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Titik kesetimbangan pada pelelangan medol Belanda
Pelelangan adalah salah satu bentuk transaksi. Dalam pelelangan diasumsikan bahwa barang yang dilelang merupakan barang yang dapat dibagi. Sehingga jika penawar menilai harga barang = v dan penawaran yang diajukan = b,
maka keuntungannya jika ia menang adalah v-b, jika
terdapat k penawar yang menang adalah --(v-b) dan U jika
Pelelangan merupakan_Masalah keputusan banvak Orang
yang dapat diubah ke dalam format permainan. Dengan menggunakan pendekatan teori permainan akan dapat ditentukan pasangan-pasangan kesetimbangannya pada 4 situasi tawar menawar 1. vi > v2 + 2
2. v1 = v2 + 2
3. VI = V2 + 1
4. vi = v2 = v
v
Stellar laboratories. IX. New Se V, Sr IV - VII, Te VI, and I VI oscillator strengths and the Se, Sr, Te, and I abundances in the hot white dwarfs G191-B2B and RE 0503-289
To analyze spectra of hot stars, advanced non-local thermodynamic equilibrium
(NLTE) model-atmosphere techniques are mandatory. Reliable atomic data is for
the calculation of such model atmospheres.
We aim to calculate new Sr IV - VII oscillator strengths to identify for the
first time Sr spectral lines in hot white dwarf (WD) stars and to determine the
photospheric Sr abundances. o measure the abundances of Se, Te, and I in hot
WDs, we aim to compute new Se V, Te VI, and I VI oscillator strengths.
To consider radiative and collisional bound-bound transitions of Se V, Sr IV
- VII, Te VI, and I VI in our NLTE atmosphere models, we calculated oscillator
strengths for these ions.
We newly identified four Se V, 23 Sr V, 1 Te VI, and three I VI lines in the
ultraviolet (UV) spectrum of RE0503-289. We measured a photospheric Sr
abundance of 6.5 +3.8/-2.4 x 10**-4 (mass fraction, 9500 - 23800 times solar).
We determined the abundances of Se (1.6 +0.9/-0.6 x 10**-3, 8000 - 20000), Te
(2.5 +1.5/-0.9 x 10**-4, 11000 - 28000), and I (1.4 +0.8/-0.5 x 10**-5, 2700 -
6700). No Se, Sr, Te, and I line was found in the UV spectra of G191-B2B and we
could determine only upper abundance limits of approximately 100 times solar.
All identified Se V, Sr V, Te VI, and I VI lines in the UV spectrum of
RE0503-289 were simultaneously well reproduced with our newly calculated
oscillator strengths.Comment: 26 pages, 5 figure
Understanding Preservation Theorems, II
This is an exposition of much of Sections VI.3 and XVIII.3 of "Proper and
Improper Forcing", including preservations for "no random reals over V", "reals
of V form a non-meager set", "every dense open set contains a dense open set in
V", weak bounding, and weak -bounding. The current version of
part I covering Sections VI.1 and VI.2 is available from the author.Comment: To appear in ML
Model for processive movement of myosin V and myosin VI
Myosin V and myosin VI are two classes of two-headed molecular motors of the
myosin superfamily that move processively along helical actin filaments in
opposite directions. Here we present a hand-over-hand model for their
processive movements. In the model, the moving direction of a dimeric molecular
motor is automatically determined by the relative orientation between its two
heads at free state and its head's binding orientation on track filament. This
determines that myosin V moves toward the barbed end and myosin VI moves toward
the pointed end of actin. During the moving period in one step, one head
remains bound to actin for myosin V whereas two heads are detached for myosin
VI: The moving manner is determined by the length of neck domain. This
naturally explains the similar dynamic behaviors but opposite moving directions
of myosin VI and mutant myosin V (the neck of which is truncated to only
one-sixth of the native length). Because of different moving manners, myosin VI
and mutant myosin V exhibit significantly broader step-size distribution than
native myosin V. However, all three motors give the same mean step size of 36
nm (the pseudo-repeat of actin helix). Using the model we study the dynamics of
myosin V quantitatively, with theoretical results in agreement with previous
experimental ones.Comment: 18 pages, 7 figure
Metal-Oxo Photo-oxidants, Photochemistry and Photophysics of trans-[Os^(VI)(tmc)(O)_2]^(2+)(tmc = 1,4,8,11-tetramethyl-1,4,8,11-tetra-azacyclotetradecane) and trans-[Os^(VI)(CN)_4(O)_2]^(2-)
