Hostname: page-component-848d4c4894-89wxm Total loading time: 0 Render date: 2024-07-06T00:35:26.201Z Has data issue: false hasContentIssue false
  • English
  • Français

Where do running penumbral waves emerge in chromosphere?

Published online by Cambridge University Press:  27 November 2018

T. G. Priya ,
Jiangtao Su  and
Robertus Erd̎elyi
T. G. Priya
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: priyatg@nao.cas.cn University of Chinese Academy of Sciences19 A Yuquan Rd, Shijingshan District, Beijing 100049, China
Jiangtao Su
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: priyatg@nao.cas.cn University of Chinese Academy of Sciences19 A Yuquan Rd, Shijingshan District, Beijing 100049, China
Robertus Erd̎elyi
Affiliation:
Solar Physics and Space Plasma Research Centre, School of Mathematics and Statistics, University of Sheffield, Hicks Building, Hounsfield Road, P.O.Box 32, Sheffield S3 7RH, UK
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The earlier work on the oscillatory phenomena in sunspot structures have supported in validating the detection of long-period oscillations, which are generated by the photospheric umbral response to the five minute p-mode global oscillations. We report here on the events of 3- min umbral oscillations which are detected within a duration of one hour from a single-polarity sunspot of active region NOAA 12132. The umbral oscillations that appear first around umbral boundaries is speculated to be excited by the wavefronts at the umbral-penumbral boundaries due to sub-photospheric or photospheric granular buffetings. The appearance of the wavefronts in spiral structures suggests that the wave guides are twisted. In addition, the newly formed running penumbral waves (RPWs) appears to be connected with the preceding RPWs.

Keywords

Sun: chromosphereSun: oscillationsSun: sunspots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 155 - 156
Copyright
Copyright © International Astronomical Union 2018 

References

Cao, W., Gorceix, N., Coulter, R., et al. 2010, Astronomische Nachrichten, 331, 636Google Scholar
Giovanelli, R.-G., 2013, solphys, 27, 71Google Scholar
Jess, D. B., Reznikova, V. E., Van Doorsselaere, T., Keys, P. H. et al. 2013, ApJ, 779, 168Google Scholar
Khomenko, E., Centeno, R., Collados, M., & Trujillo Bueno, J., 2008, ApJ, 676, L85Google Scholar
Priya, T. G., Wenda, Cao, Jiangtao, Su., Jie, Chen., Xinjie, Mao., Yuanyong, Deng., & Robert, Erdlyi., 2018, ApJ, 852, 15Google Scholar
Su, J. T., Ji, K. F., Cao, W., Banerjee, D., Priya, T. G., et al. 2016, ApJ, 817, 117Google Scholar
Zirin, H. & Stein, A., 1972, ApJ (Letters), 178, L85Google Scholar