SSTRED: Data- and metadata-processing pipeline for CHROMIS and CRISP

Löfdahl, Mats G.; Hillberg, T.; Rodríguez, J. de la Cruz; Vissers, G. J. M.; Andriienko, O.; Scharmer, G.; Haugan, S. V. H.; Fredvik, T.

doi:10.1051/0004-6361/202141326

Cited by 50 publications

(41 citation statements)

References 58 publications

(47 reference statements)

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“…After the acquisition, the data have been reduced using the SSTRED pipeline (de la Cruz Löfdahl et al 2021). In order to take into account atmospheric effects, the data have been also processed using the Multi-Object Multi-Frame Blind Deconvolution method (MOMFBD) described in van Noort et al (2005).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Spatio-temporal analysis of chromospheric heating in a plage region

Morosin,

Rodríguez,

Baso

et al. 2022

Preprint

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Context. Our knowledge of the heating mechanisms that are at work in the chromosphere of plage regions remains highly unconstrained from observational studies. While many heating candidates have been proposed in theoretical studies, the exact contribution from each of them is still unknown. The problem is rather difficult because there is not direct way of estimating the heating terms from chromospheric observations. Aims. The purpose of our study is to estimate the chromospheric heating terms from a multi-line high spatial-resolution plage dataset, characterize their spatio-temporal distribution and set constraints on the heating processes that are at work in the chromosphere. Methods. We make use of non-local thermodynamical equilibrium (NLTE) inversions in order to infer a model of the photosphere and chromosphere of a plage dataset acquired with the Swedish 1-m Solar Telescope (SST). We use this model atmosphere to calculate the chromospheric radiative losses from the main chromospheric cooler from H i, Ca ii and Mg ii atoms. In this study, we approximate the chromospheric heating terms by the net radiative losses predicted by the inverted model. In order to make the analysis of timeseries over a large field-of-view (FOV) computationally tractable, we make use of a neural network which is trained from the inverted models of two non-consecutive time-steps. We have divided the chromosphere in three regions (lower, middle, upper) and analyzed how the distribution of the radiative losses is correlated with the physical parameters of the model. Results. In the lower chromosphere, the contribution from the Ca ii lines is dominant and predominantly located in the surroundings of the photospheric footpoints. In the upper chromosphere, the H i contribution is dominant. Radiative losses in the upper chromosphere form a relatively homogeneous patch that covers the entire plage region. The Mg ii also peaks in the upper chromosphere. Our time analysis shows that in all pixels, the net radiative losses can be split in a periodic component with an average amplitude of amp Q = 7.6 kW m −2 and a static (or very slowly evolving) component with a mean value of -26.1 kW m −2 . The period of the modulation present in the net radiative losses matches that of the line-of-sight velocity of the model. Conclusions. Our interpretation is that in the lower chromosphere, the radiative losses are tracing the sharp lower edge of the hot magnetic canopy that is formed above the photosphere, where the electric current is expected to be large. Therefore Ohmic current dissipation could explain the observed distribution. In the upper chromosphere, both the magnetic field and the distribution of net radiative losses are room-filling and relatively smooth, whereas the amplitude of the periodic component is largest. Our results suggest that acoustic wave heating may be responsible for one third of the energy deposition in the upper chromosphere, whereas other heating mechanisms must be responsible for the rest: turbulent Alfvén wave dissipation or...

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Section: Observations and Data Reductionmentioning

confidence: 99%

Spatio-temporal analysis of chromospheric heating in a plage region

Morosin,

Rodríguez,

Baso

et al. 2022

Preprint

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“…Table A.1 makes it clear that most of these data currently include observations of the chromosphere at the Ca II 8542 Å and Hα 6563 Å lines. It is worth noting that the Level 1 data of IBIS-A can be accessed with the CRIsp SPectral EXplorer (CRISPEX) graphical user interface (Vissers & Rouppe van der Voort 2012;Löfdahl et al 2021), version 1.7.4, which was developed to manage the CRISP and CHROMIS data. To this purpose, the IBIS data format needs to be adapted to the FITS format accepted by the CRISPEX interface with a code available at the IBIS-A site specified in the following.…”

Section: Data Formatmentioning

confidence: 99%

IBIS-A: The IBIS data Archive. High resolution observations of the solar photosphere and chromosphere with contextual data

