43 research outputs found
The interaction of planetary nebulae and their AGB progenitors with the interstellar medium
Interaction with the Interstellar Medium (ISM) cannot be ignored in
understanding planetary nebula (PN) evolution and shaping. In an effort to
understand the range of shapes observed in the outer envelopes of PNe, we have
run a comprehensive set of three-dimensional hydrodynamic simulations, from the
beginning of the asymptotic giant branch (AGB) superwind phase until the end of
the post--AGB/PN phase. A 'triple-wind' model is used, including a slow AGB
wind, fast post--AGB wind and third wind reflecting the linear movement through
the ISM. A wide range of stellar velocities, mass-loss rates and ISM densities
have been considered. We find ISM interaction strongly affects outer PN
structures, with the dominant shaping occuring during the AGB phase. The
simulations predict four stages of PN--ISM interaction whereby the PN is
initially unaffected (1), then limb-brightened in the direction of motion (2),
then distorted with the star moving away from the geometric centre (3) and
finally so distorted that the object is no longer recognisable as a PN and may
not be classed as such (4). Parsec-size shells around PN are predicted to be
common. The structure and brightness of ancient PNe is largely determined by
the ISM interaction, caused by rebrightening during the second stage; this
effect may address the current discrepancies in Galactic PN abundance. The
majority of PNe will have tail structures. Evidence for strong interaction is
found for all known planetary nebulae in globular clusters.Comment: 22 pages, 16 figures, accepted by MNRAS (consists of 14 page journal
paper and 8 page online-only appendix). Email C Wareing for high quality PDF
versio
On the Exchange of Kinetic and Magnetic Energy Between Clouds and the Interstellar Medium
We investigate, through 2D MHD numerical simulations, the interaction of a
uniform magnetic field oblique to a moving interstellar cloud. In particular we
explore the transformation of cloud kinetic energy into magnetic energy as a
result of field line stretching. Some previous simulations have emphasized the
possible dynamical importance of a ``magnetic shield'' formed around clouds
when the magnetic field is perpendicular to the cloud motion (Jones et al.
1996, Miniati et al. 1998). It was not clear, however, how dependent those
findings were to the assumed field configuration and cloud properties. To
expand our understanding of this effect, we examine several new cases by varing
the magnetic field orientation angle with respect to the cloud motion (\theta),
the cloud-background density contrast, and the cloud Mach number.
We show that in 2D and with \theta large enough, the magnetic field tension
can become dominant in the dynamics of the motion of high density contrast, low
Mach number clouds. In such cases a significant fraction of cloud kinetic
energy can be transformed into magnetic energy with the magnetic pressure at
the cloud nose exceeding the ram pressure of the impinging flow. We derive a
characteristic timescale for this process of energy ``conversion''. We find
also that unless the cloud motion is highly aligned to the magnetic field,
reconnection through tearing mode instabilities in the cloud wake limit the
formation of a strong flux rope feature following the cloud. Finally we attempt
to interpret some observational properties of the magnetic field in view of our
results.Comment: 24 pages in aaspp4 Latex and 7 figures. Accepted for publication in
The Astrophysical Journa
Magnetic Instabilities and Phase Diagram of the Double-Exchange Model in Infinite Dimensions
Dynamical mean-field theory is used to study the magnetic instabilities and
phase diagram of the double-exchange (DE) model with Hund's coupling J_H >0 in
infinite dimensions. In addition to ferromagnetic (FM) and antiferromagnetic
(AF) phases, the DE model supports a broad class of short-range ordered (SRO)
states with extensive entropy and short-range magnetic order. For any site on
the Bethe lattice, the correlation parameter q of a SRO state is given by the
average q=, where theta_i is the angle between any spin and
its neighbors. Unlike the FM (q=0) and AF (q=1) transitions, the transition
temperature of a SRO state (T_{SRO}) with 0<q<1 cannot be obtained from the
magnetic susceptibility. But a solution of the coupled Green's functions in the
weak-coupling limit indicates that a SRO state always has a higher transition
temperature than the AF for all fillings p<1 and even than the FM for 0.26\le p
\le 0.39. For 0.39<p<0.73, where both the FM and AF phases are unstable for
small J_H, a SRO phase has a non-zero T_{SRO} except close to p=0.5. As J_H
increases, T_{SRO} eventually vanishes and the FM dominates. For small J_H, the
T=0 phase diagram is greatly simplified by the presence of the SRO phase. A SRO
phase is found to have lower energy than either the FM or AF phases for 0.26\le
