Geophysical observations began at Athabasca in November 1998, using a
~Ssmall~T magnetometer initially loaned (later donated) by UCLA. One solar
cycle later, interesting research results have sprouted from this ~Ssmall~T
seed. As part of the Canada Foundation for Innovation~Rs attempt to develop
world-class infrastructure, an observatory building was constructed in
2002, which allowed branching into multispectral auroral imaging at this
subauroral site. Shortly thereafter, the AUTUMN magnetometer network of
UCLA instruments was modestly funded, and UCLA magnetometers emplaced at
four subauroral sites in Alberta. A fifth AUTUMN magnetometer was placed
(by UC Berkeley) in Inuvik to feed data to the THEMIS project. In addition,
support for the STEP network of Kanji Hayashi has been extended, with
fieldwork every year since 2004 in support of its operation. In 2005, a
major commitment of guest equipment from STELAB enabled optimal
exploitation of the Athabasca site for combined optical and induction coil
studies which throw new light on the interaction of EMIC waves with protons
in the inner radiation belts, and most recently with relativistic
electrons. In 2007, cooperation with NRCan and seismologists resulted in
ongoing magnetometer data from a meridian chain on the east coast of Hudson
Bay, extending the MEASURE chain through the auroral zone. In-house
instrument development has included very low cost ground magnetometers for
educational and scientific use. Highlights of AUGO science over one solar
cycle will be presented, along with plans for its recently funded ($1.5
million) relocation to a new site free of light pollution.

Large-scale, long-lived coronal streamers are clearly identified on the
so-called coronal full limb synoptic maps (LSM). They are bright features
against polar coronal holes in the high latitudes, but are originated from
active regions in the more equatorial regions. Close inspection reveals
that individual sunspot active regions survive one or two solar rotations,
but continuous sunspot emergence in the vicinity of the active region
sustains the coronal streamer for as long as 10 solar rotations. 

I briefly review the physical properties of the coronal streamers. I
mainly describe the large-scale, long-lived streamers on the LSMs, which
lead to the finding of the non-contemporaneous sunspot cluster in the
photosphere. I discuss the implications of these streamers to the
structures of the interplanetary magnetic field, and the solar wind.