346 research outputs found
Valuation Strategies for Small Businesses\u27 Intangible Assets
Small business owners who attempt to sell their businesses may not receive full value if they do not adequately value their intangible assets. The purpose of this multiple case study was to explore effective strategies business leaders used to value intangible assets when considering the sale of their businesses. The participants for this study were 5 business owners in a metropolitan area in the southeastern United States who had successful valuation experiences during the sale of their businesses. Data were collected through semistructured interviews with participants, methodological triangulation, observations, and review of company documents. Data were analyzed using thematic analysis, coding narrative segments, and reviewing secondary data. The themes that emerged from data analysis include collecting and using company data concerning intangible assets; hiring a reputable accounting firm to assist in valuation; understanding the values of brand, customer base, and goodwill; and choosing the appropriate asset valuation approach. To accurately value the intangible assets of their businesses, the most significant and recurring theme in the participants\u27 responses was the need for assistance from a reputable accounting firm. The implications of this study for positive social change include the potential to enhance the economic investment in local areas where business owners appropriately value intangible assets
On a new theoretical calibration of the Stroemgren hk metallicity index: NGC6522 as a first test case
We present a new theoretical calibration of the Stroemgren metallicity index
hk by using alpha-enhanced evolutionary models transformed into the
observational plane by using atmosphere models with the same chemical mixture.
We apply the new Metallicity--Index--Color (MIC) relations to a sample of 85
field red giants (RGs) and find that the difference between photometric
estimates and spectroscopic measurements is on average smaller than 0.1 dex
with a dispersion of sigma = 0.19 dex. The outcome is the same if we apply the
MIC relations to a sample of eight RGs in the bulge globular cluster NGC6522,
but the standard deviation ranges from 0.26 (hk, v-y) to 0.49 (hk, u-y). The
difference is mainly caused by a difference in photometric accuracy. The new
MIC relations based on the (Ca-y) color provide metallicities systematically
more metal-rich than the spectroscopic ones. We found that the Ca-band is
affected by Ca abundance and possibly by chromospheric activity.Comment: Accepted for publication on The Astrophysical Journal Letter
Mass Outflow and Chromospheric Activity of Red Giant Stars in Globular Clusters II. M13 and M92
High resolution spectra of 123 red giant stars in the globular cluster M13
and 64 red giant stars in M92 were obtained with Hectochelle at the MMT
telescope. Emission and line asymmetries in Halpha, and Ca K are identified,
characterizing motions in the extended atmospheres and seeking differences
attributable to metallicity in these clusters and M15. On the red giant branch,
emission in Halpha generally appears in stars with T_eff < 4500 K and log
L/L_sun > 2.75. Fainter stars showing emission are asymptotic giant branch
(AGB) stars or perhaps binary stars. The line-bisector for Halpha reveals the
onset of chromospheric expansion in stars more luminous than log L/L_sun ~ 2.5
in all clusters, and this outflow velocity increases with stellar luminosity.
However, the coolest giants in the metal-rich M13 show greatly reduced outflow
in Halpha most probably due to decreased T_eff and changing atmospheric
structure. The Ca K_3 outflow velocities are larger than shown by Halpha at the
same luminosity and signal accelerating outflows in the chromospheres. Stars
clearly on the AGB show faster chromospheric outflows in Halpha than RGB
objects. While the Halpha velocities on the RGB are similar for all
metallicities, the AGB stars in the metal-poor M15 and M92 have higher outflow
velocities than in the metal-rich M13. Comparison of these chromospheric line
profiles in the paired metal-poor clusters, M15 and M92 shows remarkable
similarities in the presence of emission and dynamical signatures, and does not
reveal a source of the `second-parameter' effect.Comment: 41 pages, 14 figures, 11 tables, Accepted in Astronomical Journa
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The Observations Of The X-Ray Source Hz Herculis-Hercules X-1
NASAESASRCAstronom
The C+N+O abundance of Omega Centauri giant stars: implications on the chemical enrichment scenario and the relative ages of different stellar populations
We present a chemical-composition analysis of 77 red-giant stars in Omega
Centauri. We have measured abundances for carbon and nitrogen, and combined our
results with abundances of O, Na, La, and Fe that we determined in our previous
work. Our aim is to better understand the peculiar chemical-enrichment history
of this cluster, by studying how the total C+N+O content varies among the
different-metallicity stellar groups, and among stars at different places along
