Ground experiment of a 50 mm balloon-borne coronagraph for near space project

We briefly report on the development of a 50 mm balloon-borne coronagraph and its recent ground experiment results made at the high altitude (4800 m above the sea level) site of Mt. Wumingshan in Daocheng, Sichuan of China. The main scientific purpose for developing this coronagraph is to investigate the morphology and dynamics of low-layer coronal structures before and during solar eruptions by observing at a float altitude of about 30 km from 1.08 Rsun to 1.5 Rsun at white light wavelength (centered at 550.0 nm, bandwidth 5 nm). The instrument is an internally occulted Lyot coronagraph developed by Yunnan Observatories in collaboration with Shangdong University (in Weihai) and Changchun Institute of Optics, Fine Mechanics and Physics. The coronagraph was designed with scattered light intensity level of better than 1×10-5 Isun in the inner field of view. A filter wheel system with linear polarizers and an sCMOS camera provided polarization and total brightness images of size 2048 x 2048 pixels. The first successful results were taken on February 27, 2021 in the Daocheng site. This coronagraph experiment obtained coronal images only showing obvious coronal structures very near limb. Furthermore, during the end of March and early April, after improving the polarizer filter system, higher-quality coronal images with pB coronal structures appeared in the full field of view were obtained in our ground-based experiments. Comparison between our results and the other coronal data in the world are discussed. The success of the 50 mm coronagraph in ground experiments is a milestone for us to develop the next-generation large-aperture coronagraph, as well as for future near space projects.

[1]  Z. Cai,et al.  Site testing campaign for the Large Optical/infrared Telescope of China: general introduction of the Daocheng site , 2020, Research in Astronomy and Astrophysics.

[2]  S. Fineschi,et al.  Simulating the Solar Corona in the Forbidden and Permitted Lines with Forward Modeling. I. Saturated and Unsaturated Hanle Regimes , 2019, The Astrophysical Journal.

[3]  Yu Liu,et al.  Operation of the astronomical monitoring stations at Mt. Wumingshan , 2018, Astronomical Telescopes + Instrumentation.

[4]  C. Fang Sixty-Year Career in Solar Physics , 2018 .

[5]  Yu Liu,et al.  The coronal green line monitoring: a traditional but powerful tool for coronal physics , 2018, Proceedings of the International Astronomical Union.

[6]  Yu Liu,et al.  The morphological comparison and analysis of coronal green line , 2018, Proceedings of the International Astronomical Union.

[7]  X. Cheng,et al.  Automatic Solar Seeing Observations at Mt. Wumingshan in Western China , 2018 .

[8]  M. Zhao,et al.  Conditions for Coronal Observations at the Lijiang Observatory in 2011 , 2017, Solar Physics.

[9]  Yongyin Lu,et al.  Progress of site survey for large solar telescopes in western China , 2015, Proceedings of the International Astronomical Union.

[10]  Yu Liu,et al.  The preliminary analysis of sunshine durations with meteorological data for the Chinese Giant Solar Telescope site survey , 2013 .

[11]  X. Zhang,et al.  Using a New Sky Brightness Monitor to Observe the Annular Solar Eclipse on 15 January 2010 , 2012, 1204.4289.

[12]  J. Kuhn,et al.  Coronal magnetic fields from the inversion of linear polarization measurements , 2009, Proceedings of the International Astronomical Union.

[13]  H. Lin Infrared Solar Polarimetry , 2009 .

[14]  Y. Liu Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations , 2009 .

[15]  Haosheng Lin,et al.  Observational Test of Coronal Magnetic Field Models. I. Comparison with Potential Field Model , 2007, 0710.3223.