[P-EM14] Frontiers in solar physics

[PEM14-P05] Inconspicuous Solar Polar Coronal X-ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer (EIS) Doppler Outflows

*Alphonse Sterling¹, Conrad Schwanitz^2,3, Louise K Harra^2,3, Nour E Raouafi⁴, Navdeep K Panesar^5,6, Ronald L Moore^7,1 (1.NASA/MSFC, Huntsville, AL, 35812, USA, 2.Institute for Particle Physics and Astrophysics, ETH, 8092 Zurich, Switzerland, 3.Physikalisch Meteorologisches Observatorium Davos, World Radiation Center, 7260 Davos, Switzerland, 4.The John Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA, 5. Bay Area Environmental Research Institute, NASA Research Park, Moffett Field, CA 94035, USA, 6.Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Building 252, Palo Alto, CA 94304, USA, 7.Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35805, USA)

Keywords:Solar Coronal Jets, Solar (Mini)filament Eruptions, Hinode/EIS and XRT Observations, SDO/AIA and HMI Observations

We examine in greater detail five events previously identified as being sources of strong transient coronal outflows in a solar polar region in Hinode/EUV Imaging Spectrometer (EIS) Doppler data. Although relatively compact or faint and inconspicuous in Hinode/Soft X-ray Telescope (XRT) soft X-ray (SXR) images and in Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) EUV images, we find that all of these events are consistent with being faint coronal X-ray jets. The evidence for this is that the events result from eruption of minifilaments of projected sizes spanning 5000---14,000 km and with erupting velocities spanning 19---46 km/s, which are in the range of values observed in cases of confirmed X-ray polar coronal hole jets. In SXR images, and in some EUV images, all five events show base brightenings, and faint indications of a jet spire that (in four of five cases where determinable) moves away from the brightest base brightening; these properties are common to more obvious X-ray jets. For a comparatively low-latitude event, the minifilament erupts from near (<~few arcsec) a location of near-eruption-time opposite-polarity magnetic-flux-patch convergence, which again is consistent with many observed coronal jets. Thus, although too faint to be identified as jets a priori, otherwise all five events are identical to typical coronal jets. This suggests that jets may be more numerous than recognized in previous studies, and might contribute substantially to solar wind outflow, and to the population of magnetic switchbacks observed in Parker Solar Probe (PSP) data. This work was supported by NASA's Heliophysics Guest Investigator (HGI), Heliophysics Supporting Research (HSR), and Heliophysics System Observatory Connect (HSOC) Programs, and by the NASA/MSFC Hinode Project.