58,164 research outputs found
Test of shell-model interactions for nuclear structure calculations
The binding energy and excitation spectra of 6Li are calculated in a no-core shell-model space giving encouraging results. The results of this calculation are then treated as a theoretical experiment, against which different effective-interaction approximations are compared. In this way insight into the perturbation expansion for the effective interaction is obtained
Agterberg, Zheng, and Mukherjee Reply
Reply to Ikeda (arXiv:0712.3341).Comment: To appear in Phys. Rev. Let
Quantum computing through electron propagation in the edge states of quantum spin Hall systems
We propose to implement quantum computing based on electronic spin qubits by
controlling the propagation of the electron wave packets through the helical
edge states of quantum spin Hall systems (QSHs). Specfically, two
non-commutative single-qubit gates, which rotate a qubit around z and y axes,
can be realized by utilizing gate voltages either on a single QSH edge channel
or on a quantum point contact structure. The more challenging two-qubit
controlled phase gate can be implemented through the on-demand capacitive
Coulomb interaction between two adjacent edge channels from two parallel QSHs.
As a result, a universal set of quantum gates can be achieved in an
all-electrical way. The fidelity and purity of the two-qubit gate are
calculated with both time delay and finite width of the wave packets taken into
consideration, which can reach high values with the existing high-quality
single electron source
Networking Effects on Cooperation in Evolutionary Snowdrift Game
The effects of networking on the extent of cooperation emerging in a
competitive setting are studied. The evolutionary snowdrift game, which
represents a realistic alternative to the well-known Prisoner's Dilemma, is
studied in the Watts-Strogatz network that spans the regular, small-world, and
random networks through random re-wiring. Over a wide range of payoffs, a
re-wired network is found to suppress cooperation when compared with a
well-mixed or fully connected system. Two extinction payoffs, that characterize
the emergence of a homogeneous steady state, are identified. It is found that,
unlike in the Prisoner's Dilemma, the standard deviation of the degree
distribution is the dominant network property that governs the extinction
payoffs.Comment: Changed conten
Scattering and Blow up for the Two Dimensional Focusing Quintic Nonlinear Schr\"odinger Equation
Using the concentration-compactness method and the localized virial type
arguments, we study the behavior of solutions to the focusing quintic NLS
in , namely,
Denoting by and , the mass and energy of a solution
respectively, and the ground state solution to , and
assuming , we characterize the threshold for global versus
finite time existence. Moreover, we show scattering for global existing time
solutions and finite or "weak" blow up for the complement region. This work is
in the spirit of Kenig and Merle and Duyckaerts, Holmer, and Roudenko.Comment: 37 pages, 2 figures and updated reference
Cosmic clocks: A Tight Radius - Velocity Relationship for HI-Selected Galaxies
HI-Selected galaxies obey a linear relationship between their maximum
detected radius Rmax and rotational velocity. This result covers measurements
in the optical, ultraviolet, and HI emission in galaxies spanning a factor of
30 in size and velocity, from small dwarf irregulars to the largest spirals.
Hence, galaxies behave as clocks, rotating once a Gyr at the very outskirts of
their discs. Observations of a large optically-selected sample are consistent,
implying this relationship is generic to disc galaxies in the low redshift
Universe. A linear RV relationship is expected from simple models of galaxy
formation and evolution. The total mass within Rmax has collapsed by a factor
of 37 compared to the present mean density of the Universe. Adopting standard
assumptions we find a mean halo spin parameter lambda in the range 0.020 to
0.035. The dispersion in lambda, 0.16 dex, is smaller than expected from
simulations. This may be due to the biases in our selection of disc galaxies
rather than all halos. The estimated mass densities of stars and atomic gas at
Rmax are similar (~0.5 Msun/pc^2) indicating outer discs are highly evolved.
The gas consumption and stellar population build time-scales are hundreds of
Gyr, hence star formation is not driving the current evolution of outer discs.
The estimated ratio between Rmax and disc scale length is consistent with
long-standing predictions from monolithic collapse models. Hence, it remains
unclear whether disc extent results from continual accretion, a rapid initial
collapse, secular evolution or a combination thereof.Comment: 14 pages, 7 figures, 3 in colour. Published in MNRAS. This v2
corrects wrong journal in the references section (all instances of
"Astrophysics and Space Sciences" should have been ApJ). The Posti+2017 has
also been updated. An erratum has been submitted to MNRA
Magnetic coupling of a rotating black hole with its surrounding accretion disk
Effects of magnetic coupling (MC) of a rotating black hole (BH) with its
surrounding accretion disk are discussed in detail in the following aspects:
(i) The mapping relation between the angular coordinate on the BH horizon and
the radial coordinate on the disk is modified based on a more reasonable
configuration of magnetic field, and a condition for coexistence of the
Blandford-Znajek (BZ) and the MC process is derived. (ii) The transfer
direction of energy and angular momentum in MC process is described
equivalently by the co-rotation radius and by the flow of electromagnetic
angular momentum and redshifted energy, where the latter is based on an
assumption that the theory of BH magnetosphere is applicable to both the BZ and
MC processes. (iii) The profile of the current on the BH horizon and that of
the current density flowing from the magnetosphere onto the horizon are given
in terms of the angular coordinate of the horizon. It is shown that the current
on the BH horizon varies with the latitude of the horizon and is not continuous
at the angular boundary between the open and closed magnetic field lines. (iv)
The MC effects on disk radiation are discussed, and a very steep emissivity is
produced by MC process, which is consistent with the recent XMM-Newton
observation of the nearby bright Seyfert 1 galaxy MCG-6-30-15 by a variety of
parameters of the BH-disk system.Comment: 24 pages, 19 figures. Accepted by Ap
M Dwarfs from Hubble Space Telescope Star Counts. IV
We study a sample of about 1400 disk M dwarfs that are found in 148 fields
observed with the Wide Field Camera 2 (WFC2) on the Hubble Space Telescope and
162 fields observed with pre-repair Planetary Camera 1 (PC1), of which 95 of
the WFC2 fields are newly analyzed. The method of maximum likelihood is applied
to derive the luminosity function and the Galactic disk parameters. At first,
we use a local color-magnitude relation and a locally determined
mass-luminosity relation in our analysis. The results are consistent with those
of previous work but with considerably reduced statistical errors. These small
statistical errors motivate us to investigate the systematic uncertainties.
Considering the metallicity gradient above the Galactic plane, we introduce a
modified color-magnitude relation that is a function of Galactic height. The
resultant M dwarf luminosity function has a shape similar to that derived using
the local color-magnitude relation but with a higher peak value. The peak
occurs at and the luminosity function drops sharply toward . We then apply a height-dependent mass-luminosity function
interpolated from theoretical models with different metallicities to calculate
the mass function. Unlike the mass function obtained using local relations,
which has a power-law index , the one derived from the
height-dependent relations tends to be flat (). The resultant
local surface density of disk M dwarfs (12.2 +/- 1.6 M_sun pc^{-2}) is somewhat
smaller than the one obtained using local relations (14.3 +/- 1.3 M_sun
pc^{-2}). Our measurement favors a short disk scale length, H = 2.75 +/- 0.16
(statistical) +/- 0.25 (systematic) kpc.Comment: 20 pages, 10 ps figures, accepted for publication in Ap
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