scholarly journals X-ray observations of the nova shell IPHASX J210204.7+471015*

2021 ◽  
Author(s):  
J A Toalá ◽  
G Rubio ◽  
E Santamaría ◽  
M A Guerrero ◽  
S Estrada-Dorado ◽  
...  
Keyword(s):  
Time Series ◽  
Binary System ◽  
Binary Star ◽  
Optical Observations ◽  
X Ray ◽  
Imaging Camera ◽  
Nova Shells ◽  
Intermediate Polars ◽  
Time Series Analyses ◽  
Nova Shell

Abstract We present the analysis of XMM-Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7+471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Her: an X-ray-emitting plasma with temperature of TX = (6.4 ± 3.1) × 106 K, a non-thermal X-ray component, and an estimated X-ray luminosity of LX = 1030 erg s−1. Time series analyses unveil the presence of two periods, the dominant with a period of 2.9 ± 0.2 hr, which might be attributed to the spin of the white dwarf, and a secondary of 4.5 ± 0.6 hr that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130–170 yr) or to its asymmetric disrupted morphology which is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions.

scholarly journals X-Ray and Optical Observations of a New X-Ray Soft Intermediate Polar: RX J0512.2–3241

1997 ◽  
Vol 163 ◽  
pp. 689-689
Author(s):  
V. Burwitz ◽  
K. Reinsch ◽  
K. Beuermann ◽  
H.-C. Thomas
Keyword(s):  
Optical Observations ◽  
Galactic Latitude ◽  
Ccd Photometry ◽  
X Ray ◽  
Probable Spin ◽  
Sky Survey ◽  
Intermediate Polars ◽  
Orbital Periods ◽  
Low Magnetic Field

The V~17.6 mag optical counterpart of the bright, soft, high-galactic latitude X-ray source RX J0512.2–3241 detected during the ROSAT All-Sky Survey, has been identified as a new, asynchronously rotating, magnetic cataclysmic variable (intermediate polar). The X-ray spectrum of RXJ0512–32 is similar to that of polars, it shows a soft component with no intrinsic absorption and a blackbody temperature kTbb~38 eV. From our optical follow-up B and V CCD photometry (cf. Fig. 1) we derive most probable spin and orbital periods of (863.5 ± 0.7) s and (3.45 ± 0.03) h respectively. A lower limit for the distance to the system is d > 740 pc. From this evidence we suggest that RXJ0512-32 is a further member of the ROSAT discovered class of soft X-ray intermediate polars (for details see Burwitz et al., 1996, A&A 310, L25). This still small class of systems (see Haberl and Motch 1995, A&A 297, L37) has X-ray characteristics similar to those of low magnetic field polars and may be their long sought evolutionary progenitors.

New insight into the origin of the GeV flare in the binary system PSR B1259-63/LS 2883 from the 2017 periastron passage

2020 ◽  
Vol 497 (1) ◽  
pp. 648-655
Author(s):  
M Chernyakova ◽  
D Malyshev ◽  
S Mc Keague ◽  
B van Soelen ◽  
J P Marais ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Energy Release ◽  
Broad Band ◽  
Strong Shock ◽  
Optical Observations ◽  
X Rays ◽  
X Ray ◽  
Inverse Compton ◽  
Pulsar Wind

ABSTRACT PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbiting around an O9.5Ve star, LS 2883, with a period of ∼3.4 yr. The interaction of the pulsar wind with the LS 2883 outflow leads to unpulsed broad-band emission in the radio, X-rays, GeV, and TeV domains. While the radio, X-ray, and TeV light curves show rather similar behaviour, the GeV light curve appears very different with a huge outburst about a month after a periastron. The energy release during this outburst seems to significantly exceed the spin-down luminosity of the pulsar and both the GeV light curve and the energy release vary from one orbit to the next. In this paper, we present for the first time the results of optical observations of the system in 2017, and also reanalyse the available X-ray and GeV data. We present a new model in which the GeV data are explained as a combination of the bremsstrahlung and inverse Compton emission from the unshocked and weakly shocked electrons of the pulsar wind. The X-ray and TeV emission is produced by synchrotron and inverse Compton emission of energetic electrons accelerated on a strong shock arising due to stellar/pulsar winds collision. The brightness of the GeV flare is explained in our model as a beaming effect of the energy released in a cone oriented, during the time of the flare, in the direction of the observer.

scholarly journals X-RAY AND OPTICAL OBSERVATIONS OF THE UNIQUE BINARY SYSTEM HD 49798/RX J0648.0-4418

2011 ◽  
Vol 737 (2) ◽  
pp. 51 ◽  
Author(s):  
S. Mereghetti ◽  
N. La Palombara ◽  
A. Tiengo ◽  
F. Pizzolato ◽  
P. Esposito ◽  
...  
Keyword(s):  
Binary System ◽  
Optical Observations ◽  
X Ray

scholarly journals Exploratory X-Ray Monitoring of Luminous Radio-quiet Quasars at High Redshift: Extended Time-series Analyses and Stacked Imaging Spectroscopy

