EUV brightenings using EUI and SPICE on board Solar Orbiter - Solar Orbiter (2023)

(Solar Orbiter nugget #6by Z. Huang1, L. Teriaca1 , R. Aznar Cuadrado1 , L. P. Chitta1 , S. Mandal1 , H. Peter1 , U. Schühle1 , S.K. Solanki1 , F. Auchère2 , D. Berghmans3 , É. Buchlin2 , M. Carlsson4, 5 , A. Fludra6 , T. Fredvik4, 5 , A. Giunta6 , T. Grundy6 , D. Hassler7 , S. Parenti2 , and F. Plaschke8)


The smallest coronal transient extreme-ultraviolet (EUV) brightening events that were observed so far, so-called campfires, were discovered by Berghmans et al.[1] in 2021 using data from the High Resolution Extreme Ultraviolet telescope (HRIEUV), which is part of the Extreme Ultraviolet Imager[2] (EUI) on board the ESA and NASA Solar Orbiter mission[3]. The high spatial and temporal resolution of HRIEUV enables us to study the small EUV brightenings (hereafter EUI brightenings) that are barely detected in other observations.

The discovery of EUI brightenings extends the boundary of EUV brightening event sizes to a smaller scale and helps to identify their potential role in coronal heating. To understand that, temperature is an important property and spectral data are necessary to study the temperature evolution of solar events. A first successful attempt at obtaining suitable simultaneous observations of the same region on the Sun with the instruments HRIEUV and SPectral Imaging of the Coronal Environment [4,5] (SPICE) occurred in 2021, during the cruise phase of Solar Orbiter. These observations provided the opportunity to investigate EUI brightenings, especially their thermal properties using both imaging and spectral data.

Combination of EUI and SPICE data

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For the purpose of studying their temperature properties, We selected EUI brightening events that can be identified in HRIEUV data and are also covered by the slit of SPICE. In this study, we focused on three cases from two different parts of the spacecraft orbit.

The first dataset was obtained on 23 February 2021 and the other datasets were obtained on 12 and 13 September 2021. Information about the datasets is included in Table 1. In dataset 1, SPICE took both context and small high-cadence rasters. The two context rasters are obtained by stepping the slit in 192 steps, while for each small raster, the slit scanned over three spatial positions.

In data set 2, SPICE observed in sit-and-stare mode.

Table 1. Overview of the observations.














2 s

1.65 s



20 s

Context rasters




20 s

4.7 s

Small rasters




2 s

1.65 s


10.2 s

10 s

Sit and stare



1 m




2 s



* All times refer to the starting times of the observations

Figure 1 shows overviews of the HRIEUV field of view that is covered in these two data sets. To accurately align the data from the two instruments, we applied a two-step approach and made use of time-series data. After alignment, we determined the positions of the EUI brightenings. Since the SPICE slit covered just a narrow region, only three EUI brightenings were identified in the HRIEUV and SPICE data. The white boxes in Fig. 1 mark the region also covered by the SPICE slit and the blue arrows point to the positions of EUI brightenings.SPICE spectra are dominated by the instrumental profile, which can be reasonably fitted by a Gaussian function. We used this to retrieve the integrated line radiance.

EUV brightenings using EUI and SPICE on board Solar Orbiter - Solar Orbiter (1)

Fig.1 HRIEUV images of the solar corona taken from the analyzed data sets. (a) Image obtained on 23 February 2021 at 17:17:28 UT (data set 1). The region that is also covered by SPICE slit (3-step) is marked by the white box. (b) Image obtained on 12 September 2021 at 22:06:10 UT (data set 2). The region also covered by the SPICE slit (sit and stare) is marked by the white box. (c) Image obtained on 13 September 2021 at 00:21:42 UT (data set 2). The region also covered by the SPICE slit (sit and stare) is marked by the white box. Blue arrows in all panels point to the positions of EUI brightenings.