p0 but appears for J_H\neq 0. For
p near 1, PS occurs between an AF with p=1 and either a SRO or a FM phase. The
stability of a SRO state at T=0 can be understood by examining the interacting
DOS,which is gapped for any nonzero J_H in an AF but only when J_H exceeds a
critical value in a SRO state.Comment: 38 pages, 11 figures, submitted to New Journal of Physic
A Spatially Resolved `Inside-out' Outburst of IP Pegasi
We present a comprehensive photometric dataset taken over the entire outburst
of the eclipsing dwarf nova IP Peg in September/October 1997. Analysis of the
lightcurves taken over the long rise to the peak-of-outburst shows conclusively
that the outburst started near the centre of the disc and moved outwards. This
is the first dataset that spatially resolves such an outburst. The dataset is
consistent with the idea that long rise times are indicative of such
`inside-out' outbursts. We show how the thickness and the radius of the disc,
along with the mass transfer rate change over the whole outburst. In addition,
we show evidence of the secondary and the irradiation thereof. We discuss the
possibility of spiral shocks in the disc; however we find no conclusive
evidence of their existence in this dataset.Comment: 8 pages, 8 figures, to be appear in MNRA
X Her and TX Psc: Two cases of ISM interaction with stellar winds observed by Herschel
The asymptotic giant branch (AGB) stars X Her and TX Psc have been imaged at
70 and 160 microns with the PACS instrument onboard the Herschel satellite, as
part of the large MESS (Mass loss of Evolved StarS) Guaranteed Time Key
Program. The images reveal an axisymmetric extended structure with its axis
oriented along the space motion of the stars. This extended structure is very
likely to be shaped by the interaction of the wind ejected by the AGB star with
the surrounding interstellar medium (ISM). As predicted by numerical
simulations, the detailed structure of the wind-ISM interface depends upon the
relative velocity between star+wind and the ISM, which is large for these two
stars (108 and 55 km/s for X Her and TX Psc, respectively). In both cases,
there is a compact blob upstream whose origin is not fully elucidated, but that
could be the signature of some instability in the wind-ISM shock. Deconvolved
images of X Her and TX Psc reveal several discrete structures along the
outermost filaments, which could be Kelvin-Helmholtz vortices. Finally, TX Psc
is surrounded by an almost circular ring (the signature of the termination
shock?) that contrasts with the outer, more structured filaments. A similar
inner circular structure seems to be present in X Her as well, albeit less
clearly.Comment: 11 pages, Astronomy & Astrophysics, in pres
Thin shell morphology in the circumstellar medium of massive binaries
We investigate the morphology of the collision front between the stellar
winds of binary components in two long-period binary systems, one consisting of
a hydrogen rich Wolf-Rayet star (WNL) and an O-star and the other of a Luminous
Blue Variable (LBV) and an O-star. Specifically, we follow the development and
evolution of instabilities that form in such a shell, if it is sufficiently
compressed, due to both the wind interaction and the orbital motion. We use
MPI-AMRVAC to time-integrate the equations of hydrodynamics, combined with
optically thin radiative cooling, on an adaptive mesh 3D grid. Using parameters
for generic binary systems, we simulate the interaction between the winds of
the two stars. The WNL+O star binary shows a typical example of an adiabatic
wind collision. The resulting shell is thick and smooth, showing no
instabilities. On the other hand, the shell created by the collision of the O
star wind with the LBV wind, combined with the orbital motion of the binary
components, is susceptible to thin shell instabilities, which create a highly
structured morphology. We identify the nature of the instabilities as both
linear and non-linear thin-shell instabilities, with distinct differences
between the leading and the trailing parts of the collision front. We also find
that for binaries containing a star with a (relatively) slow wind, the global
shape of the shell is determined more by the slow wind velocity and the orbital
motion of the binary, than the ram pressure balance between the two winds. The
interaction between massive binary winds needs further parametric exploration,
to identify the role and dynamical importance of multiple instabilities at the
collision front, as shown here for an LBV+O star system.Comment: 10 pages, 13 figures. Accepted for publication in A&
The Halos of Planetary Nebulae in the Mid-Infrared: Evidence for Interaction with the Interstellar Medium
The motion of planetary nebulae (PNe) through the interstellar medium (ISM)
is thought to lead to a variety of observational consequences, including the
formation of bright rims; deformation and fragmentation of the shells; and a
shift of the central stars away from the geometric centres of the envelopes.
