Image

Fe XIV, 530.3 nm

Our expedition observed emission from the following ions in the visible and near IR wavelength range: Fe IX (435.9 nm), Fe X (637.4 nm), Fe XI (789.2 nm), Fe XIII (1074.7 nm), Fe XIV (530.3 nm) and Ni XV (670.2 nm). These emission lines provide an excellent diagnostic tool for probing the physics of the solar corona. One of the tools is clear from the following graph. Fe XIV line at 530.3 nm is the most prominent emission line in the visible part of the coronal spectrum.
 

Click on the image or on the following reference to display the higher resolution image version (842 KB, PNG format).

ImageTSE_2019_Rodeo_FeXIV.png
Date02. 07. 2019
Time2nd contact 20:40:01 UT, 3rd contact 20:42:53 UT
PlaceRodeo, Argentina
CoordinateS 30° 11.645',   W 69° 6.155',  Alt. 1550 m
ConditionsClear sky, solar altitude 11.5° above horizon
Optics2× Achromat 4/300 mm equipped with following narrow band filters:
  On-band filter: Andover, center wavelength: 530.3 nm, bandwidth 0.5 nm
  Off-band filter: Andover, center wavelength: 527.3 nm, bandwidth 0.5 nm
Camera2×Atik 314L
Exposure0.1 - 12.8 s
ProcessingComposition of 58 eclipse images (29 On-band and 29 Off-band) taken with two cameras. Images were calibrated by means of dark frames and flat-fields, aligned by means of phase correlation, composed by means of LDIC 6.0 software, continuum was removed from Fe XIV emission by subtracting the Off-band images. The resulting image was processed using Corona 6.0 software in order to visualize coronal structures. The final processing was done using ACC 6.1 software.
Image processing by Miloslav Druckmüller
SoftwareAstro D3F 2.0, PhaseCorr 7.0, LDIC 6.0, Corona 6.0, Sofo ACC 6.1
OrientationThis image has correct solar North-top orientation
Copyright© 2019 Miloslav Druckmüller, Shadia Habbal, Pavel Štarha, Jana Hoderová, Judd Johnson,
 

Miloslav Druckmüller
Institute of Mathematics, Faculty of Mechanical Engineering
Brno University of Technology, Czech Republic
druckmuller@fme.vutbr.cz
Page last update: 26.11.2019