31 research outputs found
The Transition Zone in Balmer-Dominated Shocks
We examine the structure of the post-shock region in supernova remnants
(SNRs). The ``shock transition zone'' is set up by charge transfer and
ionization events between atoms and ions, and has a width
cm , where is the total pre-shock density (including
both atoms and ions). For Balmer-dominated SNRs with shock velocity km s, the Rankine-Hugoniot conditions for ion velocity and
temperature are obeyed instantly, leaving the full width at half-maximum (FWHM)
of the broad H line versus relation intact. However, the spatial
variation in the post-shock densities is relevant to the problem of Ly
resonant scattering in young, core-collapse SNRs. Both two- (pre-shock atoms
and ions) and three-component (pre-shock atoms, broad neutrals and ions) models
are considered. We compute the spatial emissivities of the broad () and
narrow () H lines; a calculation of these emissivities in SN
1006 is in general agreement with the computed ones of Raymond et al. (2007).
The (dimensionless) spatial shift, , between the centroids
of and is unique for a given shock velocity and ,
the pre-shock ion fraction. Measurements of can be used
to constrain .Comment: 25 pages, 8 figures. Accepted by Astrophysical Journa
Thermal Radiation from Isolated Neutron Stars: Spectra and Polarizations
Recent observations of surface emission from isolated neutron stars (NSs) provide unique challenges to theoretical modeling of thermal radiative processes. We construct models of thermal emission from strongly magnetized NSs in which the outermost layer of the NS is in a condensed liquid or solid form, or is an ionized H or He atmosphere.
We calculate the emission properties (spectrum and polarization) of NSs with condensed Fe and H surfaces using a generalized form of Kirchhoff's Law, in the regimes where condensation may be possible. For smooth condensed surfaces, the overall emission is reduced from blackbody by less than a factor of two. The spectrum exhibits modest deviation from blackbody across a wide energy range, and shows mild absorption features associated with the electron plasma and ion cyclotron frequencies in the condensed matter. The roughness of the solid Fe condensate decreases the reflectivity of the surface, making the emission spectrum even closer to blackbody.
We provide an accurate treatment of vacuum polarization effects in magnetized NS atmosphere models. We treat the conversion of photon modes (due to ``vacuum resonance'' between plasma and vacuum polarizations), employing both the modal radiative transfer equations (coupled with an accurate mode conversion probability at the vacuum resonance) and the full radiative transfer equations for the photon Stokes parameters. We are able to quantitatively calculate the atmosphere structure, emission spectra, beam patterns, and polarizations for the range of magnetic field strengths G. In agreement with previous studies, we find that for NSs with magnetic field strengths B/2 \ga B_l\simeq 7\times 10^{13} G, vacuum polarization reduces the widths of spectral features and softens the hard tail of magnetized atmosphere models. For B\la B_l/2, vacuum polarization does not change the emission spectra, but can affect the polarization signals.
We investigate the propagation of photon polarization in NS magnetospheres, and show that vacuum polarization induces a unique energy-dependent linear polarization signature, and can generate circular polarization in the magnetospheres of rapidly rotating NSs. We discuss the implications of our results for observations of thermally emitting isolated NSs and magnetars, and the prospects for future spectral and polarization studies
Polarized X-rays from Magnetized Neutron Stars
We review the polarization properties of X-ray emission from highly
magnetized neutron stars, focusing on emission from the stellar surfaces. We
discuss how x-ray polarization can be used to constrain neutron star magnetic
field and emission geometry, and to probe strong-field quantum electrodynamics
and possibly constrain the properties of axions.Comment: to appear in "X-ray Polarimetry: A New Window in Astrophysics",
edited by R. Bellazzini, E. Costa, G. Matt and G. Tagliaferri (Cambridge
University Press
Soft X-ray Polarization in Thermal Magnetar Emission
Emission spectra from magnetars in the soft X-ray band likely contain a
thermal component emerging directly from the neutron star surface. However, the
lack of observed absorption-like features in quiescent spectra makes it
difficult to directly constrain physical properties of the atmosphere. We argue
that future X-ray polarization measurements represent a promising technique for
directly constraining the magnetar magnetic field strength and geometry. We
construct models of the observed polarization signal from a finite surface
hotspot, using the latest NS atmosphere models for magnetic fields B = 4 x
10^13--5 x 10^14 G. Our calculations are strongly dependent on the NS magnetic
field strength and geometry, and are more weakly dependent on the NS equation
of state and atmosphere composition. We discuss how the complementary
dependencies of phase-resolved spectroscopy and polarimetry might resolve
degeneracies that currently hamper the determination of magnetar physical
parameters using thermal models.Comment: 23 pages, 7 figures; MNRAS accepte
Spatial Structure and Collisionless Electron Heating in Balmer-dominated Shocks
Balmer-dominated shocks in supernova remnants (SNRs) produce strong hydrogen
lines with a two-component profile composed of a narrow contribution from cold
upstream hydrogen atoms, and a broad contribution from hydrogen atoms that have
undergone charge transfer reactions with hot protons. Observations of emission
lines from edge-wise shocks in SNRs can constrain the gas velocity and
collisionless electron heating at the shock front. Downstream hydrogen atoms
engage in charge transfer, excitation and ionization reactions, defining an
interaction region called the shock transition zone. The properties of hot
hydrogen atoms produced by charge transfers (called broad neutrals) are
critical for accurately calculating the structure and radiation from the shock
transition zone. This paper is the third in a series describing the kinetic,
