Energy-dependent orbital modulation of X-rays and constraints on emission of the jet in Cyg X-3

The orbital modulation of the X-ray and radio emission of Cyg X-3 was studied using monitoring data from CGRO/BATSE, RXTE/ASM, GBI and the Ryle telescope as well as recent INTEGRAL observations. The depth of the X-ray modulation was found to be the same at X-ray energies ranging from 1.5 up to at least 20 keV, but the shape of the lightcurves changes gradually with energy. No modulation was found in radio.

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Magnetic X-Ray Circular Dichroism in Spin-Polarized Photoelectron Diffraction

MRS Proceedings ◽

10.1557/proc-375-101 ◽

1994 ◽

Vol 375 ◽

Author(s):

G. D. Waddill ◽

J. G. Tobin ◽

X. Guo ◽

S. Y. Tong

Keyword(s):

Magnetic Structure ◽

Multiple Scattering ◽

Analytical Procedure ◽

Structural Determination ◽

X Rays ◽

Circularly Polarized ◽

X Ray ◽

Photoelectron Diffraction ◽

Spin Polarized ◽

Energy Dependent

AbstractThe first structural determination with spin-polarized, energy-dependent photoelectron diffraction using circularly-polarized x-rays is reported for Fe films on Cu(001). Circularly-polarized x-rays produce spin-polarized photoelectrons from the Fe 2p doublet, and intensity asymmetries in the 2p3/2 level are observed. Fully spin-specific multiple scattering calculations reproduce the experimentally-determined energy and angular dependences. A new analytical procedure which focuses upon intensity variations due to spin-dependent diffraction is introduced. A sensitivity to local geometric and magnetic structure is demonstrated.

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New Symbiotic Stars Monitored with the Hermes Spectrograph: A Case Study of Orbital Hα Modulation

Open Astronomy ◽

10.1515/astro-2017-0356 ◽

2012 ◽

Vol 21 (1-2) ◽

Author(s):

Alain Jorissen ◽

S. Van Eck ◽

T. Dermine ◽

H. Van Winckel ◽

N. Gorlova

Keyword(s):

X Rays ◽

Mass Ratio ◽

Orbital Elements ◽

Broad Emission ◽

Short Period ◽

Hα Emission ◽

Orbital Modulation ◽

Symbiotic Binaries ◽

Narrow Emission

AbstractWe present new orbital elements for two symbiotic systems involving a giant of spectral type S, namely V420 Hya and ER Del. These orbital elements are compared with existing elements for S-type binaries and for symbiotic binaries with M-giant primaries. It is shown that among the S-type binaries, most of the short-period systems (with P in the range 300 - 1000 d) exhibit some kind of symbiotic activity (Hα emission, UV continuum, hard X-rays), but symbiotic systems are not restricted to the short-period systems. the complex and varying Hα profile of V420 Hya has been decomposed to several components (broad emission with σ ~ 140 km/s, narrow emission with σ ~ 60 km/s, and narrow absorption components). Their orbital modulation reveals that the broad emission is located close to the companion (under the hypothesis of a system with a mass ratio M

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Dependence of the orbital modulation of X-rays from 4U 1820-303 on the accretion rate

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2007.11688.x ◽

2007 ◽

Vol 377 (3) ◽

pp. 1017-1023 ◽

Cited By ~ 19

Author(s):

A. A. Zdziarski ◽

M. Gierlinski ◽

L. Wen ◽

Z. Kostrzewa

Keyword(s):

Accretion Rate ◽

X Rays ◽

Orbital Modulation

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The Hϒ Line Spectrum of Intermediate Polars

Highlights of Astronomy ◽

10.1017/s1539299600021353 ◽

1998 ◽

Vol 11 (1) ◽

pp. 385-385

Author(s):

Y. Kim ◽

K. Beuermann

Keyword(s):

