2,148 research outputs found
Pengaruh Kompensasi Finansial dan Non Finansial terhadap Kinerja Karyawan pada PT. Bina Mandala Pratama Perkasa
Dewasa ini, dengan semakin ketatnya tingkat persaingan bisnis, mengakibatkan Perusahaan dihadapkan pada tantangan untuk dapat mempertahankan kelangsungan hidup. Oleh karena itu Perusahaan harus mampu bersaing dan salah satu alat yang dapat digunakan oleh Perusahaan adalah kompensasi. Jika program kompensasi dirasakan adil dan kompetitif oleh karyawan, maka Perusahaan akan lebih mudah untuk menarik karyawan yang potensial, mempertahankannya dan memotivasi karyawan agar lebih meningkatkan kinerjanya, sehingga produktivitas meningkat dan Perusahaan mampu menghasilkan produk dengan harga yang kompetitif. Pada akhirnya, Perusahaan bukan hanya unggul dalam persaingan, namun juga mampu mempertahankan kelangsungan hidupnya, bahkan mampu meningkatkan profitabilitas dan mengembangkan USAhanya
Massive Star Formation
The enormous radiative and mechanical luminosities of massive stars impact a
vast range of scales and processes, from the reionization of the universe, to
the evolution of galaxies, to the regulation of the interstellar medium, to the
formation of star clusters, and even to the formation of planets around stars
in such clusters. Two main classes of massive star formation theory are under
active study, Core Accretion and Competitive Accretion. In Core Accretion, the
initial conditions are self-gravitating, centrally concentrated cores that
condense with a range of masses from the surrounding, fragmenting clump
environment. They then undergo relatively ordered collapse via a central disk
to form a single star or a small-N multiple. In this case, the pre-stellar core
mass function has a similar form to the stellar initial mass function. In
Competitive Accretion, the material that forms a massive star is drawn more
chaotically from a wider region of the clump without passing through a phase of
being in a massive, coherent core. In this case, massive star formation must
proceed hand in hand with star cluster formation. If stellar densities become
very high near the cluster center, then collisions between stars may also help
to form the most massive stars. We review recent theoretical and observational
progress towards understanding massive star formation, considering physical and
chemical processes, comparisons with low and intermediate-mass stars, and
connections to star cluster formation.Comment: Accepted for publication as a chapter in Protostars and Planets VI,
University of Arizona Press (2014), eds. H. Beuther, R. Klessen, C.
Dullemond, Th. Hennin
Dynamics of a Massive Binary at Birth
Almost all massive stars have bound stellar companions, existing in binaries
or higher-order multiples. While binarity is theorized to be an essential
feature of how massive stars form, essentially all information about such
properties is derived from observations of already formed stars, whose orbital
properties may have evolved since birth. Little is known about binarity during
formation stages. Here we report high angular resolution observations of 1.3 mm
continuum and H30alpha recombination line emission, which reveal a massive
protobinary with apparent separation of 180 au at the center of the massive
star-forming region IRAS07299-1651. From the line-of-sight velocity difference
of 9.5 km/s of the two protostars, the binary is estimated to have a minimum
total mass of 18 solar masses, consistent with several other metrics, and
maximum period of 570 years, assuming a circular orbit. The H30alpha line from
the primary protostar shows kinematics consistent with rotation along a ring of
radius of 12 au. The observations indicate that disk fragmentation at several
hundred au may have formed the binary, and much smaller disks are feeding the
individual protostars.Comment: Published in Nature Astronomy. This is author's version. Full article
is available here (https://rdcu.be/brENk). 47 pages, 10 figures, including
methods and supplementary informatio
The SOFIA Massive (SOMA) Star Formation Survey. II. High Luminosity Protostars
We present multi-wavelength images observed with SOFIA-FORCAST from 10
to 40 m of seven high luminosity massive protostars, as part of the SOFIA
Massive (SOMA) Star Formation Survey. Source morphologies at these wavelengths
appear to be influenced by outflow cavities and extinction from dense gas
surrounding the protostars. Using these images, we build spectral energy
distributions (SEDs) of the protostars, also including archival data from
Spitzer, Herschel and other facilities. Radiative transfer (RT) models of Zhang
& Tan (2018), based on Turbulent Core Accretion theory, are then fit to the
SEDs to estimate key properties of the protostars. Considering the best five
models fit to each source, the protostars have masses accreting at rates of inside cores of initial masses embedded in clumps with mass surface densities and span a luminosity range of . Compared with the first eight protostars in Paper I, the sources
analyzed here are more luminous, and thus likely to be more massive protostars.
