Identification of X-ray lines in the spectrum of the arcsec-scale precessing jets of SS 433

Khabibullin, Ildar; Sazonov, S.

doi:10.1134/s1063773717060056

Cited by 3 publications

(1 citation statement)

References 16 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The overall geometry of this region with allowance for possible precession of the radiation cone axis has been fully described in . The 3D direction of the precession axis can be fully determined thanks to the spatially resolved precession pattern of radio emission at arcsec scales (Blundell & Bowler, 2004;Miller-Jones et al, 2008) and the detection of Doppler-shifted emission lines from the arcsec-scale X-ray emission of SS 433 (Migliari, Fender, & Méndez, 2002;Khabibullin & Sazonov, 2017). As a result, the location and geometry of the illumination region is fully determined by two parameters: the half-opening angle of the collimated emission cone, Θ r , and the position of the illuminating source along the line-of sight, i.e.…”

Section: Simulationmentioning

confidence: 99%

Constraints on the Collimated X-ray Emission of SS 433 from the Reflection on Molecular Clouds

Khabibullin

Sazonov

2019

Astron. Lett.

Self Cite

View full text Add to dashboard Cite

We calculate the X-ray signal that should arise due to reflection of the putative collimated X-ray emission of the Galactic supercritical accretor SS 433 on the molecular clouds in its vicinity. The molecular gas distribution in the region of interest has been constructed based on the data of the Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey in 13 CO J = 1 → 0 emission line, while the collimated emission was assumed to be aligned with the direction of the relativistic jets, which are continuously launched by the system. We consider all the available Chandra observations covering the regions possibly containing the reflection signal and put constraints on the apparent face-on luminosity of SS 433 above 4 keV. No signatures of the predicted signal have been found in the analysed regions down to a 4-8 keV surface brightness level of ∼ 10 −11 erg/s/cm 2 /deg 2 . This translates into the limit on the apparent face-on 2-10 keV luminosity of SS 433 LX,2−10 8 × 10 38 erg/s, provided that the considered clouds do fall inside the illumination cone of the collimated emission. This, however, might not be the case due to persisting uncertainty in the line-of-sight distances to SS 433 dSS433 (4.5-5.5 kpc) and to the considered molecular clouds. For the half-opening angle of the collimation cone larger than or comparable to the amplitude of the jets' precession (≈ 21 • ), the stringent upper limit quoted above is most relevant if dSS433 < 5 kpc, provided that the kinematic distances to the considered molecular clouds are sufficiently accurate (within ∼ 100 pc of the adopted values). Dropping the last assumption, a more conservative constraint is LX,2−10 10 40 erg/s for dSS433 = 4.65 − 4.85 kpc, and yet worse for dSS433 outside this range. We conclude that SS 433 is not likely to belong to the brightest ultraluminous X-ray sources if it could be observed face-on, unless its X-ray emission is highly collimated. However, better X-ray coverage of the molecular clouds in the region of interest is needed to eliminate dependence of this conclusion on incidence of the individual clouds inside the putative X-ray illumination cone of SS 433.

show abstract

Section: Simulationmentioning

confidence: 99%

Constraints on the Collimated X-ray Emission of SS 433 from the Reflection on Molecular Clouds

Khabibullin

Sazonov

2019

Astron. Lett.

Self Cite

View full text Add to dashboard Cite

show abstract

Minimalist model of the W50/SS433 extended X-ray jet: Anisotropic wind with recollimation shocks

Churazov,

Khabibullin,

Bykov

2024

A&A

View full text Add to dashboard Cite

W50 is a radio nebula around the hyperaccreting Galactic microquasar SS 433. We focus on one peculiar feature of W50, that is, on a pair of so-called extended X-ray jets (EXJs). These jets have a size of $ pc $ and a sharp inner boundary, and their spectra are well represented by a featureless X-ray continuum. We argue that EXJs could be an outcome of a powerful anisotropic wind produced by a supercritical accretion disk. In the simplest version of this model, the wind itself consists of two components. The first component is a nearly isotropic outflow that subtends most of the solid angle as seen from the compact source and creates the quasi-spherical part of the W50 nebula. The second component is a more collimated wind that is aligned with the rotation axis of the binary system (polar wind). The isotropic outflow passes through the termination shock, and its increased thermal pressure creates a sequence of recollimation shocks in the polar wind, giving it the appearance of an extended X-ray structure. In this model, the EXJ continuum spectrum is due to synchrotron emission of electrons that are accelerated at the shocks that arise in the polar wind. At variance with many other studies, the EXJ structures in this model are not directly related to the highly collimated and precessing $0.26\;\!c$ baryonic jets. Instead, the EXJ and the ears of W50 are produced by the part of the wind whose Eddington-level kinetic luminosity is confined to a half-opening angle of 5-10 degrees. This is not necessarily a recollimated version of the $0.26\;\!c$ jets.

show abstract

The X-ray Jets of SS 433 in the Period of Flaring Activity in the Summer of 2018

et al. 2022

View full text Add to dashboard Cite

Identification of X-ray lines in the spectrum of the arcsec-scale precessing jets of SS 433

Cited by 3 publications

References 16 publications

Constraints on the Collimated X-ray Emission of SS 433 from the Reflection on Molecular Clouds

Constraints on the Collimated X-ray Emission of SS 433 from the Reflection on Molecular Clouds

Minimalist model of the W50/SS433 extended X-ray jet: Anisotropic wind with recollimation shocks

The X-ray Jets of SS 433 in the Period of Flaring Activity in the Summer of 2018

Contact Info

Product

Resources

About