trans-[Os^(VI)(tmc)(O)_2]^(2+)(tmc = 1,4,8,11-tetramethyl-1,4,8,11-tetra-azacyclotetradecane) and trans-[Os^(VI)(CN)_4(O)_2]^(2-) are emissive in the solid state and in fluid solutions at room temperature (τ~ 1.0–1.5 µs); the (^3)E_g state of trans-[Os^(VI)(tmc)(O)_2]^(2+) is a powerful one-electron oxidant {[Os^(VI)(O)_2]^(2+) + e^– → [Os^V (O)_2]+, E^0_f > 2.0 V vs. normal hydrogen electrode} in aqueous solution, reacting with PPh3 and ((PhCH_2)_2)S to give O=PPh_3 and ((PhCH_2)_2)S=O, respectively
Nonlinear Spinor Fields and its role in Cosmology
Different characteristic of matter influencing the evolution of the Universe
has been simulated by means of a nonlinear spinor field. Exploiting the spinor
description of perfect fluid and dark energy evolution of the Universe given by
an anisotropic Bianchi type-VI, VI, V, III, I or isotropic
Friedmann-Robertson-Walker (FRW) one has been studied. It is shown that due to
some restrictions on metric functions, initial anisotropy in the models Bianchi
type-VI, VI, V and III does not die away, while the anisotropic Bianchi
type-I models evolves into the isotropic one.Comment: 22 pages, 12 Figure
The Ratio of Total to Selective Extinction Toward Baade's Window
We measure the ratio of total to selective extinction, R_{VI}=A_V/E(V-I),
toward Baade's Window by comparing the VIK colors of 132 Baade's Window G and K
giants from Tiede, Frogel, & Terndrup with the solar-neighborhood (V-I),(V-K)
relation from Bessell & Brett. We find R_{VI}=2.283 +/- 0.016, and show that
our measurement has no significant dependence on stellar type from G0 to K4.
Adjusting the Paczynski et al. determination of the centroid of the dereddened
Baade's Window clump for this revised value of , we find I_{0,RC}=14.43
and (V-I)_{0,RC}=1.058. This implies a distance to the Baade's Window clump of
d_{BW} = 8.63 +/- 0.16 kpc, where the error bar takes account of statistical
but not systematic uncertainties.Comment: 8 pages, 1 figure, submitted to Ap
Strong Correlations in Actinide Redox Reactions
Reduction-oxidation (redox) reactions of the redox couples An(VI)/An(V),
An(V)/An(IV), and An(IV)/An(III), where An is an element in the family of early
actinides (U, Np, and Pu), as well as Am(VI)/Am(V) and Am(V)/Am(III), are
modeled by combining density functional theory with a generalized Anderson
impurity model that accounts for the strong correlations between the 5f
electrons. Diagonalization of the Anderson impurity model yields improved
estimates for the redox potentials and the propensity of the actinide complexes
to disproportionate.Comment: 17 pages, 10 figure, 3 tables. Corrections and clarifications; this
version has been accepted for publication in The Journal of Chemical Physic
Stellar laboratories: new Ge V and Ge VI oscillator strengths and their validation in the hot white dwarf RE 0503-289
State-of-the-art spectral analysis of hot stars by means of non-LTE
model-atmosphere techniques has arrived at a high level of sophistication. The
analysis of high-resolution and high-S/N spectra, however, is strongly
restricted by the lack of reliable atomic data for highly ionized species from
intermediate-mass metals to trans-iron elements. Especially data for the latter
has only been sparsely calculated. Many of their lines are identified in
spectra of extremely hot, hydrogen-deficient post-AGB stars. A reliable
determination of their abundances establishes crucial constraints for AGB
nucleosynthesis simulations and, thus, for stellar evolutionary theory.
In a previous analysis of the UV spectrum of RE 0503-289, spectral lines of
highly ionized Ga, Ge, As, Se, Kr, Mo, Sn, Te, I, and Xe were identified.
Individual abundance determinations are hampered by the lack of reliable
oscillator strengths. Most of these identified lines stem from Ge V. In
addition, we identified Ge VI lines for the first time. We calculated Ge V and
Ge VI oscillator strengths to consider their radiative and collisional
bound-bound transitions in detail in our non-LTE stellar-atmosphere models for
the analysis of the Ge IV - VI spectrum exhibited in high-resolution and
high-S/N UV spectra of RE 0503-289. We identify four Ge IV, 37 Ge V, and seven
Ge VI lines. Most of these are identified for the first time in any star. We
reproduce almost all Ge IV, Ge VI, and Ge VI lines in the observed spectrum of
RE 0503-289 (Teff = 70 kK, log g = 7.5) at log Ge = -3.8 +/- 0.3 (mass
fraction, about 650 times solar).
Reliable measurements and calculations of atomic data are a prerequisite for
stellar-atmosphere modeling. Our oscillator-strength calculations have allowed,
for the first time, Ge V and Ge VI lines to be successfully reproduced in a
white dwarf's spectrum and to determine its photospheric Ge abundance.Comment: 54 pages, 8 figure
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