948 research outputs found
Atmospheres and radiating surfaces of neutron stars
The early 21st century witnesses a dramatic rise in the study of thermal
radiation of neutron stars. Modern space telescopes have provided a wealth of
valuable information which, when properly interpreted, can elucidate the
physics of superdense matter in the interior of these stars. This
interpretation is necessarily based on the theory of formation of neutron star
thermal spectra, which, in turn, is based on plasma physics and on the
understanding of radiative processes in stellar photospheres. In this paper,
the current status of the theory is reviewed with particular emphasis on
neutron stars with strong magnetic fields. In addition to the conventional deep
(semi-infinite) atmospheres, radiative condensed surfaces of neutron stars and
"thin" (finite) atmospheres are considered.Comment: 43 pages, 13 figures, 1 table. In v.3, there are more than 50 minor
corrections (typos, wording, style) and one important typo fix (the sign in
Eq.(61)). In v.4, beside a few minor improvements, ionization equilibrium
equation (58) is corrected. In v.5, a typo in Eq.(12) is fixe
Hydrogen atom in a magnetic field: The quadrupole moment
The quadrupole moment of a hydrogen atom in a magnetic field for field
strengths from 0 to 4.414e13 G is calculated by two different methods. The
first method is variational, and based on a single trial function. The second
method deals with a solution of the Schroedinger equation in the form of a
linear combination of Landau orbitals.Comment: 4 pages, 1 figure, 1 table; RevTeX. Final (proofs-stage) version of
the text; corrected numbers in Table 1 and in Eq.(15
Comment on "On the ionization equilibrium of hot hydrogen plasma and thermodynamic consistency of formulating finite partition functions"
Zaghloul [Phys. Plasmas 17, 062701 (2010); arXiv:1010.1161v1] reconsiders the
occupation probability formalism in plasma thermodynamics and claims
inconsistencies in previous models. I show that the origin of this incorrect
claim is an omission of the configurational factor from the partition function.
This arXiv version is supplemented with two appendices, where I add remarks and
comments on two more recent publications of the same author on the same
subject: on his response to this Comment [Phys. Plasmas 17, 124705 (2010)] and
on his criticism towards the Hummer and Mihalas's (1988) formalism [Phys.
Plasmas 17, 122903 (2010); arXiv:1010.1102v1].Comment: 4 pages: 2 pages of the journal publication + 2 pages of the
electronic supplemen
Evolution of Young Neutron Star Envelopes
We extend our initial study of diffusive nuclear burning (DNB) for neutron
stars (NSs) with Hydrogen atmospheres and an underlying layer of proton
capturing nuclei. Our initial study showed that DNB can alter the photospheric
abundance of Hydrogen on surprisingly short timescales (10^{2-4}\yrs).
Significant composition evolution impacts the radiated thermal spectrum from
the NS as well as its overall cooling rate. In this paper, we consider the case
when the rate limiting step for the H consumption is diffusion to the burning
layer, rather than the local nuclear timescale. This is relevant for NSs with
surface temperatures in excess of , such as young ( yr)
radio pulsars and accreting NSs in quiescence. When downward diffusion is the
limiting rate in DNB, the rate of H consumption is suppressed by 1-2 orders of
magnitude compared to a DNB estimate that assumes diffusive equilibrium. In
order to apply our ongoing study to young neutron stars, we also include the
important effects of strong magnetic fields (). In this
initial study of magnetic modifications to DNB, we find that the H burning time
is lengthened by 2-3 orders of magnitude for a field.
However, even for NSs with dipole field strengths of G, we find that
all of the H can be burned before the pulsar reaches an age of $\sim 10^5 \
{\rm yr}$, thus potentially revealing the underlying proton-capturing elements.
Finally, we conclude by providing an overview of what can be learned about
fallback and pulsar winds from measuring the surface composition of a young NS.Comment: 10 pages, 8 figures, to appear in Ap
Dense astrophysical plasmas
We briefly examine the properties of dense plasmas characteristic of the
atmospheres of neutron stars and of the interior of massive white dwarfs. These
astrophysical bodies are natural laboratories to study respectively the problem
of pressure ionization of hydrogen in a strong magnetic field and the
crystallization of the quantum one-component-plasma at finite temperature.Comment: 8 pages, 3 figures, LaTeX using iopart.cls and iopart12.clo
(included). In the special issue "Liquid State Theory: from White Dwarfs to
Colloids" (International Conf. in the honor of Prof. J.-P. Hansen's 60th
birthday, Les Houches, April 1-5, 2002
Testing cosmological variability of fundamental constants
One of the topical problems of contemporary physics is a possible variability
of the fundamental constants. Here we consider possible variability of two
dimensionless constants which are most important for calculation of atomic and
molecular spectra (in particular, the X-ray ones): the fine-structure constant
\alpha=e^2/\hbar c and the proton-to-electron mass ratio \mu=m_p/m_e. Values of
the physical constants in the early epochs are estimated directly from
observations of quasars - the most powerful sources of radiation, whose spectra
were formed when the Universe was several times younger than now. A critical
analysis of the available results leads to the conclusion that present-day data
do not reveal any statistically significant evidence for variations of the
fundamental constants under study. The most reliable upper limits to possible
variation rates at the 95% confidence level, obtained in our work, read:
|\dot\alpha/\alpha| < (1.4e-14)/yr,
|\dot\mu/\mu| < (1.5e-14)/yr
on the average over the last ten billion years.Comment: 9 pages, 2 figures, 2 tables, LaTeX using aipproc.sty (included). In:
X-ray and Inner-Shell Processes, R.W. Dunford, D.S. Gemmel, E.P. Kanter, B.
Kraessig, S.H. Southworth, L. Young (eds.), AIP Conf. Proc. (AIP, Melville,
2000) vol. 506, p. 50
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