Emergence of Granular-sized Magnetic Bubbles Through the Solar Atmosphere. III. The Path to the Transition Region

DOI: 
10.3847/0004-637X/825/2/93
Publication date: 
01/07/2016
Main author: 
Ortiz, Ada
IAA authors: 
Ortiz, Ada;Ramón Bellot Rubio, Luis
Authors: 
Ortiz, Ada;Hansteen, Viggo H.;Ramón Bellot Rubio, Luis;de la Cruz Rodríguez, Jaime;De Pontieu, Bart;Carlsson, Mats;Rouppe van der Voort, Luc
Journal: 
The Astrophysical Journal
Refereed: 
Yes
Publication type: 
Article
Volume: 
825
Pages: 
93
Abstract: 
We study, for the first time, the ascent of granular-sized magnetic bubbles from the solar photosphere through the chromosphere into the transition region and above. Such events occurred in a flux emerging region in NOAA 11850 on 2013 September 25. During that time, the first co-observing campaign between the Swedish 1-m Solar Telescope (SST) and the Interface Region Imaging Spectrograph (IRIS) spacecraft was carried out. Simultaneous observations of the chromospheric Hα 656.28 nm and Ca ii 854.2 nm lines, plus the photospheric Fe i 630.25 nm line, were made with the CRISP spectropolarimeter at the Spitzer Space Telescope (SST) reaching a spatial resolution of 0.″14. At the same time, IRIS was performing a four-step dense raster of the emerging flux region, taking slit jaw images at 133 (C ii, transition region), 140 (Si iv, transition region), 279.6 (Mg ii k, core, upper chromosphere), and 283.2 nm (Mg ii k, wing, photosphere). Spectroscopy of several lines was performed by the IRIS spectrograph in the far- and near-ultraviolet, of which we have used the Si iv 140.3 and the Mg ii k 279.6 nm lines. Coronal images from the Atmospheric Imaging Assembly of the Solar Dynamics Observatory were used to investigate the possible coronal signatures of the flux emergence events. The photospheric and chromospheric properties of small-scale emerging magnetic bubbles have been described in detail in Ortiz et al. Here we are able to follow such structures up to the transition region. We describe the properties, including temporal delays, of the observed flux emergence in all layers. We believe this may be an important mechanism of transporting energy and magnetic flux from subsurface layers to the transition region and corona.
Database: 
ADS
SCOPUS
WOK
URL: 
https://ui.adsabs.harvard.edu/#abs/2016ApJ...825...93O/abstract
ADS Bibcode: 
2016ApJ...825...93O
Keywords: 
Sun: chromosphere;Sun: magnetic fields;Sun: transition region;Astrophysics - Solar and Stellar Astrophysics