The authors pointed out that the energy and mass requirements for coronal heating and solar wind can be satisfied by the jets. In search of the possible chromospheric counterparts for these jets, Wang et al. The count rate for UV jets is much lower than that in spicules, so we could exclude spicules from being the counterparts of UV jets. Observations at Halpha-1.0A make most spicules invisible. Frequently, we observed the darkenings in the Halpha-1.0A images, which are always located close to network magnetic elements.
Most jets are from repeatedly ejections from the same site throughout the day.
The observable fields are in the form of discrete magnetic elements. Obviously, these studies need to be extended to many regions, including the quiet network, the enhanced network and coronal holes, with new SOHO observations. Although the existing BBSO VMG system is capable of providing the most sensitive magnetogram, further improvements to the magnetograph system are planned to obtain even better data to support SOHO quiet Sun Observations. We are developing a digital magnetograph system to substitute the current video magnetograph system. The optical disk stores images in analog form, but its serial port allows us to have computer control and grab every image easily.