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1. Coronal Heating Rate in the Slow Solar Wind

Author

Telloni, Daniele, Romoli, Marco, Velli, Marco, Zank, Gary P., Adhikari, Laxman, Downs, Cooper, Burtovoi, Aleksandr, Susino, Roberto, Spadaro, Daniele, Zhao, Lingling, Liberatore, Alessandro, Shi, Chen, De Leo, Yara, Abbo, Lucia, Frassati, Federica, Jerse, Giovanna, Landini, Federico, Nicolini, Gianalfredo, Pancrazzi, Maurizio, Russano, Giuliana, Sasso, Clementina, Andretta, Vincenzo, Da Deppo, Vania, Fineschi, Silvano, Grimani, Catia, Heinzel, Petr, Moses, John D., Naletto, Giampiero, Stangalini, Marco, Teriaca, Luca, Uslenghi, Michela, Berlicki, Arkadiusz, Bruno, Roberto, Capobianco, Gerardo, Capuano, Giuseppe E., Casini, Chiara, Casti, Marta, Chioetto, Paolo, Corso, Alain J., D'Amicis, Raffaella, Fabi, Michele, Frassetto, Fabio, Giarrusso, Marina, Giordano, Silvio, Guglielmino, Salvo L., Magli, Enrico, Massone, Giuseppe, Messerotti, Mauro, Nisticò, Giuseppe, Pelizzo, Maria G., Reale, Fabio, Romano, Paolo, Schühle, Udo, Solanki, Sami K., Straus, Thomas, Ventura, Rita, Volpicelli, Cosimo A., Zangrilli, Luca, Zimbardo, Gaetano, Zuppella, Paola, Bale, Stuart D., and Kasper, Justin C.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics
Abstract

This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a minor fraction of the solar wind energy flux, since most of the energy dissipation that feeds the heating and acceleration of the coronal flow occurs much closer to the Sun than the heights probed in the present study, which range from 6.3 to 13.3 solar radii. The energy deposited to the supersonic wind is then used to explain the observed slight residual wind acceleration and to maintain the plasma in a non-adiabatic state. As derived in the Wentzel-Kramers-Brillouin limit, the present energy transfer rate estimates provide a lower limit, which can be very useful in refining the turbulence-based modeling of coronal heating and subsequent solar wind acceleration.

Published
2023

2. On the evolution of a sub-C class flare: a showcase for the capabilities of the revamped Catania Solar Telescope

Author

Romano, Paolo, Guglielmino, Salvo L., Costa, Pierfrancesco, Falco, Mariachiara, Buttaccio, Salvatore, Costa, Alessandro, Martinetti, Eugenio, Occhipinti, Giovanni, Spadaro, Daniele, Ventura, Rita, Capuano, Giuseppe E., and Zuccarello, Francesca

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Solar flares are occasionally responsible for severe Space Weather events, which can affect space-borne and ground-based infrastructures, endangering anthropic technological activities and even human health and safety. Thus, an essential activity in the framework of Space Weather monitoring is devoted to the observation of the activity level of the Sun. In this context, the acquisition system of the Catania Solar Telescope has been recently upgraded in order to improve its contribution to the European Space Agency (ESA) - Space Weather Service Network through the ESA Portal, which represents the main asset for Space Weather in Europe. Here, we describe the hardware and software upgrades of the Catania Solar Telescope and the main data products provided by this facility, which include full-disc images of the photosphere and chromosphere, together with a detailed characterization of the sunspot groups. As a showcase of the observational capabilities of the revamped Catania Solar Telescope, we report the analysis of a B5.4 class flare occurred on 2020 December 7, simultaneously observed by the IRIS and SDO satellites.

