High-Resolution X-Ray Spectra of the Symbiotic Star Ss73 17

Eze, R. N. C.; Luna, G. J. M.

doi:10.1088/0004-637x/709/2/816

Cited by 17 publications

(24 citation statements)

References 19 publications

(33 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The temperature inferred from a single-temperature fit will be lower than k T max . The plasma temperatures from single temperature fits to boundary layer emission in Kennea et al (2009) from RT Cru, T CrB, CH Cyg, and SS73 17 are lower than the maximum temperatures determined from cooling flow fits in RT Cru (Luna & Sokoloski 2007), T CrB (Luna et al 2008), and SS73 17 (Eze et al 2010). The higher absorbing column in front of the hard component is consistent with this component being closer to the central engine than the lower temperature plasma.…”

Section: Discussionmentioning

confidence: 77%

DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg

Stute¹,

Luna²,

Sokoloski³

2011

ApJ

View full text Add to dashboard Cite

We report the detection of X-ray emission from the symbiotic star V1329 Cyg with XMM-Newton. The spectrum from the EPIC pn, MOS1, and MOS2 instruments consists of a two-temperature plasma with k T 1 = 0.11 +0.02 −0.02 keV and k T 2 = 0.93 +0.12 −0.14 keV. Unlike the vast majority of symbiotic stars detected in X-rays, the soft component of the spectrum seems to be absorbed only by interstellar material. The shock velocities corresponding to the observed temperatures are about 300 km s −1 and about 900 km s −1 . We did not find either periodic or aperiodic X-ray variability, with upper limits on the amplitudes of such variations being 46% and 16% (rms), respectively. We also did not find any ultraviolet variability with an rms amplitude of more than approximately 1%. The derived velocities and the unabsorbed nature of the soft component of the X-ray spectrum suggest that some portion of the high energy emission could originate in shocks within a jet and beyond the symbiotic nebula. The lower velocity is consistent with the expansion velocity of the extended structure present in Hubble Space Telescope observations. The higher velocity could be associated with an internal shock at the base of the jet or with shocks in the accretion region.

show abstract

Section: Discussionmentioning

confidence: 77%

DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg

Stute¹,

Luna²,

Sokoloski³

2011

ApJ

View full text Add to dashboard Cite

show abstract

“…Unfortunately, the accuracy of our He-like and H-like EW measurements with the Chandra HETG and Suzaku CCDs are not adequate to constrain measurement of the G ratio of the Fe XXV line sufficiently to merit comparison with the measured bremsstrahlung temperature (see Eze et al 2010). However, we believe that since the hard X-rays from the source is thermal in origin, it is likely that theses emission lines are produced through collisional plasma rather than photoionization.…”

Section: On the Origin Of The Fe Kα Emission Linementioning

confidence: 87%

The FE Kα EMISSION LINE OF INTERMEDIATE POLAR V1223 SAGITTARII

Nwaffiah¹,

Eze²

2014

Journal of The Korean Astronomical Society

View full text Add to dashboard Cite

Abstract:We present measurements of the Fe Kα emission line of the intermediate polar V1223 Sagittarii observed with the Suzaku satellite. The spectrum is modeled with an absorbed thermal bremsstrahlung spectrum and three Gaussians for the three components of the Fe Kα lines. We resolve the neutral or lowionized (6.41keV), He-like (6.70keV), and H-like (7.00keV) iron lines. We also obtain a thermal continuum temperature of 25 keV, which supports a thermal origin of the hard X-rays observed from the shock heated layers of gas between the white dwarf and the shock front. Hence, we believe that the He-like and H-like lines are from the collisional plasma. On the origin of the Fe Kα fluorescence line, we find that it could be partly from reflections of hard X-rays from the white dwarf surface and the N H absorption columns. We also discuss the Fe Kα emission line as veritable tool for the probe of some astrophysical sites.

show abstract

“…Individual rapidly rotating G giant stars with accurate determinations of their X-ray luminosities using two-temperature thermal plasma emission models are marked by solid blue dots at the temperature of each thermal component connected by dotted lines (Gondoin et al 2002;Gondoin 2003aGondoin ,b, 2004Gondoin , 2005a. Individual cataclysmic variables (Eracleous et al 1991) and symbiotic stars (Mürset et al 1997;Stute & Sahai 2009;Eze et al 2010) curve of NGC 2392 is too fast to be associated with the rotational period of a late-type companion.…”

Section: Coronal Activity From a Companionmentioning

confidence: 99%

Variable Hard X-Ray Emission from the Central Star of the Eskimo Nebula

Guerrero

Toalá²,

Chu

2019

ApJ

View full text Add to dashboard Cite

The central star of NGC 2392 shows the hardest X-ray emission among central stars of planetary nebulae (CSPNe). The recent discovery of a spectroscopic companion with an orbital period of 1.9 days could provide an explanation for its hard X-ray emission, as well as for the collimation of its fast outflow. Here we analyse the available Chandra and XMM-Newton X-ray observations to determine accurately the spectral and temporal variation properties of the CSPN of NGC 2392. The X-ray emission can be described by an absorbed thermal plasma model with temperature 26 +8 −5 MK and X-ray luminosity (8.7±1.0)×10 30 erg s −1 . No long-term variability is detected in the X-ray emission level, but the Chandra light curve is suggestive of short-term variations with a period ∼0.26 days. The possible origins of this X-ray emission are discussed. X-ray emission from the coronal activity of a companion or shocks in the stellar wind can be ruled out. Accretion of material from an unseen main-sequence companion onto the CSPN or from the CSPN wind onto a white dwarf companion are the most plausible origins for its hard X-ray emission, although the mismatch between the rotational period of the CSPN and the modulation time-scale of the X-ray emission seems to preclude the former possibility.

show abstract

High-Resolution X-Ray Spectra of the Symbiotic Star Ss73 17

Cited by 17 publications

References 19 publications

DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg

DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg

The FE Kα EMISSION LINE OF INTERMEDIATE POLAR V1223 SAGITTARII

Variable Hard X-Ray Emission from the Central Star of the Eskimo Nebula

Contact Info

Product

Resources

About