MAGNETIC TOPOLOGY OF BUBBLES IN QUIESCENT PROMINENCES

• Published in: The Astrophysical journal Vol. 761; no. 1; pp. 1 - 13
• Main Authors: DUDIK, J, AULANIER, G, SCHMIEDER, B, ZAPIOR, M, HEINZEL, P
• Format: Journal Article
• Language: English
• Published: Bristol IOP 10.12.2012; American Astronomical Society
• Subjects: ASTRONOMY; ASTROPHYSICS; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BRIGHTNESS; Bubbles; Coronas; Dipping; Earth, ocean, space; Exact sciences and technology; MAGNETIC FIELDS; MAGNETIC RECONNECTION; MAGNETISM; Physics; Plumes; Prominences; Separators; SOLAR CORONA; SOLAR PROMINENCES; SUN; SURFACES; TOPOLOGY; ULTRAVIOLET RADIATION; Poland; Magnetic reconnection; Field line; Flux rope; Sun: corona; Viewing angle; Topology; Sun: UV radiation; Sun; Linear model; Alignment; Ultraviolet radiation; Sun: filaments, prominences; Sun: magnetic topology; Filaments; Quiescent prominence; Sun: surface magnetism; Magnetic fields
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637x/761/1/9

We study a polar-crown prominence with a bubble and its plume observed in several coronal filters by the SDO/AIA and in H[alpha] by the MSDP spectrograph in Bialkow (Poland) to address the following questions: what is the brightness of prominence bubbles in EUV with respect to the corona outside of the prominence and the prominence coronal cavity? What is the geometry and topology of the magnetic field in the bubble? What is the nature of the vertical threads seen within prominences? We find that the brightness of the bubble and plume is lower than the brightness of the corona outside of the prominence, and is similar to that of the coronal cavity. We constructed linear force-free models of prominences with bubbles, where the flux rope is perturbed by inclusion of parasitic bipoles. The arcade field lines of the bipole create the bubble, which is thus devoid of magnetic dips. Shearing the bipole or adding a second one can lead to cusp-shaped prominences with bubbles similar to the observed ones. The bubbles have complex magnetic topology, with a pair of coronal magnetic null points linked by a separator outlining the boundary between the bubble and the prominence body. We conjecture that plume formation involves magnetic reconnection at the separator. Depending on the viewing angle, the prominence can appear either anvil-shaped with predominantly horizontal structures, or cusp-shaped with predominantly vertical structuring. The latter is an artifact of the alignment of magnetic dips with respect to the prominence axis and the line of sight.