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Temperature properties of EUI brightenings

EUI brightening E-1 (see Fig. 1a) is recognized in dataset 1. E-1 is very small, with an area of about 2.2 Mm2 and only survives for about 50s. Thus, the detection of E-1 is at the limit of the SPICE capabilities. It could not have been independently identified without the aid of HRIEUV observations. In the spectral data (Ne VIII, CIII, Lyb and O VI) from SPICE, only the O VI spectra show an increase around the time when the EUI brightening appears. No obvious clue of the EUI brightening is found in Ne VIII, which might indicate that this EUI brightening has a sufficient emission measure (to be detected by SPICE) only at temperatures close to the typical temperature of O VI (0.3 MK) and none, or very little, at coronal temperatures.

In dataset 2, two EUI brightenings (E-2 and E-3, see Fig. 1b and 1c) occur at the position of the SPICE slit. Compared with E-1, these brightenings are larger. They also last longer (i.e., 6 min for E-2 and 4 min for E-3, instead of less than a minute for E-1) and were observed by SPICE at higher time cadence (i.e., 10.2 s instead of 20 s) and with a longer exposure time (i.e., 10 s instead of 4.7 s). From the integrated line radiances of lines provided by SPICE (N IV, Ne VIII, S V, O IV, C III, Lyb and O VI), these two EUI brightenings are observed up to Ne VIII temperatures (0.6 MK). They are also detectable in O VI (0.3 MK) and in some other transition region (TR) lines.

As shown in Fig. 2a, E-3 is a loop-like event south of a larger brightening. In E-3, the EUI brightening emission in some TR lines shows two peaks around the peak time of the HRIEUV data and of Ne VIII. This can be seen in greater detail in Fig. 2b, where the temporal change of the C III, O VI and Ne VIII intensities are shown. The uncertainties of SPICE data are estimated by square-summing the photon noise component to the readout noise and to the dark noise. The different peak times may indicate the thermal evolution of E-3, that is, the temperature of this EUI brightening increases from the typical emission temperature of C III (log T[/K] = 4.8) to that of O VI (log T[/K] = 5.5) and then continues to rise to Ne VIII (log T[/K] = 5.8), which is the temperature of the lower corona. After the Ne VIII peak time, the EUI brightening starts to cool down to TR temperatures, which explains the appearance of the second emission peak in O VI and C III lines.

EUV brightenings using EUI and SPICE on board Solar Orbiter - Solar Orbiter (2)

Fig.2 EUI brightening (E-3). Panel (a): HRIEUV image taken on 13 September 2021 at 00:21:40 UT, at about the time when the intensity of the EUI brightening peaked. The smaller dashed box shows the region covered by one SPICE-binned pixel (4′′ × 4.392′′). The C III (green), O VI (blue) and Ne VIII (orange) intensities (normalized) at this pixel in panel (b) is calculated from Gaussian fits to the line in the SPICE data. Their peaks are marked by arrows in different colors. The error bars were calculated from the uncertainties of the fitting parameters. This region was also used to calculate the HRIEUV intensity (dashed line) in panel (b). The larger solid box shows the region we used to compute the light curve (solid line) shown in panel (b). The horizontal bar in the lower left corner shows the SPICE exposure duration, which is about 10 s.


Spectral data from SPICE allow us to follow the thermal properties of EUI brightenings. Our results indicate that at least some EUI brightenings barely reach coronal temperatures.

(Video) ESA/NASA Solar Orbiter SO/PHI with Sami Solanki (Max Planck Institute for Solar System research)

This work is now accepted in Astronomy and Astrophysics, forthcoming articles.



