W 50 Morphology and the Dynamics of SS 433 Formation—The Origin of TeV Gammas from the Microquasar

• 發表在: Particles
• 主要作者: Michael Bowler
• 格式: Article
• 語言: 英语
• 出版: MDPI AG 2024-09-01
• 主題: stars; binaries; SS 433; circumstellar matter; W 50; TeV gamma astronomy
• 在線閱讀: https://www.mdpi.com/2571-712X/7/3/47

The precessing jets of microquasar SS 433 have punched through the supernova remnant W 50 from the explosion forming the compact object. The jets collimate before reaching beyond the shell, some 40 pc downstream, just the region of origin of TeV gamma radiation. Collimation could be effected by ambient pressure in the SNR cavity; I investigate conditions under which the W 50 morphology and the sites of TeV gamma radiation can be explained in terms of collimation, with associated shocks, induced by ambient pressure. The SNR is now ~<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msup><mrow><mn>10</mn></mrow><mrow><mn>5</mn></mrow></msup></mrow></semantics></math></inline-formula> years after the supernova; with the present pressure, collimation and associated shocks would indeed occur ~40 pc downstream. Modeling of the evolution of binary systems indicates that the Roche lobe overflow and the initiation of the jets may be recent rather than early; present day collimation would still occur ~40 pc downstream, but the cone angle of the precession must then have increased with time—driven by the Roche lobe overflow. The morphology of W 50 and the site of the origin of TeV radiation are readily explained in terms of the collimation of the jets by internal SNR pressure.