Spectral Range ◽

Line Spectrum ◽

Model Parameters ◽

X Rays ◽

X Ray ◽

Rotational Modulation ◽

Intermediate Polars ◽

Dominant Process ◽

Energy Dependent ◽

Insight Into

By using of a model for the propagation of the emitted X-rays through the infalling material and the reemission of the energy deposited by photoabsorption in the optical (and UV) spectral range (Kim & Beuermann, 1995) we calculated Hϒ line spectrum of intermediate polars. Photoabsorption of X-rays by the infalling material is the dominant process in forming the observed energy-dependent rotational modulation of the X-ray flux. X-ray and optical modulations are sensitive to model parameters in different ways. In principle these dependences allow us to obtain improved insight into the geometry of intermediate polars. Some results of our calculation will be presented in this paper in comparison with the Hβ spectrum calculated by Kim & Beuermann (1996).

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Study of energy dependent behaviour of half-lens polycapillary optics using synchrotron x-rays

10.1063/5.0017646 ◽

2020 ◽

Author(s):

Ayushi Trivedi ◽

Ajay Khooha ◽

P. Mondal ◽

S. R. Kane ◽

M. K. Tiwari

Keyword(s):

X Rays ◽

Polycapillary Optics ◽

Energy Dependent ◽

Dependent Behaviour

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Modelling Photoelectron Effects In X-Ray Lithography

MRS Proceedings ◽

10.1557/proc-306-47 ◽

1993 ◽

Vol 306 ◽

Cited By ~ 3

Author(s):

L. E. Ocola ◽

F. Cerrina

Keyword(s):

Monte Carlo ◽

Spatial Distribution ◽

Kinetic Energy ◽

Monte Carlo Simulations ◽

Energy Range ◽

X Rays ◽

X Ray ◽

Atomic Species ◽

Energy Dependent ◽

X Ray Absorption

AbstractThe study of photoelectron effects in X-ray Lithography motivates the need for modeling codes to simulate these effects to have an estimate of the influence of x-ray generated photoelectrons in the exposure of resists. We have performed a series of Monte Carlo simulations to study the spatial distribution of photoelectrons in a resist, PMMA, and parametrized this distribution with a set of energy-dependent gaussians for monochromatic X-rays within an energy range of 0.5 KeV to 2.5 KeV. We discuss the effects of the the redistribution of the photoelectron kinetic energy as a function of the electrons generated by the x-ray absorption in various atomic species.

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ROSAT observations of non-magnetic CVs

International Astronomical Union Colloquium ◽

10.1017/s0252921100038847 ◽

1996 ◽

Vol 158 ◽

pp. 273-276 ◽

Cited By ~ 2

Author(s):

A. van Teeseling ◽

F. Verbunt ◽

K. Beuermann

Keyword(s):

Boundary Layer ◽

Accretion Disk ◽

White Dwarf ◽

Accretion Rate ◽

Cataclysmic Variables ◽

Rotation Velocity ◽

X Rays ◽

X Ray ◽

Orbital Modulation ◽

Magnetic Cataclysmic Variables

In non-magnetic cataclysmic variables the accreted matter forms an accretion disk around the white dwarf. In the boundary layer between the white dwarf and the accretion disk the accreted matter decelerates from Keplerian velocities to the rotation velocity of the white dwarf. If the accretion rate is high the boundary layer would be optically thick and cool (T ~ 105K), and if the accretion rate is low the boundary layer would be optically thin and hot (T ~ 108K) (Pringle & Savonije 1979).There are several observational problems with this simple picture: a soft X-ray component could only be detected so far in 5 dwarf novae in outburst and not in any nova-like variable. Also in high-accretion-rate systems there is a hot optically thin X-ray source, which has, however, an X-ray luminosity which is much less than the UV luminosity of the system (van Teeseling & Verbunt 1994). Finally, there is evidence for orbital modulation in the X-rays from some systems (e.g. van Teeseling et al. 1995).

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