The calibration and initial results of the HeI D3 line flash spectrum obtained during the 2008 total solar eclipse

  • Hui Li
  • HaiSheng Ji
  • HouKun Ni
  • HaiYing Zhang
  • YaNan Zhang
  • HongRui Liu
  • YuanYong Deng
  • DongGuang Wang
  • QiuSheng Du
  • TuanHui Zhou
  • JingWei Li
  • JinHua Shen
Article
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Abstract

The flash spectra in the HeI D3 line were obtained during the 2008 total solar eclipse. This paper describes the instrument and the calibration of the obtained flash spectrum, and presents our initial results. The average integrated intensity is E ave = 8.13 × 1013 erg·cm−1·s−1·ster−1 at h = 1100 km, which confirms that the HeI D3 emission is negatively correlated with the solar activity. The surface brightness reaches a maximum of F ave = 8.25×105 erg·cm−2·s−1·ster−1 at about h ≈ (1290 ± 75) km and then decreases exponentially with height when h > 1800 km with an exponential index β = 1.63×10−8 cm−1.

Keywords

total solar eclipse flash spectrum spectral line 
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References

  1. 1.
    Sakurai T. Eleven-year solar cycle periodicity in sky brightness observed at Norikura, Japan. Earth Planets Space, 2002, 54: 153–157ADSGoogle Scholar
  2. 2.
    Athay R, Menzel D. A model of the chromosphere from the helium and continuum emissions. Astrophys J, 1956, 123: 285–298CrossRefADSGoogle Scholar
  3. 3.
    Dunn R, Evans J, Jefferies J, et al. The chromospheric spectrum at the 1962 eclipse. Astrophys J Suppl Ser, 1968, 15: 275–324CrossRefADSGoogle Scholar
  4. 4.
    Kurokawa H, Tominaga S, Kubota J, et al. The flash spectrum observed at the total eclipse of February 5, 1962. Publ Astron Soc Jpn, 1969, 21(2): 141–166ADSGoogle Scholar
  5. 5.
    Gulyaev R. The intensity distribution of the D3 helium line near the solar limb. Sol Phys, 1971, 18: 410–416CrossRefADSGoogle Scholar
  6. 6.
    Gulyaev R. The brightness of the helium D3 line in the undisturbed chromosphere from eclipse observations. Sol Phys, 1975, 44: 25–40CrossRefADSGoogle Scholar
  7. 7.
    Ji H, You J, Fan Z. A study of the helium D3 line in the flash spectrum of the 1983 eclipse. Chin Astron Astrophys, 1997, 21(3): 347–351CrossRefADSGoogle Scholar
  8. 8.
    Livshits M, Akimov L, Belkina I, et al. Helium emission in the middle chromosphere. Sol Phys, 1976, 49: 315–327CrossRefADSGoogle Scholar
  9. 9.
    Akimov L, Belkina I, Beletsky S, et al. Structure and emission of the solar chromosphere in the helium D3 line from observations of total solar eclipses. Kinematika i Fizika Nebesnykh Tel, 2002, 18: 136–148ADSGoogle Scholar
  10. 10.
    Belkina I, Dyatel N. Investigation of the chromosphere in the D3 helium line at the eclipse of September 22, 1968. Sov Astron, 1972, 16(3): 476–479ADSGoogle Scholar
  11. 11.
    You J, Fan Z, Ji H, et al. Photometric and height calibration of the spectra observed at the 1983 total solar eclipse. Chin Astron Astrophys, 1992, 16: 235–236ADSGoogle Scholar
  12. 12.
    Li H, Fan Z, You J. Infrared imaging solar spectrograph at Purple Mountain Observatory. Sol Phys, 1999, 185: 67–76CrossRefADSGoogle Scholar
  13. 13.
    Li H, You J, Wu Q, et al. Updated multichannel infrared solar spectrograph at Purple Mountain Observatory. Chin Phys Lett, 2002, 19: 742–744CrossRefADSGoogle Scholar
  14. 14.
    Cox A N. Allen’s Astrophysical Quantities. 4th ed. Berlin: Springer-Verlag, 2000. 354Google Scholar

Copyright information

© Science in China Press and Springer Berlin Heidelberg 2009

Authors and Affiliations

  • Hui Li
    • 1
  • HaiSheng Ji
    • 1
  • HouKun Ni
    • 2
  • HaiYing Zhang
    • 2
  • YaNan Zhang
    • 1
  • HongRui Liu
    • 1
  • YuanYong Deng
    • 3
  • DongGuang Wang
    • 3
  • QiuSheng Du
    • 1
  • TuanHui Zhou
    • 1
  • JingWei Li
    • 1
  • JinHua Shen
    • 1
  1. 1.Purple Mountain Observatory2 NanjingChina
  2. 2.Nanjing Institute of Astronomical Optics & TechnologyNanjingChina
  3. 3.National Astronomical Observatories of ChinaBeijingChina

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