6 research outputs found
Asteroseismological studies of three Beta Cephei stars: IL Vel, V433 Car and KZ Mus
We have acquired between 127 and 150 h of time-resolved multicolour
photometry for each of the three Beta Cephei stars IL Vel, V433 Car and KZ Mus
over a time span of four months from two observatories. All three objects are
multiperiodic with at least three modes of pulsation. Mode identification from
the relative colour amplitudes is performed. We obtain unambiguous results for
the two highest-amplitude modes of IL Vel (both are l=1) and the three
strongest modes of KZ Mus (l=2,0 and 1), but none for V433 Car. Spectroscopy
shows the latter star to be a fast rotator (v sin i = 240 km/s), whereas the
other two have moderate v sin i (65 and 47 km/s, respectively). We performed
model calculations with the Warsaw-New Jersey stellar evolution and pulsation
code. We find that IL Vel is an object of about 12 Msun in the second half of
its main sequence evolutionary track. Its two dipole modes are most likely
rotationally split components of the mode originating as p1 on the ZAMS; one of
these modes is m=0. V433 Car is suggested to be an unevolved 13 Msun star just
entering the Beta Cephei instability strip. KZ Mus seems less massive (about
12.7 Msun) and somewhat more evolved, and its radial mode is probably the
fundamental one. In this case its quadrupole mode would be the one originating
as g1, and its dipole mode would be p1. It is suggested that mode
identification of slowly rotating Beta Cephei stars based on photometric colour
amplitudes is reliable; we estimate that a relative accuracy of 3% in the
amplitudes is sufficient for unambiguous identifications. Due to the good
agreement of our theoretical and observational results we conclude that the
prospects for asteroseismology of multiperiodic slowly rotating Beta Cephei
star are good.Comment: 16 pages, 16 figures, MNRAS, in pres
A multisite photometric study of two unusual Beta Cep stars: the magnetic V2052 Oph and the massive rapid rotator V986 Oph
We report a multisite photometric campaign for the Beta Cep stars V2052 Oph
and V986 Oph. 670 hours of high-quality differential photoelectric Stromgren,
Johnson and Geneva time-series photometry were obtained with eight telescopes
on five continents during 182 nights. Frequency analyses of the V2052 Oph data
enabled the detection of three pulsation frequencies, the first harmonic of the
strongest signal, and the rotation frequency with its first harmonic.
Pulsational mode identification from analysing the colour amplitude ratios
confirms the dominant mode as being radial, whereas the other two oscillations
are most likely l=4. Combining seismic constraints on the inclination of the
rotation axis with published magnetic field analyses we conclude that the
radial mode must be the fundamental. The rotational light modulation is in
phase with published spectroscopic variability, and consistent with an oblique
rotator for which both magnetic poles pass through the line of sight. The
inclination of the rotation axis is 54o <i< 58o and the magnetic obliquity 58o
<beta< 66o. The possibility that V2052 Oph has a magnetically confined wind is
discussed. The photometric amplitudes of the single oscillation of V986 Oph are
most consistent with an l=3 mode, but this identification is uncertain.
Additional intrinsic, apparently temporally incoherent, light variations of
V986 Oph are reported. Different interpretations thereof cannot be
distinguished at this point, but this kind of variability appears to be present
in many OB stars. The prospects of obtaining asteroseismic information for more
rapidly rotating Beta Cep stars, which appear to prefer modes of higher l, are
briefly discussed.Comment: 12 pages, 8 figures, MNRAS, in pres
Asteroseismology of the Beta Cephei star Nu Eridani: photometric observations and pulsational frequency analysis
We undertook a multisite photometric campaign for the Beta Cephei star Nu
Eridani. More than 600 hours of differential photoelectric uvyV photometry were
obtained with 11 telescopes during 148 clear nights. The frequency analysis of
our measurements shows that the variability of Nu Eri can be decomposed into 23
sinusoidal components, eight of which correspond to independent pulsation
frequencies between 5 - 8 c/d. Some of these are arranged in multiplets, which
suggests rotational m-mode splitting of nonradial pulsation modes as the cause.
If so, the rotation period of the star must be between 30 - 60 d. One of the
signals in the light curves of Nu Eri has a very low frequency of 0.432 c/d. It
can be a high-order combination frequency or, more likely, an independent
pulsation mode. In the latter case Nu Eri would be both a Beta Cephei star and
a slowly pulsating B (SPB) star. The photometric amplitudes of the individual
pulsation modes of Nu Eri appear to have increased by about 20 per cent over
the last 40 years. So do the amplitudes of the dominant combination frequencies
of the star. Among the latter, we only could identify sum frequencies with
certainty, not difference frequencies, which suggests that neither light-curve
distortion in its simplest form nor resonant mode coupling are their single
cause. One of our comparison stars, Mu Eridani, turned out to be variable with
a dominant time scale of 1.62 d. We believe that it is either an SPB star just
leaving its instability strip or that its variations are of rotational origin.Comment: 10 pages, 5 figure
The d Scuti star FG Vir. V. The 2002 photometric multisite campaign
Astronomy and Astrophysics, v. 419, n. 2, p. 695-701, 2004. http://dx.doi.org/10.1051/0004-6361:20035830International audienc