4,372 research outputs found
J08069+1527: A newly discovered high amplitude, hybrid subdwarf B pulsator
We present our discovery of a new hybrid pulsating subdwarf B star,
J08069+1527. The effective temperature and surface gravity of 28,500400\,K
and 5.370.04\,dex, respectively, place this object inside the instability
strip and also among other pulsating hot subdwarfs of a hybrid nature, right
next to another fascinating star: Balloon\,090100001. From this proximity, we
anticipated this star could pulsate in both high and low frequency modes.
Indeed, our analysis of photometric data confirmed our prediction. We detected
two peaks in the high frequency region and two other peaks at low frequencies.
In addition, the amplitude of the dominant mode is very high and comparable to
the dominant peaks in other hybrid subdwarf B stars. Since this star is bright,
we performed time-series low resolution spectroscopy. Despite a low
signal-to-noise (S/N) ratio, we were able to detect the main peak from these
data. All our results strongly indicate that J08069+1527 is a high amplitude
pulsating hot subdwarf B star of hybrid nature. By analogy to the other
pulsating sdB star, we judge that the dominant mode we detected here has radial
nature. Future stellar modeling should provide us with quite good constrains as
p- and g-modes presented in this star are driven in different parts of its
interior.Comment: 7 pages, 10 figures, accepted for publication in MNRA
IMF isotopic properties in semi-peripheral collisions at Fermi energies
We study the neutron and proton dynamical behavior along the fragmentation
path in semi-peripheral collisions: 58Fe+58Fe (charge asymmetric, N/Z = 1.23)
and 58Ni+58Ni (charge symmetric, N/Z = 1.07), at 47 AMeV. We observe that
isospin dynamics processes take place also in the charge-symmetric system
58Ni+58Ni, that may produce more asymmetric fragments. A neutron enrichment of
the neck fragments is observed, resulting from the interplay between
pre-equilibrium emission and the phenomenon of "isospin-migration". Both
effects depend on the EoS (Equation of State) symmetry term. This point is
illustrated by comparing the results obtained with two different choices of the
symmetry energy density dependence.
New correlation observables are suggested, to study the reaction mechanism
and the isospin dynamics.Comment: 5 pages, 8 figures, Revtex4 Latex Styl
Instability of Boost-invariant hydrodynamics with a QCD inspired bulk viscosity
We solve the relativistic Navier-Stokes equations with homogeneous
boost-invariant boundary conditions, and perform a stability analysis of the
solution. We show that, if the bulk viscosity has a peak around as
inferred from QCD-based arguments, the background solution "freezes" at
to a nearly constant temperature state. This state is however highly unstable
with respect to certain inhomogeneous modes. Calculations show that these modes
have enough time to blow up and tear the system into droplets. We conjecture
that this is how freeze-out occurs in the QGP created in heavy ion collisions,
and perhaps similar transitions in the early universe.Comment: Accepted for publication, Rapid Communication in Physical Review C
Discussion extended, derivation and conclusions not change
Multicolour photometry of Balloon 090100001: linking the two classes of pulsating hot subdwarfs
We present results of the multicolour UBVR photometry of the high-amplitude
EC14026-type star, Balloon 090100001. The data span over a month and consist of
more than a hundred hours of observations. Fourier analysis of these data led
us to the detection of at least 30 modes of pulsation of which 22 are
independent. The frequencies of 13 detected modes group in three narrow ranges,
around 2.8, 3.8 and 4.7 mHz, where the radial fundamental mode, the first and
second overtones are likely to occur. Surprisingly, we also detect 9
independent modes in the low-frequency domain, between 0.15 and 0.4 mHz. These
modes are typical for pulsations found in PG1716+426-type stars, discovered
recently among cool B-type subdwarfs. The modes found in these stars are
attributed to the high-order g modes. As both kinds of pulsations are observed
in Balloon 090100001, it represents a link between the two classes of pulsating
hot subdwarfs. At present, it is probably the most suitable target for testing
evolutionary scenarios and internal constitution models of these stars by means
of asteroseismology.
Three of the modes we discovered form an equidistant frequency triplet which
can be explained by invoking rotational splitting of an = 1 mode. The
splitting amounts to about 1.58 Hz, leading to a rotation period of 7.1
0.1 days.Comment: 12 pages, 14 figures, accepted for publication in MNRAS. For
full-resolution postscript file, visit
http://www.as.wsp.krakow.pl/~andy/balloon.ps.g
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