193 research outputs found
Makna Hidup Pada Penyandang Disabilitas Daksa Di BBRSBD PROF. DR. Soeharso Surakarta
Become the sunatullah every life journey experienced by humans is sometimes pleasant and unpleasant. This as a test for humans aims to see the quality of their human beings. A pleasant experience may not be a problem, but how about unpleasant experiences such as tragic accidents, bomb explosions, and other calamities that result in disability, certain issues become a problem for the victims. This study aims to understand and describe how the meaning of life for people with disabilities and how dynamics get the meaning of life. The research method used is qualitative phononology where data collection is obtained from semi-structured interviews with the selection of informants using purposive sampling. Criteria for informants in this study were persons with physical disabilities due to accidents and willing to be research informants as evidenced by informed consent. The meaning of life to be a person with a disability can be seen from the feeling of being meaningful and happy and trying to improve worship because it is still given life and is grateful for the present life. After becoming a disabled person who initially lacked confidence became more confident, ridiculing, empathizing with others who were worse than himself, honing his potential or abilities and thinking about the future and feeling his life meant.
Keywords: Meaning of life, people with disabilities, physical disabilit
Self-adjustment mechanisms and their application for orthosis design
Medical orthoses aim at guiding anatomical joints along their natural trajectories while preventing pathological movements, especially in case of trauma or injuries. The motions that take place between bone surfaces have complex kinematics. These so-called arthrokinematic motions exhibit axes that move both in translation and rotation. Traditionally, orthoses are carefully adjusted and positioned such that their kinematics approximate the arthrokinematic movements as closely as possible in order to protect the joint. Adjustment procedures are typically long and tedious. We suggest in this paper another approach. We propose mechanisms having intrinsic self-aligning properties. They are designed such that their main axis self-adjusts with respect to the joint’s physiological axis during motion. When connected to a limb, their movement becomes homokinetic and they have the property of automatically minimizing internal stresses. The study is performed here in the planar case focusing on the most important component of the arthrokinematic motions of a knee joint
Malin 1: interacting galaxy pair?
Malin 1 is a unique, extraordinarily large low surface brightness galaxy. The
structure and the origins of the galaxy are poorly understood. The reason for
such a situation is an absence of detailed observational data, especially, of
high-resolution kinematics. In this Letter we study the stellar kinematics of
the inner part (r < 15 kpc) of Malin 1. We present spectroscopic arguments in
favour of a small galaxy - Malin 1B - being a companion probably interacting
with the main galaxy - Malin 1. This object is clearly seen in many published
images of Malin 1 but is not mentioned in any astronomical databases. Malin 1B
is located at the projected distance of 14 kpc from the Malin 1's nucleus and
has small - 6516 km/s - relative velocity, which we determined for the
first time. We suggest that ongoing interaction with Malin 1B can explain main
morphological features of the Malin 1's central region - two-armed spiral
structure, a bar, and an external one-armed spiral pattern. We also
investigated the large scale environment of Malin 1 and postulate that the
galaxy SDSS J123708.91+142253.2 might be responsible for the formation of
extended low-surface brightness envelope by means of head-on collision with
Malin 1 (in the framework of collision scenario proposed by Mapelli et al.
2008). To test the collisional origins of Malin 1 global structure, more
observational data and new numerical models are needed.Comment: 5 pages, 4 figures, accepted for publication in MNRA
The Role of a Hot Gas Environment on the Evolution of Galaxies
Most spiral galaxies are found in galaxy groups with low velocity
dispersions; most E/S0 galaxies are found in galaxy groups with relatively high
velocity dispersions. The mass of the hot gas we can observe in the E/S0 groups
via their thermal X-ray emission is, on average, as much as the baryonic mass
of the galaxies in these groups. By comparison, galaxy clusters have as much or
more hot gas than stellar mass. Hot gas in S-rich groups, however, is of low
enough temperature for its X-ray emission to suffer heavy absorption due to
Galactic HI and related observational effects, and hence is hard to detect. We
postulate that such lower temperature hot gas does exist in low velocity
dispersion, S-rich groups, and explore the consequences of this assumption. For
a wide range of metallicity and density, hot gas in S-rich groups can cool in
far less than a Hubble time. If such gas exists and can cool, especially when
interacting with HI in existing galaxies, then it can help link together a
number of disparate observations, both Galactic and extragalactic, that are
otherwise difficult to understand.Comment: 16 pages with one figure. ApJ Letters, in pres
Warm Molecular Hydrogen Emission in Normal Edge-On Galaxies NGC 4565 and NGC 5907
We have observed warm molecular hydrogen in two nearby edge-on disk galaxies,
NGC 4565 and NGC 5907, using the Spitzer high-resolution infrared spectrograph.
