sun. We point out that the oscillation amplitudes may depend on which spectral lines are used for the velocity measurements.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3aad487aaf7787d63436db581a6e60d5a9de89e0

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Citations in the corpus

The HARPS search for southern extra-solar planets - XIII. A planetary system with 3 super-Earths (4.2, 6.9, and 9.2 M) (2008, result): “The radial velocity intrinsic variability including the noise due to stellar granulation (Kjeldsen et al. 2005) and any effect related to the stellar magnetic activity is not known but, due to the low level of calcium reemission, this effect is by comparison with other similar stars less than 1 ms…”
Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters (2016, methodology): “Funding for the Stellar Astrophysics Centre (SAC) is provided by The Danish National Research Foundation (Grant DNRF106).”
SOLAR-LIKE OSCILLATIONS IN LOW-LUMINOSITY RED GIANTS: FIRST RESULTS FROM KEPLER (2010, background): “…average small separation δν01 in these red giants is negative, whereas it is positive in the Sun and the handful of other main-sequence stars for which it has been measured: α Cen A (Bedding et al. 2004), α Cen B (Kjeldsen et al. 2005), γ Pav (Mosser et al. 2008), and τ Cet (Teixeira et al. 2009).”
AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, background): “A double hump has also been observed in the power envelope of α Centauri B (Kjeldsen et al. 2005), yet another K dwarf, an indication that νmax may become ambiguous for low-mass dwarfs.”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, unknown): “…6 . . . Bouchy & Carrier (2001); 7 . . . Teixeira et al. (2009), estimated from the mean density of 2.21±0.01 gcm−3 determined by the authors; 8 . . . Kjeldsen et al. (2005), oscillations discovered by Carrier & Bourban (2003); 9 . . . Bazot et al. (2011); 10 . . . Bouchy et al. (2005); 11 . . .…”
FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, background): “…(Appourchaux et al. 2008), and from ground-based Doppler observations for the remaining sample (Carrier & Bourban 2003; Kjeldsen et al. 2003; Bedding et al. 2004; Carrier et al. 2005a,b; Kjeldsen et al. 2005; Bedding et al. 2007; Arentoft et al. 2008; Teixeira et al. 2009; Bazot et al. 2011).”
Planetary detection limits taking into account stellar noise - I. Observational strategies to reduce stellar oscillation and granulation effects (2010, methodology): “…sample is taken from the literature:57.2µHz for βHyi (Bedding et al. 2007) , 106µHz for αCen A (Kjeldsen et al. 2005), 90µHz for µAra (Bazot et al. 2005), 169µHz for τCeti (Teixeira et al. 2009) and 162µHz for αCen B (Kjeldsen et al. 2005) 5 The width of the box changes according to the frequency.”
SOAP 2.0: A TOOL TO ESTIMATE THE PHOTOMETRIC AND RADIAL VELOCITY VARIATIONS INDUCED BY STELLAR SPOTS AND PLAGES (2014, background): “At the meter-persecond level, RV measurements are affected by solartype oscillations (Arentoft et al. 2008; Kjeldsen et al. 2005; Bouchy et al. 2005; Mayor et al. 2003), granulation phenomena (Dumusque et al. 2011b; Lindegren & Dravins 2003; Dravins 1982), and activity signals (Robertson et al.…”
Five Planets Orbiting 55 Cancri (2007, methodology): “In November 2004 we began making three consecutive observations (and sometimes five) of 55 Cnc to average over stellar p-mode oscillations that can add 1 m s−1 velocity noise to G8V main sequence stars (Kjeldsen et al. 2005).”