77 citations · 362 across the 13 of their papers we have counts for
13 papers
Evolution of dynamic fibrils from the cooler chromosphere to the hotter corona
Sudip Mandal, Hardi Peter, Lakshmi Pradeep Chitta +17
Dynamic fibrils (DFs) are commonly observed chromospheric features in solar active regions. Recent observations from the Extreme Ultraviolet Imager (EUI) aboard the Solar Orbiter h…
Picoflare jets power the solar wind emerging from a coronal hole on the Sun
L. P. Chitta, A. N. Zhukov, D. Berghmans +17
Coronal holes are areas on the Sun with open magnetic field lines. They are a source region of the solar wind, but how the wind emerges from coronal holes is not known. We observed…
A multiple spacecraft detection of the 2 April 2022 M-class flare and filament eruption during the first close Solar Orbiter perihelion
M. Janvier, S. Mzerguat, P. R. Young +56
The Solar Orbiter mission completed its first remote-sensing observation windows in the spring of 2022. On 2/4/2022, an M-class flare followed by a filament eruption was seen both…
Imaging and spectroscopic observations of extreme-ultraviolet brightenings using EUI and SPICE on board Solar Orbiter
Ziwen Huang, L. Teriaca, R. Aznar Cuadrado +16
The smallest extreme-ultraviolet (EUV) brightening events that were detected so far, called campfires, have recently been uncovered by the High Resolution EUV telescope (HRIEUV), w…
Slow solar wind sources. High-resolution observations with a quadrature view
Krzysztof Barczynski, Louise Harra, Conrad Schwanitz +16
The origin of the slow solar wind is still an open issue. One possibility that has been suggested is that upflows at the edge of an active region can contribute to the slow solar w…
Signatures of dynamic fibrils at the coronal base: Observations from Solar Orbiter/EUI
Sudip Mandal, Hardi Peter, Lakshmi Pradeep Chitta +20
The solar chromosphere hosts a wide variety of transients, including dynamic fibrils (DFs) that are characterised as elongated, jet-like features seen in active regions, often thro…
What drives decayless kink oscillations in active region coronal loops on the Sun?
Sudip Mandal, Lakshmi P. Chitta, Patrick Antolin +19
We study here the phenomena of decayless kink oscillations in a system of active region (AR) coronal loops. Using high resolution observations from two different instruments, namel…
Solar coronal heating from small-scale magnetic braids
L. P. Chitta, H. Peter, S. Parenti +19
Relaxation of braided coronal magnetic fields through reconnection is thought to be a source of energy to heat plasma in active region coronal loops. However, observations of activ…
Automatic detection of small-scale EUV brightenings observed by the Solar Orbiter/EUI
N. Alipour, H. Safari, C. Verbeeck +23
Context. Accurate detections of frequent small-scale extreme ultraviolet (EUV) brightenings are essential to the investigation of the physical processes heating the corona. Aims. W…
First observations from the SPICE EUV spectrometer on Solar Orbiter
A. Fludra, M. Caldwell, A. Giunta +28
We present first science observations taken during the commissioning activities of the Spectral Imaging of the Coronal Environment (SPICE) instrument on the ESA/NASA Solar Orbiter…
Stereoscopy of extreme UV quiet Sun brightenings observed by Solar Orbiter/EUI
A. N. Zhukov, M. Mierla, F. Auchère +27
The 3D fine structure of the solar atmosphere is still not fully understood as most of the available observations are taken from a single vantage point. The goal of the paper is to…
Investigating the origin of the FIP effect with a shell turbulence model
Victor Réville, Alexis P. Rouillard, Marco Velli +4
The enrichment of coronal loops and the slow solar wind with elements that have low First Ionisation Potential, known as the FIP effect, has often been interpreted as the tracer of…
Energetic characterisation and statistics of solar coronal brightenings
Vincent Joulin, Éric Buchlin, Jacques Solomon +1
To explain the high temperature of the corona, much attention has been paid to the distribution of energy in dissipation events. Indeed, if the event energy distribution is steep e…