Published
2021
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3. Exploring the Solar Wind from its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter - Parker Solar Probe Quadrature

Author

Telloni, Daniele, Andretta, Vincenzo, Antonucci, Ester, Bemporad, Alessandro, Capuano, Giuseppe E., Fineschi, Silvano, Giordano, Silvio, Habbal, Shadia, Perrone, Denise, Pinto, Rui F., Sorriso-Valvo, Luca, Spadaro, Daniele, Susino, Roberto, Woodham, Lloyd D., Zank, Gary P., Romoli, Marco, Bale, Stuart D., Kasper, Justin C., Auchère, Frédéric, Bruno, Roberto, Capobianco, Gerardo, Case, Anthony W., Casini, Chiara, Casti, Marta, Chioetto, Paolo, Corso, Alain J., Da Deppo, Vania, De Leo, Yara, de Wit, Thierry Dudok, Frassati, Federica, Frassetto, Fabio, Goetz, Keith, Guglielmino, Salvo L., Harvey, Peter R., Heinzel, Petr, Jerse, Giovanna, Korreck, Kelly E., Landini, Federico, Larson, Davin, Liberatore, Alessandro, Livi, Roberto, MacDowall, Robert J., Magli, Enrico, Malaspina, David M., Massone, Giuseppe, Messerotti, Mauro, Moses, John D., Naletto, Giampiero, Nicolini, Gianalfredo, Nisticò, Giuseppe, Panasenco, Olga, Pancrazzi, Maurizio, Pelizzo, Maria G., Pulupa, Marc, Reale, Fabio, Romano, Paolo, Sasso, Clementina, Schühle, Udo, Stangalini, Marco, Stevens, Michael L., Strachan, Leonard, Straus, Thomas, Teriaca, Luca, Uslenghi, Michela, Velli, Marco, Verscharen, Daniel, Volpicelli, Cosimo A., Whittlesey, Phyllis, Zangrilli, Luca, Zimbardo, Gaetano, and Zuppella, Paola

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics, Physics - Space Physics
Abstract

This Letter addresses the first Solar Orbiter (SO) -- Parker Solar Probe (PSP) quadrature, occurring on January 18, 2021, to investigate the evolution of solar wind from the extended corona to the inner heliosphere. Assuming ballistic propagation, the same plasma volume observed remotely in corona at altitudes between 3.5 and 6.3 solar radii above the solar limb with the Metis coronagraph on SO can be tracked to PSP, orbiting at 0.1 au, thus allowing the local properties of the solar wind to be linked to the coronal source region from where it originated. Thanks to the close approach of PSP to the Sun and the simultaneous Metis observation of the solar corona, the flow-aligned magnetic field and the bulk kinetic energy flux density can be empirically inferred along the coronal current sheet with an unprecedented accuracy, allowing in particular estimation of the Alfv\'en radius at 8.7 solar radii during the time of this event. This is thus the very first study of the same solar wind plasma as it expands from the sub-Alfv\'enic solar corona to just above the Alfv\'en surface., Comment: 10 pages, 4 figures

Published
2021
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4. Comparative case study of two methods to assess the eruptive potential of selected active regions

Author

Zuccarello, Francesca, Ermolli, Ilaria, Korsos, Marianna B., Giorgi, Fabrizio, Guglielmino, Salvo L., Erdelyi, Robertus, and Romano, Paolo

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Solar eruptive events, like flares and coronal mass ejections, are characterized by the rapid release of energy that can give rise to emission of radiation across the entire electromagnetic spectrum and to an abrupt significant increase in the kinetic energy of particles. These energetic phenomena can have important effects on the Space Weather conditions and therefore it is necessary to understand their origin, in particular, what is the eruptive potential of an active region (AR). In these case studies, we compare two distinct methods that were used in previous works to investigate the variations of some characteristic physical parameters during the pre-flare states of flaring ARs. These methods consider: i) the magnetic flux evolution and the magnetic helicity accumulation, and ii) the fractal and multi-fractal properties of flux concentrations in ARs. Our comparative analysis is based on time series of photospheric data obtained by the Solar Dynamics Observatory between March 2011 and June 2013. We selected two distinct samples of ARs: one is distinguished by the occurrence of more energetic M- and X-class flare events, that may have a rapid effect on not just the near-Earth space, but also on the terrestrial environment; the second is characterized by no-flares or having just few C- and B-class flares. We found that the two tested methods complement each other in their ability to assess the eruptive potentials of ARs and could be employed to identify ARs prone to flaring activity. Based on the presented case study, we suggest that using a combination of different methods may aid to identify more reliably the eruptive potentials of ARs and help to better understand the pre-flare states.