the Na-O anticorrelation. We find the (anti)correlations among the light
elements that would be expected on theoretical ground for matter that has been
nuclearly processed via high-temperature proton captures. The overall
[(C+N+O)/Fe] increases by 0.5 dex from [Fe/H] -2.0 to [Fe/H] -0.9. Our results
provide insight into the chemical-enrichment history of the cluster, and the
measured CNO variations provide important corrections for estimating the
relative ages of the different stellar populations.Comment: 26 pages, 9 figure - Accepted for publication in Ap
Magnetic field amplification and electron acceleration to near-energy equipartition with ions by a mildly relativistic quasi-parallel plasma protoshock
The prompt emissions of gamma-ray bursts are seeded by radiating
ultrarelativistic electrons. Internal shocks propagating through a jet launched
by a stellar implosion, are expected to amplify the magnetic field & accelerate
electrons. We explore the effects of density asymmetry & a quasi-parallel
magnetic field on the collision of plasma clouds. A 2D relativistic PIC
simulation models the collision of two plasma clouds, in the presence of a
quasi-parallel magnetic field. The cloud density ratio is 10. The densities of
ions & electrons & the temperature of 131 keV are equal in each cloud. The mass
ratio is 250. The peak Lorentz factor of the electrons is determined, along
with the orientation & strength of the magnetic field at the cloud collision
boundary. The magnetic field component orthogonal to the initial plasma flow
direction is amplified to values that exceed those expected from shock
compression by over an order of magnitude. The forming shock is
quasi-perpendicular due to this amplification, caused by a current sheet which
develops in response to the differing deflection of the incoming upstream
electrons & ions. The electron deflection implies a charge separation of the
upstream electrons & ions; the resulting electric field drags the electrons
through the magnetic field, whereupon they acquire a relativistic mass
comparable to the ions. We demonstrate how a magnetic field structure
resembling the cross section of a flux tube grows in the current sheet of the
shock transition layer. Plasma filamentation develops, as well as signatures of
orthogonal magnetic field striping. Localized magnetic bubbles form. Energy
equipartition between the ion, electron & magnetic energy is obtained at the
shock transition layer. The electronic radiation can provide a seed photon
population that can be energized by secondary processes (e.g. inverse Compton).Comment: 12 pages, 15 Figures, accepted to A&
Multiple populations in Omega Centauri: a cluster analysis of spectroscopic data
Omega Cen is composed of several stellar populations. Their history might
allow us to reconstruct the evolution of this complex object. We performed a
statistical cluster analysis on the large data set provided by Johnson and
Pilachowski (2010). Stars in Omega Cen divide into three main groups. The
metal-poor group includes about a third of the total. It shows a moderate O-Na
anticorrelation, and similarly to other clusters, the O-poor second generation
stars are more centrally concentrated than the O-rich first generation ones.
This whole population is La-poor, with a pattern of abundances for n-capture
elements which is very close to a scaled r-process one. The metal-intermediate
group includes the majority of the cluster stars. This is a much more complex
population, with an internal spread in the abundances of most elements. It
shows an extreme O-Na anticorrelation, with a very numerous population of
extremely O-poor and He-rich second generation stars. This second generation is
very centrally concentrated. This whole population is La-rich, with a pattern
of the abundances of n-capture elements that shows a strong contribution by the
s-process. The spread in metallicity within this metal-intermediate population
is not very large, and we might attribute it either to non uniformities of an
originally very extended star forming region, or to some ability to retain a
fraction of the ejecta of the core collapse SNe that exploded first, or both.
As previously noticed, the metal-rich group has an Na-O correlation, rather
than anticorrelation. There is evidence for the contribution of both massive
stars ending their life as core-collapse SNe, and intermediate/low mass stars,
producing the s-capture elements. Kinematics of this population suggests that
it formed within the cluster rather than being accreted.Comment: Accepted for publication in Astronomy and Astrophysic
Antiferromagnetic ordering in a 90 K copper oxide superconductor
Using elastic neutron scattering, we evidence a commensurate
antiferromagnetic Cu(2) order (AF) in the superconducting (SC) high-
cuprate (y=0.013, =93 K). As
in the Co-free system, the spin excitation spectrum is dominated by a magnetic
resonance peak at 41 meV but with a reduced spectral weight. The substitution
of Co thus leads to a state where AF and SC cohabit showing that the CuO
plane is a highly antiferromagnetically polarizable medium even for a sample
where T remains optimum.Comment: 3 figure
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