1 / 55

Sara F. Martin Helio Research La Crescenta, CA

. . Questions: Can one model depict the physics of all filaments?Or are separate models needed to explain different categories of filaments (prominences)?Active Region Filaments physically different from Quiescent Filaments?. Questions:What properties Do AR and Quiescent Filaments have i

shel
Download Presentation

Sara F. Martin Helio Research La Crescenta, CA

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

    2.

    5. Both have a spine - a thin sheet of mass that are almost completely parallel with the a polarity inversion line (PIL) at the photosphere as seen in magnetograms. Both have an overlying coronal arcade – a loop shaped coronal fields that connect the outlying network magnetic fields on the two sides of prominences. Properties in Common for AR and Quiescent Filaments

    35. Properties in Common for AR and Quiescent Filaments Both have filament channels Both have helicity of the same type (mostly writhe, very little twist) Both have a Spine, mass that almost completely parallel with the a polarity inversion line at the photosphere as seen in magnetograms Both have an overlying coronal arcade (overlying coronal field (angle of overlying arcade depend on magnetic flux density of network magnetic fields on either side of the filament

    36. Evidence for the Formation of Faint, High Prominences in the Aftermath of CMEs Sara F. Martin Helio Research, La Crescenta, CA, USA Oddbjorn Engvold and Yong Lin Institute for Astrophysics, University of Oslo, Norway

    38. In the movie from 17 Sep, the brightest knots in the prominences appear as a series of condensations from which narrow streams of mass mostly moving downward downward with velocities as high as 70 km sec-1. However, some horizontal and upward flows were also observed in the range of 20-35 km sec-1 in the upper part of the frame. An unusual property of these prominences is their sudden appearance in less than 1 day at this extreme height.

    39. Because prominences do not typically occur in the high corona, we look for unusual circumstance when this might occur. LASCO movies revealed no events at 1R on the limb at the location of these prominences on the days of their appearance. However, on 14 and 15 September, 1-2 days prior to their appearance there were two faint CMEs at approximately the same latitudes at the limb. (point to the events)

    42. The CME on the 15 Sep was also observed at the High Altitude Observatory observing station on Mauna Loa. We deduce that both of these faint CMEs originated from the back side of the sun. (The tall, faint prominences were also observed at Mauna Loa on 16 and 17 September in their full disk prominence monitor with the disk of the Sun occulted.)

    44. There were no events at the site of these prominences on 17 Sep but it is possibly noteworthy that downward motion in a partially retracting streamer is seen in the corona above the second high prominence.

    47. Conclusions * Because of their relatively sudden appearance from one day to the next at solar altitudes in excess of 200,000 km, because they last for 1-2 days, and because they follow CMEs by 1-2 days, we suggest that the source of mass for these prominences is either (1) related to the final cooling phase of flare loop systems that begin during eruptive solar events or (2) to current sheets above the coronal loop systems, where mass can accumulate and fall back to the Sun.

    48. More Conclusions * These prominences might be unusually high examples of coronal clouds that are the source of coronal rain (Tandberg-Hanssen 1995, The Nature of Solar Prominences, p.107). This type of prominence might also be unusually high examples of the “Coronal Spiders” (Allen, Bagenal and Hundhausen (Allen, U. A. Bagenal, F. and Hundhausen, A. AAS SPD #28, #01.53, 1997; New Perspectives on Solar Prominences, ASP Conf. Series, Vol 150, p 290, 1998 ) which seem to be the same as “coronal clouds” described in Tandberg-Hanssen(1995). If so, these are cases where the spider body is unusually small and the legs unusually long.

    49. Support from NSF grant ATM-0209395 is acknowledged by S.F. Martin

    52. Are there any filaments that do not fit into this spectrum of filaments?

    56. Properties in Common for AR and Quiescent Filaments Both have filament channels Both have helicity of the same type (mostly writhe, very little twist) Both have a Spine, mass that almost completely parallel with the a polarity inversion line at the photosphere as seen in magnetograms Both have an overlying coronal arcade (overlying coronal field (angle of overlying arcade depend on magnetic flux density of network magnetic fields on either side of the filament

More Related