744 research outputs found
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
The initial stellar mass function from random sampling in hierarchical clouds II: statistical fluctuations and a mass dependence for starbirth positions and times
Observed variations in the slope of the initial stellar mass function are
shown to be consistent with a model in which the protostellar gas is randomly
sampled from hierarchical clouds at a rate proportional to the square root of
the local density. RMS variations in the IMF slope around the Salpeter value
are +/- 0.4 when only 100 stars are observed, and +/- 0.1 when 1000 stars are
observed. The hierarchical-sampling model also reproduces the tendency for
massive stars to form closer to the center of a cloud, at a time somewhat later
than the formation time of the lower mass stars. The assumed density dependence
for the star formation rate is shown to be appropriate for turbulence
compression, magnetic diffusion, gravitational collapse, and clump or
wavepacket coalescence. The low mass flattening in the IMF comes from the
inability of gas to form stars below the thermal Jeans mass at typical
temperatures and pressures. Consideration of heating and cooling processes
indicate why the thermal Jeans mass should be nearly constant in normal
environments, and why it might increase in some starburst regions. The steep
IMF in the extreme field is not explained by the model, but other origins are
suggested.Comment: 21 pages, 8 figures, scheduled for ApJ vol. 515, April 10, 199
Classbeacons: Enhancing reflection-inaction of teachers through spatially distributed ambient information
© 2019 Copyright is held by the author/owner(s). ACM Reflection-in-action (RiA) refers to teachers' reflections on their teaching performance during busy classroom routines. RiA is a demanding competence for teachers, but little has been known about how HCI systems could support teachers' RiA during their busy and intensive teaching. To bridge this gap, we design and evaluate an ambient information system named ClassBeacons. ClassBeacons aims to help teachers intuitively reflect-in-action on how to divide time and attention over pupils throughout a lesson. ClassBeacons subtly depicts teachers' division of time and attention over pupils through multiple light-objects distributed over students' desks. Each light-object indicates how long the teacher has been cumulatively around it (helping an adjacent student) by shifting color. A field evaluation with eleven teachers proved that ClassBeacons enhanced teachers' RiA by supporting their sensemaking of ongoing performance and modification of upcoming actions. Furthermore, ClassBeacons was experienced to unobtrusively fit into teachers' routines without overburdening teaching in progress
The Distribution of Nearby Stars in Velocity Space Inferred from Hipparcos Data
(abridged) The velocity distribution f(v) of nearby stars is estimated, via a
maximum- likelihood algorithm, from the positions and tangential velocities of
a kinematically unbiased sample of 14369 stars observed by the HIPPARCOS
satellite. f(v) shows rich structure in the radial and azimuthal motions, v_R
and v_phi, but not in the vertical velocity, v_z: there are four prominent and
many smaller maxima, many of which correspond to well known moving groups.
While samples of early-type stars are dominated by these maxima, also up to 25%
of red main-sequence stars are associated with them. These moving groups are
responsible for the vertex deviation measured even for samples of late-type
stars; they appear more frequently for ever redder samples; and as a whole they
follow an asymmetric-drift relation, in the sense that those only present in
red samples predominantly have large |v_R| and lag in v_phi w.r.t. the local
standard of rest (LSR). The question arise, how these old moving groups got on
their eccentric orbits. A plausible mechanism, known from solar system
dynamics, which is able to manage a shift in orbit space involves locking into
an orbital resonance.