The 0-0 S(0) 28.2 micron and 0-0 S(1) 17.0 micron pure rotational lines were
detected out to 10 kpc from the center of each galaxy on both sides of the
major axis, and in NGC 4565 the S(0) line was detected at r = 15 kpc on one
side. This location lies beyond a steep drop in the radio continuum emission
from cosmic rays in the disk. Despite indications that star formation activity
decreases with radius, the H2 excitation temperature and the ratio of the H2
line and the far-IR luminosity surface densities, Sigma_L(H2}/Sigma_L(TIR},
change very little as a function of radius, even into the diffuse outer region
of the disk of NGC 4565. This suggests that the source of excitation of the H2
operates over a large range of radii, and is broadly independent of the
strength and relative location of UV emission from young stars. Although
excitation in photodissociation regions is the most common explanation for the
widespread H2 emission, cosmic ray heating or shocks cannot be ruled out. The
inferred mass surface densities of warm molecular hydrogen in both edge-on
galaxies differ substantially, being 4(-60) M_solar/pc^2 and 3(-50)
M_solar/pc^2 at r = 10 kpc for NGC 4565 and NGC 5907, respectively. The higher
values represent very unlikely point-source upper limits. The point source case
is not supported by the observed emission distribution in the spectral slits.
These mass surface densities cannot support the observed rotation velocities in
excess of 200 km/s. Therefore, warm molecular hydrogen cannot account for dark
matter in these disk galaxies, contrary to what was implied by a previous ISO
study of the nearby edge-on galaxy NGC 891.Comment: Accepted for publication in the Astronomical Journal (20 pages, 17
figures, 7 tables
A New Method of the Corotation Radius Evaluation in our Galaxy
We propose a new method for determination of the rotation velocity of the
galactic spiral density waves, correspondingly, the corotation radius, ,
in our Galaxy by means of statistical analysis of radial oxygen distribution in
the galactic disc derived over Cepheids. The corotation resonance happens to be
located at kpc, depending on the rate of gas infall on to
the galactic disc, the statistical error being kpc.
Simultaneously, the constant for the rate of oxygen synthesis in the galactic
disc was determined.
We also argue in favour of a very short time-scale formation of the galactic
disc, namely: Gyr. This scenario enables to solve the problem of
the lack of intergalactic gas infall.Comment: 5 pages, 5 figure, 1 tabl
Molecular Gas, Dust and Star Formation in the Barred Spiral NGC 5383
We present multi-wavelength (interferometer and single-dish CO J=1-0, Halpha,
broadband optical and near-infrared) observations of the classic barred spiral
NGC 5383. We compare the observed central gas and dust morphology to the
predictions of recent hydrodynamic simulations. In the nuclear region, our
observations reveal three peaks lying along a S-shaped gas and dust
distribution. In contrast, the model predicts a circumnuclear ring, not the
observed S-shaped distribution; moreover, the predicted surface density
contrast between the central gas accumulation and the bar dust lanes is an
order of magnitude larger than observed. The discrepancies are not due to
unexplored model parameter space or a nuclear bar but are probably due to the
vigorous (7 solar masses per year) star formation activity in the center.
As is common in similar bars, the star formation rate in the bar between the
bar ends and the central region is low (~0.5 solar masses per yr), despite the
high gas column density in the bar dust lanes; this is generally attributed to
shear and shocks. We note a tendency for the HII regions to be associated with
the spurs feeding the main bar dust lanes, but these are located on the leading
side of the bar. We propose that stars form in the spurs, which provide a high
column density but low shear environment. HII regions can therefore be found
even on the leading side of the bar because the ionizing stars pass
ballistically through the dust laneComment: Accepted for publication in The Astrophysical Journal, 33 pages
(includes 10 figures
Gas Mass Fractions and Star Formation in Blue-Sequence E/S0 Galaxies
Recent work has identified a population of low-redshift E/S0 galaxies that
lie on the blue sequence in color vs. stellar mass parameter space, where
spiral galaxies typically reside. While high-mass blue-sequence E/S0s often
resemble young merger or interaction remnants likely to fade to the red
sequence, we focus on blue-sequence E/S0s with lower stellar masses (< a few
10^10 M_sun), which are characterized by fairly regular morphologies and
low-density field environments where fresh gas infall is possible. This
population may provide an evolutionary link between early-type galaxies and
spirals through disk regrowth. Focusing on atomic gas reservoirs, we present
new GBT HI data for 27 E/S0s on both sequences as well as a complete tabulation
of archival HI data for other galaxies in the Nearby Field Galaxy Survey.
