Prominence measurement of total solar eclipse: March 9th 2016, Ternate, Indonesia

International Symposium on Sun, Earth, and Life

物理学;天文学;生物科学

Naufal, Luthfi^1 ; Mulki, Fargiza Abdan Malikul^1 ; Fatima, Siti^1 ; Widyanita^1 ; Zahirah, Saffanah^1 ; Satrya, Christoforus Dimas^2 ; Herdiwijaya, Dhani^1

Astronomy Department, InstitutTeknologi Bandung, Bandung

40132, Indonesia^1

Physics Department, InstitutTeknologi Bandung, Bandung

40132, Indonesia^2

关键词: Ground-based observations;    Infrared spectrum;    Infrared wavelengths;    IR cut filters;    Solar prominences;    Solar surfaces;    Total solar eclipse;    Visual wavelength;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/771/1/012007/pdf
DOI  :  10.1088/1742-6596/771/1/012007

来源: IOP

【 摘 要 】

Prominence is a hot gas that consists of electrically charged particles, which is propelled outward Solar surface. It can happen when the activity of sunspot rising up. Ground- based observation of prominence is rather difficult due to the brightness of the Sun, which it needs appropriate method. During total solar eclipse (TSE), prominence is easier to observe. In Ternate, Maluku islands (0°4632.0″N 127°2305.7″E), we observed solar prominence in visual and infrared spectra performed by using regular-DSLR camera for visual wavelength and modified-DSLR (IR-cut filter removal) for infrared wavelength, respectively. Next, we calculated the length of prominence from TSE images, and found that the real minimum length of prominence in red is 1.05 times longer than green and blue ones. And, the real maximum length of prominence is 1.08 times longer than blue and 1.04 times longer than green. The intensity of red is brighter 1.37 times to green and 1.23 times to blue. The causes of the results due to the different temperatures of the prominences and the radiation from H-alpha emission. We succeeded to observe directly the prominence with simple cameras and measured its length and brightness.