1 Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany

2 Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, 91405, Orsay, France

3 Solar-Terrestrial Centre of Excellence – SIDC, Royal Observatory of Belgium, Ringlaan -3- Av. Circulaire, 1180 Brussels, Belgium

4 Rosseland Centre for Solar Physics, University of Oslo, P.O. Box 1029 Blindern, NO-0315 Oslo, Norway

5 Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, NO-0315 Oslo, Norway

6 RAL Space, UKRI STFC, Rutherford Appleton Laboratory, Didcot, UK

(Video) First high resolution results from EUI: campfires and beyond

7 Southwest Research Institute, Boulder, CO, USA

8 Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Mendelssohnstrasse 3, 38106 Braunschweig, Germany


Solar Orbiter is a space mission of international collaboration between ESA and NASA, operated by ESA. The development of SPICE has been funded by ESA member states and ESA. It was built and is operated by a multi-national consortium of research institutes supported by their respective funding agencies: STFC RAL (UKSA, hardware lead), IAS (CNES, operations lead), GSFC (NASA), MPS (DLR), PMOD/WRC (Swiss Space Office), SwRI (NASA), UiO (Norwegian Space Agency). The EUI instrument was built by CSL, IAS, MPS, MSSL/UCL, PMOD/WRC, ROB, LCF/IO with funding from the Belgian Federal Science Policy Office (BELSPO/PRODEX PEA C4000134088); the Centre National d’Etudes Spatiales (CNES); the UK Space Agency (UKSA); the Bundesministerium für Wirtschaft und Energie (BMWi) through the Deutsches Zentrum für Luft- und Raumfahrt (DLR); and the Swiss Space Office (SSO). L.P.C. gratefully acknowledges funding by the European Union (ERC, ORIGIN, 101039844). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. S.P. acknowledges the funding by CNES through the MEDOC data and operations center.


[1] Berghmans, D., Auchère, F., Long, D. M., et al. 2021, A&A, 656, L4

[2] Rochus, P., Auchère, F., Berghmans, D., et al. 2020, A&A, 642, A8

[3] Müller, D., St. Cyr, O. C., Zouganelis, I., et al. 2020, A&A, 642, A1

[4] Spice Consortium, Anderson, M., Appourchaux, T., et al. 2020, A&A, 642, A14

[5] Fludra, A., Caldwell, M., Giunta, A., et al. 2021, A&A, 656, A38

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Solar Orbiter has as its primary science objectives: to study the drivers of the solar wind and the origin of the coronal magnetic field; to determine how solar transients drive heliospheric variability; to learn how solar eruptions produce the energetic particles that fill the heliosphere; and to study how the solar ...

What does EUI measure? ›

Site Energy Use Intensity (EUI), traditionally, is a simple quotient of energy delivered to a building divided by its area (typically expressed in Btu per square foot per year (Btu/sq. ft.

What is EUI energy intensity? ›

Energy Use Intensity (EUI) refers to the amount of energy used per square foot annually. It's calculated by dividing the total energy consumed by the building in a year by the total gross floor area. Like miles per gallon for cars, EUI is the prime indicator of a building's energy performance.

What is one advantage of using an Orbiter to study objects in space? ›

The benefits of using the orbiting spacecraft are that the orbiters are closer to the rover than the DSN antennas on Earth and the orbiters have Earth in their field of view for much longer time periods than the rover on the ground.

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Spacecraft in orbit around a planet have the ability to observe the same area again and again over a period of time. (We of course utilize this advantage every day for weather predictions made with data from Earth-orbiting weather satellites.)

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Is a higher or lower EUI better? ›

Generally, a low EUI signifies good energy performance.

Do you want a higher or lower EUI? ›

Unlike an ENERGY STAR score, which runs from 1-100, a lower EUI number generally represents better performance.

What is a good EUI? ›

EUI can vary significantly depending on building type. Hospitals have EUIs that can range from 400 to 500 kBTU/sf/year, due the high energy demand of interior lighting and hospital equipment. In contrast, a school may have an EUI in the range of 150 kBTU/sf/year.

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EUI is expressed as energy per square foot or meter per year. It is calculated by dividing the total energy consumed by the building in one year by the total gross floor area of the building.

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Energy Generation

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1 more row

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