fluid and emission properties of Balmer-dominated shocks, and is the first to
properly treat the effect of broad neutral kinetics on shock transition zone
structure. We use our models to extract shock parameters from observations of
Balmer-dominated SNRs. We find that inferred shock velocities and electron
temperatures are lower than those of previous calculations by <10% for v_s<1500
km/s, and by 10-30% for v_s>1500 km/s. This effect is primarily due to the fact
that excitation by proton collisions and charge transfer to excited levels
favor the high speed part of the neutral hydrogen velocity distribution. Our
results have a strong dependence on the ratio of electron to proton
temperatures, \beta=T_e/T_p, which allows us to construct a relation \beta(v_s)
between the temperature ratio and shock velocity. We compare our calculations
to previous results by Ghavamian et al. (2007).Comment: 41 pages, 15 figures, 2 tables. Improved comparison to previous
results, added discussion, and incorporated referee's suggestions. Submitted
to Ap
Radiation from condensed surface of magnetic neutron stars
Recent observations show that the thermal X-ray spectra of many isolated
neutron stars are featureless and in some cases (e.g., RX J1856.5-3754) well
fit by a blackbody. Such a perfect blackbody spectrum is puzzling since
radiative transport through typical neutron star atmospheres causes noticeable
deviation from blackbody. Previous studies have shown that in a strong magnetic
field, the outermost layer of the neutron star may be in a condensed solid or
liquid form because of the greatly enhanced cohesive energy of the condensed
matter. The critical temperature of condensation increases with the magnetic
field strength, and can be as high as 10^6 K (for Fe surface at B \sim 10^{13}
G or H surface at B \sim a few times 10^{14} G). Thus the thermal radiation can
directly emerge from the degenerate metallic condensed surface, without going
through a gaseous atmosphere. Here we calculate the emission properties
(spectrum and polarization) of the condensed Fe and H surfaces of magnetic
neutron stars in the regimes where such condensation may be possible. For a
smooth condensed surface, the overall emission is reduced from the blackbody by
less than a factor of 2. The spectrum exhibits modest deviation from blackbody
across a wide energy range, and shows mild absorption features associated with
the ion cyclotron frequency and the electron plasma frequency in the condensed
matter. The roughness of the solid condensate (in the Fe case) tends to
decrease the reflectivity of the surface, and make the emission spectrum even
closer to blackbody. We discuss the implications of our results for
observations of dim, isolated neutron stars and magnetars.Comment: 12 pages, 11 figures. ApJ, accepted (final version; eq.(3) corrected
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Magnetic Hydrogen Atmosphere Models and the Neutron Star RX J1856.5-3754
RX J1856.5-3754 is one of the brightest nearby isolated neutron stars, and considerable observational resources have been devoted to it. However, current models are unable to satisfactorily explain the data. We show that our latest models of a thin, magnetic, partially ionized hydrogen atmosphere on top of a condensed surface can fit the entire spectrum, from X-rays to optical, of RX J1856.5-3754, within the uncertainties. In our simplest model, the best-fit parameters are an interstellar column density N{sub H} {approx} 1 x 10{sup 20} cm{sup -2} and an emitting area with R{sup {infinity}} {approx} 17 km (assuming a distance to RX J1856.5-3754 of 140 pc), temperature T{sup {infinity}} {approx} 4.3 x 10{sup 5} K, gravitational redshift z{sub g} {approx} 0.22, atmospheric hydrogen column y{sub H} {approx} 1 g cm{sup -2}, and magnetic field B {approx} (3-4) x 10{sup 12} G; the values for the temperature and magnetic field indicate an effective average over the surface. We also calculate a more realistic model, which accounts for magnetic field and temperature variations over the neutron star surface as well as general relativistic effects, to determine pulsations; we find there exist viewing geometries that produce pulsations near the currently observed limits. The origin of the thin atmospheres required to fit the data is an important question, and we briefly discuss mechanisms for producing these atmospheres. Our model thus represents the most self-consistent picture to date for explaining all the observations of RX J1856.5-3754
XIPE: the X-ray Imaging Polarimetry Explorer
X-ray polarimetry, sometimes alone, and sometimes coupled to spectral and
temporal variability measurements and to imaging, allows a wealth of physical
phenomena in astrophysics to be studied. X-ray polarimetry investigates the
acceleration process, for example, including those typical of magnetic
reconnection in solar flares, but also emission in the strong magnetic fields
of neutron stars and white dwarfs. It detects scattering in asymmetric
structures such as accretion disks and columns, and in the so-called molecular
torus and ionization cones. In addition, it allows fundamental physics in
regimes of gravity and of magnetic field intensity not accessible to
experiments on the Earth to be probed. Finally, models that describe
fundamental interactions (e.g. quantum gravity and the extension of the
Standard Model) can be tested. We describe in this paper the X-ray Imaging
Polarimetry Explorer (XIPE), proposed in June 2012 to the first ESA call for a
small mission with a launch in 2017 but not selected. XIPE is composed of two
out of the three existing JET-X telescopes with two Gas Pixel Detectors (GPD)
filled with a He-DME mixture at their focus and two additional GPDs filled with
pressurized Ar-DME facing the sun. The Minimum Detectable Polarization is 14 %
at 1 mCrab in 10E5 s (2-10 keV) and 0.6 % for an X10 class flare. The Half
Energy Width, measured at PANTER X-ray test facility (MPE, Germany) with JET-X
optics is 24 arcsec. XIPE takes advantage of a low-earth equatorial orbit with
Malindi as down-link station and of a Mission Operation Center (MOC) at INPE
(Brazil).Comment: 49 pages, 14 figures, 6 tables. Paper published in Experimental
Astronomy http://link.springer.com/journal/1068