O I 7772 ~ continuum, dark smudge at center-top-left

On 2026-04-05, I imaged the Sun across multiple wavelengths, and found that areas that are dark smudges in oxygen are:

• rather unassuming bright-ish plages in:
  • Hα
  • Ca II 8542
  • Na I D2
• nothing obvious, small sunspot aside, in:
  • continuum
  • Fe I 7781
• dark in:
  • (O I 7772, hence smudge)
  • He I D3
  • He I 10830
  • H Paschen gamma

The images presented below are from scans recorded across several hours, each wavelength is the result of several scans stacked together. During acquisition, no major flares were reported. More about oxygen smudges here, here and here.

(tovább…)

During my campaign to observe the neutral oxygen triplet in the infrared, through full disk spectroheliograms, I noticed a few things:

• flares darken in oxygen, sometimes accompanied by shifts, one I measured was around 25 km/s
• obvious doppler shifts (of at least 1 km/s) are rare, judging by a superficial inspection of my collected data
• a general loss of contrast on the disk, active regions, plages darken and spots don’t darken that much,
• dark smudges on the disk
• chromosphere, prominences, some with doppler shifts,
• a light blanket just beyond the limb, above the active regions, a feature I am familiar with from He I D3, He I 7065 and He I 10830
• and a filament maybe (more on that later)

Smudges are areas that stand out as darker than expected, after taking into account spots, flares, and active regions. After contrasting the oxygen against a nearby continuum, either by subtraction or by division, smudges are revealed to be darker in oxygen, when compared to nearby active regions (which are themselves darkened) and thus a bit surprising. Smudges are stable across several minutes/hours, or even a day or two, while the flares I recorded are often times darker and short lived, on the order of minutes mostly. These smudges seem related to active regions, but don’t stand out in GONG Hα, where they can be a mere brighter spot like many others that don’t show up as smudges, nor AIA 1700 where the underlying area usually looks like any other active area that doesn’t show a smudge in oxygen. Better correlation can be seen with say SUVI 0304 or SUVI 0094 as small bright features in EUV, but it isn’t one-to-one either. Smudges stand out when they are somewhat towards the disk center, inside say 2/3 solar radii.

Below I compiled some scans with a nearby SUVI and AIA disk for comparison. I included smudges (marked with S), small and bright flares (marked with F), for context.

Instruments: 62/400 doublet, EO 775/25 OD4 narrow band filter, OD 0.6 neutral density filter, modified Sol’Ex, with 1800 ln/mm grating, modified/cooled ASI 678MM, JSol’Ex. Variable to good skies.

(tovább…)

O I 7772 (~) continuum, showing excess light on spots and shadows on plages

I observed the Sun in two oxygen lines, the O I 7772 and O I 8446, with the modified Sol’Ex (1800 gr/mm grating, band pass filters etc, 42/400 refractor). Unlike 7772 (the triplet), the 8446 (close doublet) doesn’t light up at the limb, as chromosphere. Regardless, I observed and processed the images. For λ7772, I have a full aperture etalon (CWL 775nm, FWHM 25NM, OD4 blocking), but only relatively wide bandpass filter(s) for λ8446, so parasite light is somewhat of an issue. Still, there is an interesting dark feature present in both observations, at around 4 o’clock, close to the edge.

(tovább…)

O I 7772 divided by a nearby continuum, stretched. Showing prominences, excess light on sunspots, darkening on active regions, and a dark shadow where the flare occurred at around 2026-02-03 07:49Z

Active region 4366 shows quite the flares. I observed the Sun at around local noon, at the infrared oxygen triplet at 777nm, focusing on the O I 7772 line. Below I present data from two scans, UT 2026-02-03-0727 with little indication of flaring, and UT 2026-02-03-0749 with clear signs of something going on.

I see what seems to be a clear indication of flaring: regions in oxygen go darker when other wavelengths shine, somewhat like He I D3 does — albeit I’ve seen bright helium flares in both D3 and even in He I 5016 before. Instrument: the modified Sol’Ex spectroheliograph,  with the 1800 ln/mm grating, and a front mounted full aperture Edmund Optics filter, CWL 775nm FWHM 25nm OD4. With the refractor thus stopped down to about 46/400, I recorded a time series. General observing conditions were poor, with passing clouds and bad seeing.

Processing: reconstructing the disks of the wavelength and a chosen continuum, dividing and stretching the two, and various other scripts for other kinds of output.

(tovább…)

before, and during the flare. Hα for reference

Did I just record a solar flare, its imprint in some form, in the infrared oxygen triplet’s O I 7772 line? I think there is something in the data, I just don’t know what exactly.

Using a modified* Sol’Ex, I recorded the Sun at the infrared oxygen triplet, together with the neutral iron Fe I 7781. Passing clouds and some haze made the session less than ideal. The recordings have been reconstructed in JSolEx, and further processed with JSolEx’s ImageMath module.

The oxygen triplet lights up in an obvious manner near and beyond the disk edge, and prominences are visible after applying curves or subtracting a continuum from the disk at the wavelength. This is what I expected, based on what I read in the literature.

Between around 10:30Z-11:00Z, local time 12:30-13:00, there was a flare on the Sun, and for the second half of it, I recorded, still between the clouds.

blink compare: bad seeing and the clouds didn’t help

(tovább…)

Paschen Gamma (enhanced) Solar Disk

Using the purpose built spectroheliograph, with stacked filters of 1075nm/50nm and 1100nm/50nm, I observed the Paschen gamma line (λ 10938.1Å), hoping to extract Hydrogen-resembling disk details. Neither the seeing, nor the low winter Sun helped the observation, worsening the already challenging endeavor.  For this observation, I used the IMX 585MM camera, instead of the 678MM, hoping to get more photons per pixel, sacrificing some spectral resolution — mixed results.

Still, the image published here, with the signal enhanced, could well be the very first Paschen Gamma Solar Disk, bringing the details to life.

The line itself is much weaker than the He I D3, it is a nebulous blur on the spectrum on the disk center, and is dwarfed by He I 10830 in the flash spectrum. In this respect, it resembles the situation of the (Balmer) epsilon line, which is overwhelmed by the calcium valley, or that of the He I D3 which is somewhat subtly visible while scanning, and is fully revealed only through continuum subtraction.

(tovább…)