The δ Scuti star FG Virginis. II. A search for high pulsation frequencies.

Details The δ Scuti star FG Virginis. II. A search for high pulsation frequencies. The δ Scuti star FG Virginis. II. A search for high pulsation frequencies.

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...309..197b&link_type=abstract

Astronomy and Astrophysics, v.309, p.197-202

Astronomy and Astrophysics

Astrophysics

14

Stars: Delta Scuti, Stars: Oscillations, Stars: Individual: Hd 106384 = Fg Vir

Scientific paper

Although the δ Scuti and roAp variables occupy similar positions on and near the main sequence, δ Scuti variables pulsate with lower radial and nonradial overtones and lower frequencies. To test whether high frequencies (as found in the roAp stars) are also present in δ Scuti stars, a multisite campaign with the Whole Earth Telescope (WET) was carried out for the star FG Vir. The 96.7hours of WET photometry were supplemented by measurements made with the Delta Scuti Network (DSN), because the DSN technique includes regular measurements of comparison stars and is better suited to monitoring the low frequencies (<=500μHz). This made possible the correction for low-frequency variability (10 pulsation frequencies from 106 to 395μHz and amplitudes from 0.001 to 0.02) in order to prevent spectral leakage into the high-frequency domain. It is shown that such a correction is essential. In the 1-10mHz region of interest (corresponding to periods between 17 and 1.7minutes) no significant stellar variability could be detected. The highest peaks in the amplitude spectra ranged from 0.00023 (near 1mHz) to 0.00012 near 10mHz, where the amplitudes are expressed in units of fractional intensity. Statistical tests show that these peaks are caused by noise. These results indicate that for FG Vir the multimode pulsations in the low-frequency region (with individual amplitudes up to 0.02) are not accompanied by photometrically detectable high overtone pulsation at high frequencies. This result is consistent with the hypothesis that high-order p-mode pulsations in the millimag range require a large magnetic field, as detected in the roAp stars.

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