89 research outputs found
Age dependence of the Vega Phenomenon: Theory
In a separate paper (Decin et al 2003), we have re-examined the observations
of IR excess obtained with the ISO satellite and discussed the ages of stars
with excess. The amount of dust (measured by the luminosity fraction
\fdust=L_\mathrm{IR}/L_{\star}) seen around main-sequence stars of different
ages shows several interesting trends. To discuss these results in the context
of a physical model, we develop in this paper an analytical model for the dust
production in Vega-type systems. Previously it has been claimed that a powerlaw
slope of about -2 in the diagram plotting amount of dust versus time could be
explained by a simple collisional cascade. We show that such a cascade in fact
results in a powerlaw \fdust\propto t^{-1} if the dust removal processes are
dominated by collisions. A powerlaw \fdust\propto t^{-2} only results when the
dust removal processes become dominated by Pointing-Robertson drag. This may be
the case in the Kuiper Belt of our own solar system, but it is certainly not
the case in any of the observed disks. A steeper slope can, however, be created
by including continuous stirring into the models. We show that the existence of
both young and old Vega-like systems with large amounts of dust (\fdust\simeq
10^{-3}) can be explained qualitatively by Kuiper-Belt-like structures with
\emph{delayed stirring}. Finally, the absence of young stars with intermediate
amounts of dust may be due to the fact that stirring due to planet formation
may not be active in young low-mass disks. The considerations in this paper
support the picture of simultaneous stirring and dust production proposed by
Kenyon and Bromley (2002).Comment: 26 pages, 3 figures, accepted for Publication in Ap
A Vega--like disk associated with the planetary system of rho (1) CNC
Wetensch. publicatieFaculteit der Wiskunde en Natuurwetenschappe
Identification of a nearby stellar association in the Hipparcos catalog: implications for recent, local star formation
The TW Hydrae Association (~55 pc from Earth) is the nearest known region of
recent star formation. Based primarily on the Hipparcos catalog, we have now
identified a group of 9 or 10 co-moving star systems at a common distance (~45
pc) from Earth that appear to comprise another, somewhat older, association
(``the Tucanae Association''). Together with ages and motions recently
determined for some nearby field stars, the existence of the Tucanae and TW
Hydrae Associations suggests that the Sun is now close to a region that was the
site of substantial star formation only 10-40 million years ago. The TW Hydrae
Association represents a final chapter in the local star formation history.Comment: 5 pages incl figs and table
Incidence and survival of remnant disks around main-sequence stars
We present photometric ISO 60 and 170um measurements, complemented by some
IRAS data at 60um, of a sample of 84 nearby main-sequence stars of spectral
class A, F, G and K in order to determine the incidence of dust disks around
such main-sequence stars. Of the stars younger than 400 Myr one in two has a
disk; for the older stars this is true for only one in ten. We conclude that
most stars arrive on the main sequence surrounded by a disk; this disk then
decays in about 400 Myr. Because (i) the dust particles disappear and must be
replenished on a much shorter time scale and (ii) the collision of
planetesimals is a good source of new dust, we suggest that the rapid decay of
the disks is caused by the destruction and escape of planetesimals. We suggest
that the dissipation of the disk is related to the heavy bombardment phase in
our Solar System. Whether all stars arrive on the main sequence surrounded by a
disk cannot be established: some very young stars do not have a disk. And not
all stars destroy their disk in a similar way: some stars as old as the Sun
still have significant disks.Comment: 16 pages, 9 figures, Astron & Astrophys. in pres
Spatial Separation of the 3.29 micron Emission Feature and Associated 2 micron Continuum in NGC 7023
We present a new 0.9" resolution 3.29 micron narrowband image of the
reflection nebula NGC 7023. We find that the 3.29 micron IEF in NGC 7023 is
brightest in narrow filaments NW of the illuminating star. These filaments have
been seen in images of K', molecular hydrogen emission lines, the 6.2 and 11.3
micron IEFs, and HCO+. We also detect 3.29 micron emission faintly but
distinctly between the filaments and the star. The 3.29 micron image is in
contrast to narrowband images at 2.09, 2.14, and 2.18 micron, which show an
extended emission peak midway between the filaments and the star, and much
fainter emission near the filaments. The [2.18]-[3.29] color shows a wide
variation, ranging from 3.4-3.6 mag at the 2 micron continuum peak to 5.5 mag
in the filaments. We observe [2.18]-[3.29] to increase smoothly with increasing
distance from the star, up until the filament, suggesting that the main
difference between the spatial distributions of the 2 micron continuum and the
the 3.29 micron emission is related to the incident stellar flux. Our result
suggests that the 3.29 micron IEF carriers are likely to be distinct from, but
related to, the 2 micron continuum emitters. Our finding also imply that, in
NGC 7023, the 2 micron continuum emitters are mainly associated with HI, while
the 3.29 micron IEF carriers are primarily found in warm molecular hydrogen,
but that both can survive in HI or molecular hydrogen. (abridged)Comment: to appear in ApJ, including 1 table and 8 figures, high resolution
figures available at http://www.ast.cam.ac.uk/~jin/n7023
Molecular gas phase counterparts to solid state grain mantles features: implication for gas/grain chemistry
Mid-Infrared Emission Features in the ISM: Feature-to-Feature Flux Ratios
Using a limited, but representative sample of sources in the ISM of our
Galaxy with published spectra from the Infrared Space Observatory, we analyze
flux ratios between the major mid-IR emission features (EFs) centered around
6.2, 7.7, 8.6 and 11.3 microns, respectively. In a flux ratio-to-flux ratio
plot of EF(6.2)/EF(7.7) as a function of EF(11.3)/EF(7.7), the sample sources
form roughly a -shaped locus which appear to trace, on an overall
basis, the hardness of a local heating radiation field. But some driving
parameters other than the radiation field may also be required for a full
interpretation of this trend. On the other hand, the flux ratio of
EF(8.6)/EF(7.7) shows little variation over the sample sources, except for two
HII regions which have much higher values for this ratio due to an ``EF(8.6\um)
anomaly,'' a phenomenon clearly associated with environments of an intense
far-UV radiation field. If further confirmed on a larger database, these trends
should provide crucial information on how the EF carriers collectively respond
to a changing environment.Comment: 16 pages, 1 figure, 1 table; accepted for publication in ApJ Letter
- âŠ