# Line-profile variations of stochastically excited oscillations in four evolved stars

@article{Hekker2010LineprofileVO,
title={Line-profile variations of stochastically excited oscillations in four evolved stars},
journal={Astronomy and Astrophysics},
year={2010},
volume={515},
pages={1-9}
}
• Published 10 February 2010
• Physics
• Astronomy and Astrophysics
Context. Since solar-like oscillations were first detected in red-giant stars, the presence of non-radial oscillation modes has been debated. Spectroscopic line-profile analysis was used in the first attempt to perform mode identification, which revealed that non-radial modes are observable. Despite the fact that the presence of non-radial modes could be confirmed, the degree or azimuthal order could not be uniquely identified. Here we present an improvement to this first spectroscopic line…

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## References

SHOWING 1-10 OF 31 REFERENCES

### Theoretical amplitudes and lifetimes of non-radial solar-like oscillations in red giants

• Physics
• 2009
Context. Solar-like oscillations have been observed in numerous red giants from ground and from space. An important question arises: could we expect to detect non-radial modes probing the internal

### Pulsations detected in the line profile variations of red giants. Modelling of line moments, line bisector and line shape

• Physics
• 2006
Observatoire de Gene`ve, 51 chemin de Maillettes, 1290 Sauverny, SwitzerlandReceived idate?; accepted idate?ABSTRACTContext. So far, red giant oscillations have been studied from radial velocity

### Oscillations of α UMa and other red giants

• Physics
• 2001
There is growing observational evidence that the variability of red giants could be caused by self-excitation of global modes of oscillation. The most recent evidence of such oscillations was

### A new method for the spectroscopic identification of stellar non-radial pulsation modes. I. The meth

Aims. We present the Fourier parameter fit method, a new method for spectroscopically identifying stellar radial and non-radial pulsation modes based on the high-resolution time-series spectroscopy

### Detection of solar-like oscillations in the red giant star $\epsilon$ Ophiuchi by MOST spacebased photometry

• Physics
• 2007
Context. Solar-like oscillations have been discovered in a few red giants, including ϵ  Oph, through spectroscopy. Acoustic modes around 60  μ Hz were clearly seen in this star, but daily aliasing of

• Physics
Nature
• 2009
The presence of radial and non-radial oscillations in more than 300 giant stars is reported, finding giant stars with equally spaced frequency peaks in the Fourier spectrum of the time series, as well as giants for which the spectrum seems to be more complex.

### SOLAR-LIKE OSCILLATIONS IN LOW-LUMINOSITY RED GIANTS: FIRST RESULTS FROM KEPLER

• Physics
• 2010
We have measured solar-like oscillations in red giants using time-series photometry from the first 34 days of science operations of the Kepler Mission. The light curves, obtained with 30 minute

### Solar-like Oscillations in the G2 Subgiant β Hydri from Dual-Site Observations

• Physics
• 2007
We have observed oscillations in the nearby G2 subgiant star β Hyi using high-precision velocity observations obtained over more than a week with the HARPS and UCLES spectrographs. The oscillation

### Precise radial velocities of giant stars. III. Spectroscopic stellar parameters

• Physics, Geology
• 2007
Context. A radial velocity survey of about 380 G and K giant stars is ongoing at Lick observatory. For each star we have a high signal to noise ratio template spectrum, which we use to determine

### Nonradial p-modes in the G9.5 giant $\epsilon$ Ophiuchi? Pulsation model fits to MOST photometry

• Physics, Geology
• 2008
The G9.5 giant ∈ Oph shows evidence of radial p-mode pulsations in both radial velocity and luminosity. We re-examine the observed frequencies in the photometry and radial velocities and find a best