2021年2月12日 · We propose a new scenario in which the SS433 jets themselves form the W50/SS433 system. We carry out magnetohydrodynamics simulations of two-side jet propagation using the public code CANS+. As found in previous jet studies, when the propagating jet is lighter than the surrounding medium, the shocked plasma flows back from the jet tip to the core.

It is at the centre of the supernova remnant W50. SS 433's designation comes from the initials of two astronomers at Case Western Reserve University: Nicholas Sanduleak and Charles Bruce Stephenson. It was the 433rd entry in their 1977 catalog of stars with strong emission lines. [7] Its emission lines were studied by Mordehai Milgrom in 1979. [8]

2021年4月6日 · We propose a new scenario in which the SS 433 jets themselves form the W50/SS 433 system. We carry out magnetohydrodynamics simulations of the propagation of two side jets using the public code CANS+.

2018年10月3日 · The lobes of W50 in which the jets terminate, about 40 parsecs from the central source, are expected to accelerate charged particles, and indeed radio and X-ray emission consistent with electron...

2024年1月26日 · W50 is a radio nebula around hyper-accreting Galactic microquasar SS433. In this letter, we focus on one peculiar feature of W50 - a pair of so-called "extended X-ray jets" (EXJs). These "jets" have a size of $\sim20\, {\rm pc}$, a sharp inner boundary, and their spectra are well represented by a featureless X-ray continuum.

2024年7月30日 · W50 is a radio nebula around the hyperaccreting Galactic microquasar SS433. 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 ∼20 pc and a sharp inner boundary, and their spectra are well represented by a featureless X-ray continuum.

W50 is a radio nebula around hyper-accreting Galactic microquasar SS 433. Here we focus on one peculiar feature of W50 - a pair of so-called "extended X-ray jets" (EXJs). These "jets" …

We propose a new scenario in which the SS 433 jets themselves form the W50/SS 433 system. We carry out magnetohydrodynamics simulations of the propagation of two side jets using the public code CANS+.

2023年7月1日 · The captivating and complex W50 nebula is powered by SS433, a microquasar, and is classified as a supernova remnant with an unusual double-lobed morphology reminiscent of a Manatee. Recent high energy TeV emission detected by HAWC, has renewed interest in this particle acceleration scenario.

2022年8月24日 · Using NuSTAR, XMM-Newton, and Chandra observations of the inner eastern lobe of W50, we have detected hard nonthermal X-ray emission up to ∼30 keV, originating from a few-arcminute-sized knotty region ("Head") located ≲18' (29 pc for a distance of 5.5 kpc) east of SS 433, and constrained its photon index to 1.58 ± 0.05 (0.5–30 keV band).