Published
2021
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6. Metis Observation of the Onset of Fully Developed Turbulence in the Solar Corona

Author

Daniele Telloni, Luca Sorriso-Valvo, Gary P. Zank, Marco Velli, Vincenzo Andretta, Denise Perrone, Raffaele Marino, Francesco Carbone, Antonio Vecchio, Laxman Adhikari, Lingling Zhao, Sabrina Guastavino, Fabiana Camattari, Chen Shi, Nikos Sioulas, Zesen Huang, Marco Romoli, Ester Antonucci, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Lucia Abbo, Frédéric Auchère, Regina Aznar Cuadrado, Arkadiusz Berlicki, Roberto Bruno, Aleksandr Burtovoi, Gerardo Capobianco, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D’Amicis, Yara De Leo, Michele Fabi, Federica Frassati, Fabio Frassetto, Silvio Giordano, Salvo L. Guglielmino, Giovanna Jerse, Federico Landini, Alessandro Liberatore, Enrico Magli, Giuseppe Massone, Giuseppe Nisticò, Maurizio Pancrazzi, Maria G. Pelizzo, Hardi Peter, Christina Plainaki, Luca Poletto, Fabio Reale, Paolo Romano, Giuliana Russano, Clementina Sasso, Udo Schühle, Sami K. Solanki, Leonard Strachan, Thomas Straus, Roberto Susino, Rita Ventura, Cosimo A. Volpicelli, Joachim Woch, Luca Zangrilli, Gaetano Zimbardo, and Paola Zuppella

Subjects
Magnetohydrodynamics, Interplanetary turbulence, Space plasmas, Solar corona, Solar wind, Astrophysics, QB460-466
Abstract

This Letter reports the first observation of the onset of fully developed turbulence in the solar corona. Long time series of white-light coronal images, acquired by Metis aboard Solar Orbiter at 2 minutes cadence and spanning about 10 hr, were studied to gain insight into the statistical properties of fluctuations in the density of the coronal plasma in the time domain. From pixel-by-pixel spectral frequency analysis in the whole Metis field of view, the scaling exponents of plasma fluctuations were derived. The results show that, over timescales ranging from 1 to 10 hr and corresponding to the photospheric mesogranulation-driven dynamics, the density spectra become shallower moving away from the Sun, resembling a Kolmogorov-like spectrum at 3 R _⊙ . According to the latest observation and interpretive work, the observed 5/3 scaling law for density fluctuations is indicative of the onset of fully developed turbulence in the corona. Metis observation-based evidence for a Kolmogorov turbulent form of the fluctuating density spectrum casts light on the evolution of 2D turbulence in the early stages of its upward transport from the low corona.

Published
2024
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7. Continuum enhancements, line profiles and magnetic field evolution during consecutive flares

Author

Zuccarello, Francesca, Guglielmino, Salvo L., Capparelli, Vincenzo, Mathioudakis, Mihalis, Keys, Peter H., Criscuoli, Serena, Falco, Mariachiara, and Murabito, Mariarita

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics
Abstract

During solar flares, magnetic energy can be converted into electromagnetic radiation from radio waves to $\gamma$ rays. Enhancements in the continuum at visible wavelengths give rise to white-light flares, as well as continuum enhancements in the FUV and NUV passbands. In addition, the strong energy release in these events can lead to the rearrangement of the magnetic field at the photospheric level, causing morphological changes in large and stable magnetic structures like sunspots. In this context, we describe observations acquired by satellite instruments (IRIS, SDO/HMI, Hinode/SOT) and ground-based telescopes (ROSA/DST) during two consecutive C7.0 and X1.6 flares occurred in active region NOAA 12205 on 2014 November 7. The flare was accompanied by an eruption. The results of the analysis show the presence of continuum enhancements during the evolution of the events, observed both in ROSA images and in \textit{IRIS} spectra. In the latter, a prominent blue-shifted component is observed at the onset of the eruption. We investigate the role played by the evolution of the $\delta$ sunspots of the active region in the flare triggering, and finally we discuss the changes in the penumbrae surrounding these sunspots as a further consequence of these flares., Comment: 19 pages, accepted for ApJ; some figures are in B/W to accomplish size limits