They are often in a clustered environment or have a companion protostar
relatively nearby. From the range of parameter space of the models, we do not
see any evidence that needs to be high to form these massive
stars. For most sources the RT models provide reasonable fits to the SEDs,
though the cold clump material often influences the long wavelength fitting.
However, for sources in very clustered environments, the model SEDs may not be
such a good description of the data, indicating potential limitations of the
models for these regions.Comment: 30 pages, 19 figures, Accepted for publication in Ap
The SOFIA Massive (SOMA) Star Formation Survey. I. Overview and First Results
We present an overview and first results of the Stratospheric Observatory For
Infrared Astronomy Massive (SOMA) Star Formation Survey, which is using the
FORCAST instrument to image massive protostars from
--. These wavelengths trace thermal emission from
warm dust, which in Core Accretion models mainly emerges from the inner regions
of protostellar outflow cavities. Dust in dense core envelopes also imprints
characteristic extinction patterns at these wavelengths, causing intensity
peaks to shift along the outflow axis and profiles to become more symmetric at
longer wavelengths. We present observational results for the first eight
protostars in the survey, i.e., multiwavelength images, including some
ancillary ground-based MIR observations and archival {\it{Spitzer}} and
{\it{Herschel}} data. These images generally show extended MIR/FIR emission
along directions consistent with those of known outflows and with shorter
wavelength peak flux positions displaced from the protostar along the
blueshifted, near-facing sides, thus confirming qualitative predictions of Core
Accretion models. We then compile spectral energy distributions and use these
to derive protostellar properties by fitting theoretical radiative transfer
models. Zhang and Tan models, based on the Turbulent Core Model of McKee and
Tan, imply the sources have protostellar masses --50
accreting at -- inside cores of
initial masses --500 embedded in clumps with mass surface
densities --3. Fitting Robitaille
et al. models typically leads to slightly higher protostellar masses, but with
disk accretion rates smaller. We discuss reasons for these
differences and overall implications of these first survey results for massive
star formation theories.Comment: Accepted to ApJ, 32 page
A Massive Protostar Forming by Ordered Collapse of a Dense, Massive Core
We present 30 and 40 micron imaging of the massive protostar G35.20-0.74 with
SOFIA-FORCAST. The high surface density of the natal core around the protostar
leads to high extinction, even at these relatively long wavelengths, causing
the observed flux to be dominated by that emerging from the near-facing outflow
cavity. However, emission from the far-facing cavity is still clearly detected.
We combine these results with fluxes from the near-infrared to mm to construct
a spectral energy distribution (SED). For isotropic emission the bolometric
luminosity would be 3.3x10^4 Lsun. We perform radiative transfer modeling of a
protostar forming by ordered, symmetric collapse from a massive core bounded by
a clump with high mass surface density, Sigma_cl. To fit the SED requires
protostellar masses ~20-34 Msun depending on the outflow cavity opening angle
(35 - 50 degrees), and Sigma_cl ~ 0.4-1 g cm-2. After accounting for the
foreground extinction and the flashlight effect, the true bolometric luminosity
is ~ (0.7-2.2)x10^5 Lsun. One of these models also has excellent agreement with
the observed intensity profiles along the outflow axis at 10, 18, 31 and 37
microns. Overall our results support a model of massive star formation
involving the relatively ordered, symmetric collapse of a massive, dense core
and the launching bipolar outflows that clear low density cavities. Thus a
unified model may apply for the formation of both low and high mass stars.Comment: 6 pages, 4 figures, 1 table, accepted to Ap
A major histocompatibility complex class I–dependent subset of memory phenotype CD8+ cells
Most memory phenotype (MP) CD44hi CD8+ cells are resting interleukin (IL)-15–dependent cells characterized by high expression of the IL-2/IL-15 receptor β (CD122). However, some MP CD8+ cells have a CD122lo phenotype and are IL-15 independent. Here, evidence is presented that the CD122lo subset of MP CD8+ cells is controlled largely by major histocompatibility complex (MHC) class I molecules. Many of these cells display surface markers typical of recently activated T cells (CD62Llo, CD69hi, CD43hi, and CD127lo) and show a high rate of background proliferation. Cells with this phenotype are highly enriched in common γ chain–deficient mice and absent from MHC-I−/− mice. Unlike CD122hi CD8+ cells, CD122lo MP CD8+ cells survive poorly after transfer to MHC-I−/− hosts and cease to proliferate. Although distinctly different from typical antigen-specific memory cells, CD122lo MP CD8+ cells closely resemble the antigen-dependent memory CD8+ cells found in chronic viral infections
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