shows absorption edges (which shows also the presence of neon) and an excess at high frequencies. Bipolar jets Following the 2006 outburst, the hydrogen Balmer emission lines included faint wings at a velocity of ±1,150 km/s. Since extended radio outflows had previously been seen during the long 2000-2002 outbursts, collimated jets along the axis of the system were the most likely explanation for this phenomenon. It is thought that the jets are only present during bright outbursts. The jets were observed again during subsequent outbursts; their velocity is highly variable at the beginning but settles on a constant velocity after roughly 1 month. A single jet can also occur. The jets could be formed by material that cannot accrete on the white dwarf that reaches the Eddington limit. References Further reading External links Image Z Andromedae AAVSO chart for Z Andromedae AAVSO long-term light curve of Z And Z Andromedae: The Prototype of the Symbiotic Class AAVSO 221650 Z Andromedae variables Andromeda (constellation) Andromedae, Z M-type giants J23333994+4849059 116287 Durchmusterung objects IRAS catalogue objects