The Equatorial Outflow of SS433

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dc.creatorParagi, Z.
dc.creatorFejes, I.
dc.creatorVermeulen, R. C.
dc.creatorSchilizzi, R. T.
dc.creatorSpencer, R. E.
dc.creatorStirling, A. M.
dc.date2002-07-02
dc.date2002-07-03
dc.date.accessioned2026-07-07T02:04:08Z
dc.date.available2026-07-07T02:04:08Z
dc.descriptionWe present VLBI imaging results for SS433 from the period 1995-2000. An equatorial emission region is detected and confirmed in 7 experiments at 1.6 and 5 GHz. The structure of the region changes with time on scales of weeks to months. The nature of emission is unknown, but it is certainly non-thermal, maybe optically thin synchrotron. The spectrum however might be attenuated by a thermal population of electrons. There were previous indications for an equatorial outflow from the system. We do detect outward motion of a radio component, and estimate a speed of 1200/sin(i) km/s. Theoretical work and IR observations suggest that the mass-loss rate in SS433 is much higher in this region than in the jets. We suggest that the high-mass microquasars might all have equatorial outflows; in fact, it is the dominant form of mass-loss in these systems.
dc.description4 pages, 3 figures (from 6 ps files), presented at the 6th EVN Symposium in Bonn, Germany, 25-28 June 2002. Note that fig. 2 is a compressed version and hence its quality is poorer. Paper compiled again with an updated EVN2002 class file - requested by the editors of the proceedings
dc.identifierhttps://arxiv.org/abs/astro-ph/0207061
dc.identifierhttp://arxiv.org/abs/astro-ph/0207061
dc.identifierin: Ros E., Porcas R.W., Lobanov A.P. and Zensus J.A. (eds.) Proc. 6th European VLBI Network Symposium, p. 263, MPIfR, Bonn (2002)
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/4636
dc.subjectAstrophysics
dc.titleThe Equatorial Outflow of SS433
dc.typetext

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