2021 ◽  
Vol 923 (1) ◽  
pp. 111
Author(s):  
Marcus O. Thomas ◽  
Ohad Shemmer ◽  
W. N. Brandt ◽  
Maurizio Paolillo ◽  
Shai Kaspi ◽  
...  
Keyword(s):  
Time Series ◽  
Rest Frame ◽  
High Redshift ◽  
Imaging Spectroscopy ◽  
Optical Monitoring ◽  
Spectral Slope ◽  
Mean Power ◽  
X Ray ◽  
Time Series Analyses ◽  
The Mean

Abstract We present three new Chandra X-ray epochs along with new ground-based optical–UV observations as the third installment in a time-series analysis of four high-redshift (z ≈ 4.1–4.4) radio-quiet quasars. In total, we present nine epochs for these sources with rest-frame temporal baselines of ∼1300–2000 days. We utilize the X-ray data to determine basic variability properties, as well as produce mean spectra and stacked images based on effective exposure times of ∼40–70 ks per source. We perform time-series analyses in the soft and hard bands, separately, and compare variability properties to those of sources at lower redshifts and luminosities. The magnitude of X-ray variability of our sources remains consistent with or lower than that of similar sources at lower redshifts, in agreement with the variability–luminosity anticorrelation. The mean power-law photon indices in the stacked Chandra spectra of our sources are consistent with the values measured from their archival XMM-Newton spectra separated by about 3 yr in the rest frame. Along with the X-ray observations, we provide near-simultaneous optical monitoring of the sources in the optical–UV regime. The overall variability in the optical-to-X-ray spectral slope is consistent with sources at lower redshifts, and the optical–UV observations display mild variability on monthly timescales.

scholarly journals Nature of Circinus X-1

1979 ◽  
Vol 32 (2) ◽  
pp. 43 ◽  
Author(s):  
RF Haynes ◽  
David L Jauncey ◽  
I Lerche ◽  
PG Murdin
Keyword(s):  
Binary Star ◽  
Compact Star ◽  
Rotation Period ◽  
Optical Emission ◽  
Period Change ◽  
Optical Observations ◽  
Star Model ◽  
Primary Star ◽  
X Ray ◽  
Shock Fronts

X-ray, radio and optical observations have been used to derive a binary star model for CircinusX-1. Mass transfer between the primary star (Mp ~ 20Mo) and the compact companion star (Me ~ Mo) triggers one or more expanding shock fronts in the vicinity of the compact star. These shocks produce the observed radio emission. Variable optical emission arises both from the changing Roche lobe surface in the highly eccentric system (e ~ 0�8) and from degradation of shock-produced X-ray photons to the optical band by material overlying the expanding shock. The X-ray radiation results from matter in the accretion disc dribbling down on to the surface of the compact star. Mass replenishment at a rate of 5 x 10-8 to 5 X 10-10 Mo per orbit (16�6 day period) occurs near periastron passage. The variation of the X-ray emission arises from absorption in the stellar wind of the primary star. The model predicts an apsidal rotation period for the elliptical orbit of 7-400 yr, an orbital circularization time of ~ 500 yr and a period change of about 0�5 day per 10 yr.

Recent Optical Observations of the X-Ray Source H0139-68; an AM-Herculis Type Binary System

1982 ◽  
Vol 4 (4) ◽  
pp. 425-428
Author(s):  
A.J. Pickles ◽  
N. Visvanathan
Keyword(s):  
Binary System ◽  
Low Energy ◽  
Optical Observations ◽  
Short Time Scale ◽  
Optical Identification ◽  
Time Resolved ◽  
X Ray ◽  
Short Time ◽  
Energy Detectors ◽  
Optical Spectrophotometry

The soft X-ray source HO 139-68 was originally detected with the low energy detectors of the HEAO A-2 experiment, and confirmed by later IPC observations (Agarwal et al. 1981). The X-ray observations show flux variations in the 0.15 – 0.4 keV band of a factor of two, or timescales of a few hours, with evidence for short time-scale flickering. Following communication of the source position to us by Agarwal and Riegler, we obtained time-resolved optical spectrophotometry of a star close to the X-ray position, using the IDPCA on the MSO 1.9m telescope. The spectrophotometry and later polarisation observations confirm the optical identification and that the source is an AM-Herculis type binary system, with a late type dwarf secondary overflowing its Roche lobe in a magnetically constrained funnel onto a magnetic white dwarf (WD) primary (Visvanathan and Pickles 1982).

Multicolour photometry of SS 433

2018 ◽  
Vol 14 (S346) ◽  
pp. 252-254
Author(s):  
D. Koçak ◽  
T. İçli ◽  
K. Yakut
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Optical Observations ◽  
High Mass ◽  
National Observatory ◽  
X Ray ◽  
Ss 433

AbstractWe presented long-term optical observations of the high mass X-ray binary system SS 433 (V1343 Aql) with a black hole component. New observations have been obtained by using the 0.6m telescope at the TÜBİTAK National Observatory (TUG) in B, V, R and I filters. We aim to investigate the long-term photometric behavior of the system.

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