These and other characteristics have been noted through imaging in the visual
wavelength regime. We report further observations of such shells taken in the
mid-infrared (MIR), acquired through programs of IRAC imaging undertaken using
the Spitzer Space Telescope (SST).
NGC 2440 and NGC 6629 are shown to possess likely interacting halos, together
with ram-pressure stripped material to one side of their shells. Similarly, the
outer halos of NGC 3242 and NGC 6772 appear to have been fragmented through
Rayleigh-Taylor (RT) instabilities, leading to a possible flow of ISM material
towards the inner portions of their envelopes. If this interpretation is
correct, then it would suggest that NGC 3242 is moving towards the NE; a
suggestion which is also supported through the presence of a 60 microns tail
extending in the opposite direction, and curved bands of H-alpha emission in
the direction of motion - components which may arise through RT instabilities
in the magnetized ISM.Comment: 14 pages, 9 figures, Accepted for publication in MNRAS. 42 pages in
arXi
Rings and Halos in the Mid-Infrared: The Planetary Nebulae NGC 7354 and NGC 3242
We present images of the planetary nebulae (PNe) NGC 7354 and NGC 3242 in
four mid-infrared (MIR) photometric bands centred at 3.6, 4.5, 5.8 and 8.0
microns; the results of observations undertaken using the Spitzer Space
Telescope (SST). The resulting images show the presence of a halo and rings in
NGC 3242, as previously observed through narrow band imaging at visual
wavelengths, as well as evidence for a comparable halo and ring system in NGC
7354. This is the first time that a halo and rings have been observed in the
latter source.
We have analysed the formation of halos as a result of radiatively
accelerated mass loss in the AGB progenitors. Although the models assume that
dust formation occurs in C-rich environments, we note that qualitatively
similar results would be expected for O-rich progenitors as well. The model
fall-offs in halo density are found to result in gradients in halo surface
brightness which are similar to those observed in the visible and MIR.Comment: 19 pages, 12 figures, Accepted for publication in MNRAS. 56 pages in
arXi
Optical polarization and near IR photometry of the proto-planetary nebula Hen 3-1475
We present BVRI CCD aperture polarization and near-infrared photometry of the
proto-planetary nebula Hen 3-1475. Its intrinsic polarization is high and shows
a strong spectral dependence. The position angles in all bands are
perpendicular to the axis of the observed bipolar structure. A Monte Carlo code
is used to model the intrinsic polarization of \hhe. Using disk dimensions and
other constraints suggested by previous works, we are able to reproduce the
observations with an optically thick disk composed by grains with a power-law
size distribution ranging from 0.06 to 0.22 um. We also reliably estimate the
foreground polarization from hundreds of stars contained in the CCD images. It
is parallel to the intrinsic polarization of Hen 3-1475. Possible implications
of this result are discussed. From IR observations, we estimate a interstellar
reddening, A(V), of about 3.2.Comment: ApJ accepted, 16 pages, 6 figure
Low-ionization structures in planetary nebulae: confronting models with observations
Around 50 PNe are presently known to possess "small-scale" low-ionization
structures (LISs). We consider here jets, jet-like, symmetrical and
non-symmetrical LISs and present a detailed comparison of the existing model
predictions with the observational morphological and kinematical properties. We
find that nebulae with LISs appear indistinctly spread among all morphological
classes of PNe, indicating that the processes leading to the formation of LISs
are not necessarily related to those responsible for the asphericity of the
large-scale morphological components of PNe. We show that both the observed
velocities and locations of most non-symmetrical LISs can be reasonably well
reproduced assuming either fossil condensations originated in the AGB wind or
in-situ instabilities. The jet models proposed to date (HD and MHD interacting
winds or accretion-disk collimated winds) appear unable to account
simultaneously for the kinematical ages and the angle between the jet and the
symmetry axes of the nebulae. The linear increase in velocity observed in
several jets favors MHD confinement compared to pure HD interacting wind
models. On the other hand, we find that the formation of jet-like systems
characterized by relatively low expansion velocities cannot be explained by any
of the existing models. Finally, the knots which appear in symmetrical and
opposite pairs of low velocity could be understood as the survival of fossil
(symmetrical) condensations formed during the AGB phase or as structures that
have experienced substantial slowing down by the ambient medium.Comment: 21 pages including 5 tables. To appear in ApJ 547, Jan 2001. Also
available at http://www.iac.es/publicaciones/preprints.htm