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Study of Hα Jets on the Quiet Sun

Wang, Haimin and Johannesson, Anders and Stage, Mike and Lee, Chikyin and Zirin, Harold (1998) Study of Hα Jets on the Quiet Sun. Solar Physics, 178 (1). pp. 55-69. ISSN 0038-0938. https://resolver.caltech.edu/CaltechAUTHORS:20200722-163251827

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Abstract

High-speed jets of solar quiet regions have been observed at Big Bear Solar Observatory in Hα−1.0 Å, and compared with high-resolution magnetograms. Over the whole Sun, the birthrate of the Hα−1.0 Å jets is about 19±3 events s⁻¹, which is much lower than the birthrate of spicules. The average lifetime of these jets is 2±1 min. Hα−1.0 Å jets are very different from spicules, in the sense of birthrate, lifetime, and shape. Jets tend to recur in the same sites, always located in boundaries of supergranules. Under the best observing conditions, we found that 80% of the major jet sites are associated with converging magnetic dipoles – mainly the sites where intranetwork elements are canceling with opposite polarity network elements. In order to establish a possible relationship between the disk Hα jets and limb macrospicules, we have also obtained time sequences of Hα center-line images at the limb. These images are enhanced by median filtering so that jet structures over the limb are easily studied. We found that these limb Hα jets (above the spicule forest) repeatedly occur in the same sites, which is the property shared by the disk Hα−1.0 Å jets. However, their mean lifetime is 10 min, substantially longer than that of disk jets. Comparison with simultaneous SOHO/EIT Heɪɪ 304 Å images shows that every Heɪɪ 304 Å jet over the limb coincides with an Hα jet, although Heɪɪ 304 Å jets extend much farther out. Some Hα jets do not have associated He jets, probably due to the difference in image resolutions. Hα spectra of selected jets are analyzed, and we found that jets are not simply blue-shifted; instead, the line profiles are broadened with significantly larger broadening on the blue side. Two-component fitting finds that the velocity of the blue-shifted component (an optically-thin component) is around 20 to 40 km s⁻¹.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1023/a:1004974927114DOIArticle
https://rdcu.be/b5NJ4PublisherFree ReadCube access
ORCID:
AuthorORCID
Wang, Haimin0000-0002-5233-565X
Additional Information:© 1998 Kluwer Academic Publishers. Received 13 December 1996; accepted 17 June 1997. We are grateful to the observing staff at BBSO for their support in obtaining the data. We also would like to thank the SOHO EIT team for making He II 304 Å images available. Thework is supported by NSF under grant NSF9628862, NASA under SOHO grant NAG5–3536 and NJIT SBR Award.
Funders:
Funding AgencyGrant Number
NSFNSF-9628862
NASANAG5-3536
New Jersey Institute of Technology (NJIT)UNSPECIFIED
Subject Keywords:Opposite Polarity, Line Profile, Average Lifetime, Network Element, Solar Observatory
Issue or Number:1
Record Number:CaltechAUTHORS:20200722-163251827
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200722-163251827
Official Citation:Wang, H., Johannesson, A., Stage, M. et al. Study of Hα Jets on the Quiet Sun. Solar Physics 178, 55–69 (1998). https://doi.org/10.1023/A:1004974927114
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104524
Collection:CaltechAUTHORS
Deposited By: Rebecca Minjarez
Deposited On:23 Jul 2020 16:53
Last Modified:23 Jul 2020 16:53

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