Normalized to stellar mass, the atomic gas masses for 12 of the 14
blue-sequence E/S0s range from 0.1 to >1.0. These gas-to-stellar mass ratios
are comparable to those of spiral and irregular galaxies and have a similar
dependence on stellar mass. Assuming that the HI is accessible for star
formation, we find that many of our blue-sequence E/S0s can increase in stellar
mass by 10-60% in 3 Gyr in both of two limiting scenarios, exponentially
declining star formation and constant star formation. In a constant star
formation scenario, about half of the blue-sequence E/S0s require fresh gas
infall on a timescale of <3 Gyr to avoid exhausting their atomic gas reservoirs
and evolving to the red sequence. We present evidence that star formation in
these galaxies is bursty and likely involves externally triggered gas inflows.
Our analysis suggests that most blue-sequence E/S0s are indeed capable of
substantial stellar disk growth on relatively short timescales. (abridged)Comment: ApJ, accepted, 26 pages with 12 figures (5 color), 5 table
Molecular Gas Kinematics in Barred Spiral Galaxies
To quantify the effect that bar driven mass inflow can have on the evolution
of a galaxy requires an understanding of the dynamics of the inflowing gas. In
this paper we study the kinematics of the dense molecular gas in a set of seven
barred spiral galaxies to determine which dynamical effects dominate. The
kinematics are derived from observations of the CO J=(1-0) line made with the
Berkeley-Illinois-Maryland Association (BIMA) millimeter array. We compare the
observed kinematics to those predicted by ideal gas hydrodynamic and ballistic
cloud-based models of gas flow in a barred potential. The hydrodynamic model is
in good qualitative agreement with both the current observations of the dense
gas and previous observations of the kinematics of the ionized gas. The
observed kinematics indicate that the gas abruptly changes direction upon
entering the dust lanes to flow directly down the dust lanes along the leading
edge of the bar until the dust lanes approach the nuclear ring. Near the
location where the dust lanes intersect the nuclear ring, we see two velocity
components: a low velocity component, corresponding to gas on circular orbits,
and a higher velocity component, which can be attributed to the fraction of gas
flowing down the bar dust lane which sprays past the contact point toward the
other half of the bar. The ballistic cloud-based model of the ISM is not
consistent with the observed kinematics. The kinematics in the dust lanes
require large velocity gradients which cannot be reproduced by an ISM composed
of ballistic clouds with long mean-free-paths. Therefore, even the dense ISM
responds to hydrodynamic forces.Comment: To be published in the Astrophysical Journal, Nov. 20, 199
X-Ray Searches for Emission from the WHIM in the Galactic Halo and the Intergalactic Medium
At least 50% of the baryons in the local universe are undetected and
predicted to be in a hot dilute phase (1E5-1E7 K) in low and moderate
overdensity environments. We searched for the predicted diffuse faint emission
through shadowing observations whereby cool foreground gas absorbs more distant
diffuse emission. Observations were obtained with Chandra and XMM-Newton. Using
the cold gas in two galaxies, NGC 891 and NGC 5907, shadows were not detected
and a newer observation of NGC 891 fails to confirm a previously reported X-ray
shadow. Our upper limits lie above model predictions. For Local Group studies,
we used a cloud in the Magellanic Stream and a compact high velocity cloud to
search for a shadow. Instead of a shadow, the X-ray emission was brighter
towards the Magellanic Stream cloud and there is a less significant brightness
enhancement toward the other cloud also. The brightness enhancement toward the
Magellanic Stream cloud is probably due to an interaction with a hot ambient
medium that surrounds the Milky Way. We suggest that this interaction drives a
shock into the cloud, heating the gas to X-ray emitting temperatures.Comment: 10 ApJ pages with 10 figure
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