5,241 research outputs found
Locating the magnetospheric ring current
Protons are studied in the global depression of the earth's horizontal magnetic field. It is shown that 10 to 100 keV protons dominate ring current energetics in two preferred regions of cyclotron instability, which serve as stable trapping boundaries for ring current protons. The only apparent means of removing this stably trapped belt of particles are considered to be by charge exchange interactions, or by outward expansion of the plasmapause to erode the ring current. Both of these processes require about two days, which is the characteristic decay period of the main phase depression. Questions whose answers are necessary to formulate a quantitative theory of geomagnetic storms which relates main phase depression to solar wind parameters are included
Unstable growth of unducted whistlers propagating at an angle to the geomagnetic field
Unstable growth rate of unducted whistler waves propagating at angle to geomagnetic fiel
Parton Distributions
I discuss our current understanding of parton distributions. I begin with the
underlying theoretical framework, and the way in which different data sets
constrain different partons, highlighting recent developments. The methods of
examining the uncertainties on the distributions and those physical quantities
dependent on them is analysed. Finally I look at the evidence that additional
theoretical corrections beyond NLO perturbative QCD may be necessary, what type
of corrections are indicated and the impact these may have on the
uncertainties.Comment: Invited talk at "XXI International Symposium on Lepton and Photon
Interactions at High Energies," (Fermilab, Chicago, August 2003). 12 pages,
21 figure
Results of B0s → CP eigenstates at Belle
We report the measurement of the absolute branching fraction for B0s → J/ψ φ, for B0s → J/ψ K+K− and a determination of the s-wave contribution in the φ mass range as well as a first observation of B0s → J/ψ η and B0s
→ J/ψ η'. These results are based on a 121 fb−1 data sample collected with the Belle detector
at the KEK-B asymmetric e+e− collider near the Υ(5S) resonance
Event Horizon Deformations in Extreme Mass-Ratio Black Hole Mergers
We study the geometry of the event horizon of a spacetime in which a small
compact object plunges into a large Schwarzschild black hole. We first use the
Regge-Wheeler and Zerilli formalisms to calculate the metric perturbations
induced by this small compact object, then find the new event horizon by
propagating null geodesics near the unperturbed horizon. A caustic is shown to
exist before the merger. Focusing on the geometry near the caustic, we show
that it is determined predominantly by large-l perturbations, which in turn
have simple asymptotic forms near the point at which the particle plunges into
the horizon. It is therefore possible to obtain an analytic characterization of
the geometry that is independent of the details of the plunge. We compute the
invariant length of the caustic. We further show that among the leading-order
horizon area increase, half arises from generators that enter the horizon
through the caustic, and the rest arises from area increase near the caustic,
induced by the gravitational field of the compact object.Comment: 23 pages, 14 figure
Mitochondrial Dna Replacement Versus Nuclear Dna Persistence
In this paper we consider two populations whose generations are not
overlapping and whose size is large. The number of males and females in both
populations is constant. Any generation is replaced by a new one and any
individual has two parents for what concerns nuclear DNA and a single one (the
mother) for what concerns mtDNA. Moreover, at any generation some individuals
migrate from the first population to the second.
In a finite random time , the mtDNA of the second population is completely
replaced by the mtDNA of the first. In the same time, the nuclear DNA is not
completely replaced and a fraction of the ancient nuclear DNA persists. We
compute both and . Since this study shows that complete replacement of
mtDNA in a population is compatible with the persistence of a large fraction of
nuclear DNA, it may have some relevance for the Out of Africa/Multiregional
debate in Paleoanthropology
Shell sources as a probe of relativistic effects in neutron star models
A perturbing shell is introduced as a device for studying the excitation of
fluid motions in relativistic stellar models. We show that this approach allows
a reasonably clean separation of radiation from the shell and from fluid
motions in the star, and provides broad flexibility in the location and
timescale of perturbations driving the fluid motions. With this model we
compare the relativistic and Newtonian results for the generation of even
parity gravitational waves from constant density models. Our results suggest
that relativistic effects will not be important in computations of the
gravitational emission except possibly in the case of excitation of the neutron
star on very short time scales.Comment: 16 pages LaTeX with 6 eps figures; submitted to Phys. Rev.
Gravitating Fluxbranes
We consider the effect that gravity has when one tries to set up a constant
background form field. We find that in analogy with the Melvin solution, where
magnetic field lines self-gravitate to form a flux-tube, the self-gravity of
the form field creates fluxbranes. Several exact solutions are found
corresponding to different transverse spaces and world-volumes, a dilaton
coupling is also considered.Comment: 14 pages, 5 figure
On the Solution to the "Frozen Star" Paradox, Nature of Astrophysical Black Holes, non-Existence of Gravitational Singularity in the Physical Universe and Applicability of the Birkhoff's Theorem
Oppenheimer and Snyder found in 1939 that gravitational collapse in vacuum
produces a "frozen star", i.e., the collapsing matter only asymptotically
approaches the gravitational radius (event horizon) of the mass, but never
crosses it within a finite time for an external observer. Based upon our recent
publication on the problem of gravitational collapse in the physical universe
for an external observer, the following results are reported here: (1) Matter
can indeed fall across the event horizon within a finite time and thus BHs,
rather than "frozen stars", are formed in gravitational collapse in the
physical universe. (2) Matter fallen into an astrophysical black hole can never
arrive at the exact center; the exact interior distribution of matter depends
upon the history of the collapse process. Therefore gravitational singularity
does not exist in the physical universe. (3) The metric at any radius is
determined by the global distribution of matter, i.e., not only by the matter
inside the given radius, even in a spherically symmetric and pressureless
gravitational system. This is qualitatively different from the Newtonian
gravity and the common (mis)understanding of the Birkhoff's Theorem. This
result does not contract the "Lemaitre-Tolman-Bondi" solution for an external
observer.Comment: 8 pages, 4 figures, invited plenary talk at "The first Galileo-Xu
Guangqi conference", Shanghai, China, 2009. To appear in International
Journal of Modern Physics D (2010
Components of the gravitational force in the field of a gravitational wave
Gravitational waves bring about the relative motion of free test masses. The
detailed knowledge of this motion is important conceptually and practically,
because the mirrors of laser interferometric detectors of gravitational waves
are essentially free test masses. There exists an analogy between the motion of
free masses in the field of a gravitational wave and the motion of free charges
in the field of an electromagnetic wave. In particular, a gravitational wave
drives the masses in the plane of the wave-front and also, to a smaller extent,
back and forth in the direction of the wave's propagation. To describe this
motion, we introduce the notion of `electric' and `magnetic' components of the
gravitational force. This analogy is not perfect, but it reflects some
important features of the phenomenon. Using different methods, we demonstrate
the presence and importance of what we call the `magnetic' component of motion
of free masses. It contributes to the variation of distance between a pair of
particles. We explicitely derive the full response function of a 2-arm laser
interferometer to a gravitational wave of arbitrary polarization. We give a
convenient description of the response function in terms of the spin-weighted
spherical harmonics. We show that the previously ignored `magnetic' component
may provide a correction of up to 10 %, or so, to the usual `electric'
component of the response function. The `magnetic' contribution must be taken
into account in the data analysis, if the parameters of the radiating system
are not to be mis-estimated.Comment: prints to 29 pages including 9 figures, new title, additional
explanations and references in response to referee's comments, to be
published in Class. Quant. Gra
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