Planned intervention: On Wednesday April 3rd 05:30 UTC Zenodo will be unavailable for up to 2-10 minutes to perform a storage cluster upgrade.
Published September 11, 2015 | Version v1
Presentation Open

Tracing the Prevalent Small-scale Transition Region Jets Observed with IRIS to Coronal Structures

  • 1. Michigan State University

Contributors

  • 1. Harvard Smithsonian Center for Astrophysics

Description

The transition region, the interface between the chromosphere and corona, is dominated by network-like emission and magnetic field structures. Observations from  the Interface Region Imaging Spectrograph (IRIS) reveal the prevalence of small-scale, jet-like features with temperatures of about 0.1 million degrees from network structures. These network jets have been suggested to be supersonic mass flows and may play an important role in transporting mass and energy to the corona and solar wind. Furthermore, EUV imaging observations reveal outward-propagating disturbances within coronal plumes originating from network regions. Previous investigations are inconclusive about the nature of these propagating disturbances. Some works suggest they are upward propagating slow magnetoacoustic waves, while others suggest they are coronal mass flows rather than waves.  We present the first comparative study between coronal propagating disturbances observed in the AIA 171 Å (Fe X/Fe IX)  passband and transition region network jets observed in IRIS 1330 Å (C II) slit-jaw images. By relating these two features, we seek further insight into the nature of coronal propagating disturbances and ultimately into the energy and mass transfer between the transition region, corona, and solar wind. Our preliminary study  indicates that network jets and coronal propagating disturbances are spatially correlated, suggesting that coronal propagating disturbances could be either waves triggered by network jets or the coronal continuations of those mass flows outward into the solar wind. Our continuing investigation will focus on disambiguating these two scenarios by characterizing the temporal and structural relationship between these coronal propagating disturbances and associated network jets.

Notes

This work was supported by the NSF-REU Solar Physics Program at SAO, grant number AGS 1263241; grant number NNX15AF48G from NASA to SAO; and by the IRIS contract 8100002705 from Lockheed-Martin to SAO.

Files

Wendeln_presentation.pdf

Files (288.6 MB)

Name Size Download all
md5:cb2a7290b0883e31877378488e1e0ac1
57.2 MB Download
md5:0f2f9d623e2cbbf3fa1163900e5802fc
8.0 MB Download
md5:afba5aa8989609b2637e054011f3952d
5.3 MB Download
md5:59d97c56028056a7d8b9e6219bbf3e6d
4.6 MB Download
md5:71e6cc4ce1d7fca048afb70bccb435a8
10.0 MB Download
md5:3c2e165a6522af469b3bfea2702024d7
18.6 MB Download
md5:8c25c8f9fe8eb8bc04e39cb6cdad4864
11.6 MB Download
md5:3d529d0e308d617d226decf6608448a5
3.3 MB Download
md5:f34a97bfacf0a3542c51407e45742c4f
11.2 MB Download
md5:f066bfddbf21db393fd602bf427d5458
16.3 MB Preview Download
md5:64332517ee4082661accd9d826924b08
142.6 MB Download