Continuous Upflow of Plasmas at the Edge of an Active Region as Revealed by the X-ray Telescope (XRT) aboard Hinode

Details Continuous Upflow of Plasmas at the Edge of an Active Region as Revealed by the X-ray Telescope (XRT) aboard Hinode Continuous Upflow of Plasmas at the Edge of an Active Region as Revealed by the X-ray Telescope (XRT) aboard Hinode

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.7205s&link_type=abstract

American Astronomical Society Meeting 210, #72.05; Bulletin of the American Astronomical Society, Vol. 39, p.179

Astronomy and Astrophysics

Astronomy

Scientific paper

We present X-ray imaging observations with Hinode X-Ray Telescope (XRT) of an active region NOAA AR 10942 made in the period of 20-22 February 2007. A prominent feature that drew our particular attention is that there revealed continuous upflow of soft-X-ray-emitting plasmas along apparently-open field lines towards the outer corona emanating from the edge of the active region.
The field lines are originated from an ensamble of small spots of following polarity, and are located at a border between the active region and an adjacent equatorial coronal hole(s) located to the east. The upflow was observed to be continuous throughout the three days of observation intervals with projected velocity of 140 km/s, accompanied with undulating motion of the field lines.
We assert that these upflowing plasmas would be a possible source of slow solar wind material, which supports a foresighted notion which grew out of interplanetary scintillation observations that slow solar wind most likely has its origin in the vicinity of active regions with large flux expansion (Kojima et al. 1999).
A preliminaty analysis indicates that the temperature of the upflowing material near the base of the field lines is 1.3 MK with number density of 2 × 109 /cm3. Assuming that all the material is to escape to the interplanetary space, this leads to a mass loss rate of 2 × 1011 g/s which amounts to a good fraction of the total mass loss rate for solar wind. It is noteworthy that, even apart from this unique upflow, we see continuous (up)flows of plasmas anywhere around (surrounding) the active region.
Details of the upflow will be presented and their possible implication to slow solar wind discussed.

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