Ermolli,

Giorgi,

Murabito

et al. 2022

Preprint

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Context. The IBIS data Archive (IBIS-A) stores data acquired with the Interferometric BIdimensional Spectropolarimeter (IBIS), which was operated at the Dunn Solar Telescope of the US National Solar Observatory from June 2003 to June 2019. The instrument provided series of high-resolution narrow-band spectro-polarimetric imaging observations of the photosphere and chromosphere in the range 5800−8600 Å and co-temporal broad-band observations in the same spectral range and with the same field-of-view of the polarimetric data. Aims. We present the data currently stored in IBIS-A, as well as the interface utilized to explore such data and facilitate its scientific exploitation. To this purpose we also describe the use of IBIS-A data in recent and undergoing studies relevant to Solar Physics and Space Weather research. Methods. IBIS-A includes raw and calibrated observations, as well as science-ready data. The latter comprise maps of the circular, linear, and net circular polarization, and of the magnetic and velocity fields derived for a significant fraction of the series available in the archive. IBIS-A furthermore contains links to observations complementary to the IBIS data, such as co-temporal high-resolution observations of the solar atmosphere available from the instruments onboard the Hinode and IRIS satellites, and full-disc multiband images from INAF solar telescopes. Results. IBIS-A currently consists of 30 TB of data taken with IBIS during 28 observing campaigns performed in 2008 and from 2012 to 2019 on 159 days. 29% of the observations are released as Level 1 data calibrated for instrumental response and compensated for residual seeing degradation, while 10% of these data is also available as Level 1.5 format as multi-dimensional arrays of circular, linear, and net circular polarization maps, and line-of-sight velocity patterns. 81% of the photospheric calibrated series present Level 2 data with the view of the magnetic and velocity fields of the targets, as derived from data inversion with the Very Fast Inversion of the Stokes Vector code (VFISV). Metadata and movies of each calibrated and science-ready series are also available to help users evaluating observing conditions. Conclusions. IBIS-A represents a unique resource for investigating the plasma processes in the solar atmosphere and the solar origin of Space Weather events. The archive presently contains 454 different series of observations. A recently undertaken effort to preserve IBIS observations is expected to lead in the future to an increase of the raw measurements and fraction of processed data available in IBIS-A.

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“…The restored WB continuum images have the same cadence as the Hβ data. More details on the optical setup on the SST imaging table are provided by Löfdahl et al (2021).…”

Section: Observationsmentioning

confidence: 99%

“…High spatial resolution was achieved by the combination of good seeing conditions, the adaptive optics system and the highquality CRISP and CHROMIS reimaging systems (Scharmer et al 2019). We further applied image restoration using the , Löfdahl et al 2021. The lower cadence and lower spatial resolution CRISP data (pixel scale 0 .…”

Section: Observationsmentioning

confidence: 99%

Signatures of ubiquitous magnetic reconnection in the lower solar atmosphere

Joshi

Voort

Rodríguez

2020

A&A

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Ellerman Bomb-like brightenings of the hydrogen Balmer line wings in the quiet Sun, also known as quiet Sun Ellerman bombs (QSEBs), are a signature of the fundamental process of magnetic reconnection at the smallest observable scale in the lower solar atmosphere. We analyze high spatial resolution observations (0.″1) obtained with the Swedish 1-m Solar Telescope to explore signatures of QSEBs in the Hβ line. We find that QSEBs are ubiquitous and uniformly distributed throughout the quiet Sun, predominantly occurring in intergranular lanes. We find up to 120 QSEBs in the field of view for a single moment in time; this is more than an order of magnitude higher than the number of QSEBs found in earlier Hα observations. This suggests that about half a million QSEBs could be present in the lower solar atmosphere at any given time. The QSEB brightenings found in the Hβ line wings also persist in the line core with a temporal delay and spatial offset toward the nearest solar limb. Our results suggest that QSEBs emanate through magnetic reconnection along vertically extended current sheets in the lower solar atmosphere. The apparent omnipresence of small-scale magnetic reconnection may play an important role in the energy balance of the solar chromosphere.

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SSTRED: Data- and metadata-processing pipeline for CHROMIS and CRISP

Cited by 50 publications

References 58 publications

Spatio-temporal analysis of chromospheric heating in a plage region

Spatio-temporal analysis of chromospheric heating in a plage region

IBIS-A: The IBIS data Archive. High resolution observations of the solar photosphere and chromosphere with contextual data

Signatures of ubiquitous magnetic reconnection in the lower solar atmosphere

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