1 Paper in press in Solar Physics (accepted 7 nov 2011) Formation of a White-Light Jet within a Quadrupolar Magnetic Configuration Boris Filippov 1  Serge Koutchmy 2  Ehsan Tavabi 3 1 Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Russian Academy of Sciences, Troitsk, Moscow Region 142190, Russia (e-mail: bfilip@izmiran.ru) 2 Institut d'Astrophysique de Paris, CNRS and Univ. P.& M. Curie, 98 bis Boulevard Arago, 75014 Paris, France (e-mail: koutchmy@iap.fr) 3 Payame Noor University of Zanjan and Institute of Geophysics, University of Tehran, 14155-6466, Iran (e-mail: etavabi@yahoo.com) Abstract. We analyze multi-wavelength and multi-viewpoint observations of a large-scale event viewed on 7 April 2011 originating from an active region complex. The activity leads to a white- light jet being formed in the outer corona. The topology and evolution of the coronal structures were imaged in high resolution using the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). In addition, large field-of-view images of the corona were obtained using the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) telescope onboard the PRoject for Onboard Autonomy (PROBA2) microsatellite, providing evidence for the connectivity of the coronal structures with outer coronal features that were imaged with the Large Angle Spectrometric Coronagraph (LASCO) C2 on Solar and Heliospheric Observatory (SOHO). The data-sets reveal an Eiffel-tower type jet configuration extending into a narrow jet in the outer corona. The event starts from the growth of a dark area in the central part of the structure. The darkening was also observed in projection on the disk by the Solar TErrestrial RElations Observatory-Ahead (STEREO-A) spacecraft from a different point of view. We assume that the dark volume in the corona descends from a coronal cavity of a flux rope that moved up higher in the corona but still failed to erupt. The quadrupolar magnetic configuration corresponds to a saddle-like shape of the dark volume and provides a possibility for the plasma to escape along the open field lines into the outer corona, forming the white-light jet. Keywords: Coronal Jets; Filaments; Dark Cavities; Magnetic fields; Reconnection 1. Introduction Among the different forms of solar activity, there are apparently linear collimated plasma flows, which are presumably guided by magnetic fields, usually referred to as jets. These are found in the literature concerning soft X-ray and extreme ultraviolet (EUV) observations, and as ray-like features in eclipse observations (Saito and Tandberg-Hanssen, 1973). A wide variety of jet-like structures are observed in the solar atmosphere. They can be formed both from relatively cool plasma as spicules, spikes, macro-spicules and surges (Koutchmy and Stellmacher, 1976; Rompolt and Svestka, 1996; Sterling, 2000; Yamauchi et al., 2005) as well as from hot plasma and seen in X-rays, white-light and EUV (Brueckner, 1981; Shibata et al., 1992; Shimojo et al., 1996; Koutchmy et al., 1997; Koutchmy et al., 1998, 2010; Pike and Mason, 1998; Wang et al., 1998; Chae et al., 1999; Harrison et al., 2001). Wang et al. (1998) discovered that numerous white-light LASCO-C2 jet-like ejections above the polar regions were the outward extensions of