Many jets are detected at X-ray wavelengths in the Sun ’ s polar regions , and the ejected plasma along the jets has been suggested to contribute mass to the fast solar wind .
From in-situ measurements in the magnetosphere , it has been found that the fast solar wind has photospheric abundances while the slow solar wind has coronal abundances .
Therefore , we investigated the abundances of polar jets to determine whether they are the same as that of the fast solar wind .
For this study , we selected 22 jets in the polar region observed by Hinode/EIS ( EUV Imaging Spectrometer ) and XRT ( X-Ray Telescope ) simultaneously on 2007 November 1-3 .
We calculated the First Ionization Potential ( FIP ) bias factor from the ratio of the intensity between high ( S ) and low ( Si , Fe ) FIP elements using the EIS spectra .
The values of the FIP bias factors for the polar jets are around 0.7-1.9 , and 75 \% of the values are in the range of 0.7-1.5 , which indicates that they have photospheric abundances similar to the fast solar wind .
The results are consistent with the reconnection jet model where photospheric plasma emerges and is rapidly ejected into the fast wind .