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Astron. Astrophys. 330, L9-L12 (1998)

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Letter to the Editor

Accretion instabilities and jet formation in GRS 1915+105

I.F. Mirabel 1, 2, V. Dhawan 3, S. Chaty 1, L.F. Rodrguez 4, J.Mart 1, C.R. Robinson 5, J. Swank 6 and T.R. Geballe 7

1 Service d'Astrophysique, CEA/DSM/DAPNIA/SAp, Centre d'études de Saclay, F-91191 Gif-sur-Yvette Cedex, France
2 Instituto de Astronomía y Física del Espacio. C.C.67, Suc. 28, 1428 Buenos Aires, Argentina
3 National Radio Astronomy Observatory, Socorro, NM 87801, USA
4 Instituto de Astronoma, UNAM, Morelia, Michoacán 58090, Mexico
5 Marshall Space Flight Center, Space Science Laboratory, ES84, Huntsville, AL 35812, USA
6 Goddard Space Flight Ctr., Code 666, Greenbelt, MD 20771, USA
7 Joint Astronomy Centre, Hawaii Headquarters, 660 N. A'ohoku Place, Hilo, HI 96720, USA

Received 23 October 1997 / Accepted 10 November 1997


We report simultaneous observations in the X-ray, infrared, and radio wavelengths of the galactic superluminal source GRS 1915+105. During episodes of rapid disappearance and follow up replenishment of the inner accretion disk evidenced by the X-ray oscillating flux, we observe the ejection of relativistic plasma clouds in the form of synchrotron flares at infrared and radio wavelengths. The expelled clouds contain very energetic particles with Lorentz factors of [FORMULA], or more. These ejections can be viewed as small-scale analogs of the more massive ejecta with relativistic bulk motions that have been previously observed in GRS 1915+105.

Key words: accretion, accretion disks: stars: individual: GRS 1915+105 – stars: variables – Infrared: stars – radio continuum: stars – X-rays: stars

© European Southern Observatory (ESO) 1998

Online publication: January 8, 1998