Apart from these moving groups, there is a smooth background distribution,
akin to Schwarzschild's ellipsoidal model, with axis ratio of about 1:0.6:0.35
in v_R, v_phi, and v_z. The contours are aligned with the direction, but
not w.r.t. the v_phi and v_z axes: the mean v_z increases for stars rotating
faster than the LSR. This effect can be explained by the stellar warp of the
Galactic disk. If this explanation is correct, the warp's inner edge must not
be within the solar circle, while its pattern rotates with frequency of about
13 km/s/kpc or more retrograde w.r.t. the stellar orbits.Comment: 16 pages LaTeX (aas2pp4.sty), 6 figures, accepted by A
Updated Information on the Local Group
The present note updates the information published in my recent monograph on
\underline{The Galaxies of the Local Group}. Highlights include (1) the
addition of the newly discovered Cetus dwarf spheroidal as a certain member of
the Local Group, (2) an improved distance for SagDIG, which now places this
object very close to the edge of the Local Group zero-velocity surface, (3)
more information on the evolutionary histories of some individual Local Group
members, and (4) improved distance determinations to, and luminosities for, a
number of Local Group members. These data increase the number of certain (or
probable) Local Group members to 36. The spatial distribution of these galaxies
supports Hubble's claim that the Local Group ``is isolated in the general
field.'' Presently available evidence suggests that star formation continued
much longer in many dwarf spheroidals than it did in the main body of the
Galactic halo. It is suggested that ``young'' globular clusters, such as
Ruprecht 106, might have formed in now defunct dwarf spheroidals. Assuming
SagDIG, which is the most remote Local Group galaxy, to lie on, or just inside,
the zero-velocity surface of the Local Group yields a dynamical age \gtrsim
17.9 \pm 2.7 Gyr.Comment: 19 pages, 1 figure, to be published in the April 2000 issue of PAS
A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups
Nearby late-type stars are excellent targets for seeking young objects in
stellar associations and moving groups. The origin of these structures is still
misunderstood, and lists of moving group members often change with time and
also from author to author. Most members of these groups have been identified
by means of kinematic criteria, leading to an important contamination of
previous lists by old field stars. We attempt to identify unambiguous moving
group members among a sample of nearby-late type stars by studying their
kinematics, lithium abundance, chromospheric activity, and other age-related
properties. High-resolution echelle spectra () of a sample of
nearby late-type stars are used to derive accurate radial velocities that are
combined with the precise Hipparcos parallaxes and proper motions to compute
galactic-spatial velocity components. Stars are classified as possible members
of the classical moving groups according to their kinematics. The spectra are
also used to study several age-related properties for young late-type stars,
i.e., the equivalent width of the lithium Li~{\sc i} \space 6707.8 \space \AA
\space line or the index. Additional information like X-ray
fluxes from the ROSAT All-Sky Survey or the presence of debris discs is also
taken into account. The different age estimators are compared and the moving
group membership of the kinematically selected candidates are discussed. From a
total list of 405 nearby stars, 102 have been classified as moving group
candidates according to their kinematics. i.e., only 25.2 \% of the
sample. The number reduces when age estimates are considered, and only 26
moving group candidates (25.5\% of the 102 candidates) have ages in agreement
with the star having the same age as an MG memberComment: 39 pages, 11 figures. Accepted for publication in Astronomy \&
Astrophysic
Blue Straggler Stars: Early Observations that Failed to Solve the Problem
In this chapter, I describe early ideas on blue stragglers, and various
observations (some published, some not) that promised but failed to resolve the
question of their origin. I review the data and ideas that were circulating
from Allan Sandage's original discovery in 1953 of "anomalous blue stars" in
the globular cluster M3, up until about 1992, when what seems to have been the
only previous meeting devoted to Blue Straggler Stars (BSSs) was held at the
Space Telescope Science Institute.Comment: Chapter 2, in Ecology of Blue Straggler Stars, H.M.J. Boffin, G.
Carraro & G. Beccari (Eds), Astrophysics and Space Science Library, Springe
Target selection for the SUNS and DEBRIS surveys for debris discs in the solar neighbourhood
Debris discs - analogous to the Asteroid and Kuiper-Edgeworth belts in the
Solar system - have so far mostly been identified and studied in thermal
emission shortward of 100 um. The Herschel space observatory and the SCUBA-2
camera on the James Clerk Maxwell Telescope will allow efficient photometric
surveying at 70 to 850 um, which allow for the detection of cooler discs not
yet discovered, and the measurement of disc masses and temperatures when
combined with shorter wavelength photometry. The SCUBA-2 Unbiased Nearby Stars
(SUNS) survey and the DEBRIS Herschel Open Time Key Project are complimentary
legacy surveys observing samples of ~500 nearby stellar systems. To maximise
the legacy value of these surveys, great care has gone into the target
selection process. This paper describes the target selection process and
presents the target lists of these two surveys.Comment: 67 pages with full tables, 7 figures, accepted to MNRA
Stone-Wales Transformation Paths in Fullerene C60
The mechanisms of formation of a metastable defect isomer of fullerene C60
due to the Stone-Wales transformation are theoretically studied. It is
demonstrated that the paths of the "dynamic" Stone-Wales transformation at a
high sufficient for overcoming potential barriers) temperature can differ from
the two "adiabatic" transformation paths discussed in the literature. This
behavior is due to the presence of a great near-flat segment of the
potential-energy surface in the neighborhood of metastable states. Besides, the
sequence of rupture and formation of interatomic bonds is other than that in
the case of the adiabatictransformation.Comment: 10 pages, 6 figure
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