Published
2019
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8. Historical solar Ca II K observations at the Rome and Catania observatories

Author

Chatzistergos, Theodosios, Ermolli, Ilaria, Falco, Mariachiara, Giorgi, Fabrizio, Guglielmino, Salvo L., Krivova, Natalie A., Romano, Paolo, and Solanki, Sami K.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Here we present the little explored Ca II K archives from the Rome and the Catania observatories and analyse the digitised images from these archives to derive plage areas., Comment: 5 pages, 3 figures, to be published in "Nuovo Cimento C" as proceeding of the Third Meeting of the Italian Solar and Heliospheric Community

Published
2019
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9. IRIS observations of magnetic interactions in the solar atmosphere between pre-existing and emerging magnetic fields. II. UV emission properties

Author

Guglielmino, Salvo L., Young, Peter R., and Zuccarello, Francesca

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Multi-wavelength ultraviolet (UV) observations by the IRIS satellite in active region NOAA 12529 have recently pointed out the presence of long-lasting brightenings, akin to UV bursts, and simultaneous plasma ejections occurring in the upper chromosphere and transition region during secondary flux emergence. These signatures have been interpreted as evidence of small-scale, recurrent magnetic reconnection episodes between the emerging flux region (EFR) and the pre-existing plage field. Here, we characterize the UV emission of these strong, intermittent brightenings and we study the surge activity above the chromospheric arch filament system (AFS) overlying the EFR. We analyze the surges and the cospatial brightenings observed at different wavelengths. We find an asymmetry in the emission between the blue and red wings of the Si IV 1402 \AA{} and Mg II k 2796.3 \AA{} lines, which clearly outlines the dynamics of the structures above the AFS that form during the small-scale eruptive phenomena. We also detect a correlation between the Doppler velocity and skewness of the Si IV 1394 \AA{} and 1402 \AA{} line profiles in the UV burst pixels. Finally, we show that genuine emission in the Fe XII 1349.4 \AA{} line is cospatial to the Si IV brightenings. This definitely reveals a pure coronal counterpart to the reconnection event., Comment: 19 pages, 8 figures + 3 figures in the Appendix; accepted in ApJ

Published
2018
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10. IRIS observations of magnetic interactions in the solar atmosphere between pre-existing and emerging magnetic fields. I. Overall evolution

Author

Guglielmino, Salvo L., Zuccarello, Francesca, Young, Peter R., Murabito, Mariariata, and Romano, Paolo

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We report multi-wavelength ultraviolet observations taken with the IRIS satellite, concerning the emergence phase in the upper chromosphere and transition region of an emerging flux region (EFR) embedded in the pre-existing field of active region NOAA 12529. IRIS data are complemented by full-disk observations of the Solar Dynamics Observatory satellite, relevant to the photosphere and the corona. The photospheric configuration of the EFR is also analyzed by measurements taken with the spectropolarimeter aboard the Hinode satellite, when the EFR was fully developed. Recurrent intense brightenings that resemble UV bursts, with counterparts in all coronal passbands, are identified at the edges of the EFR. Jet activity is also observed at chromospheric and coronal levels, near the observed brightenings. The analysis of the IRIS line profiles reveals the heating of dense plasma in the low solar atmosphere and the driving of bi-directional high-velocity flows with speed up to 100 km/s at the same locations. Compared with previous observations and numerical models, these signatures suggest evidence of several long-lasting, small-scale magnetic reconnection episodes between the emerging bipole and the ambient field. This process leads to the cancellation of a pre-existing photospheric flux concentration and appears to occur higher in the atmosphere than usually found in UV bursts, explaining the observed coronal counterparts., Comment: 12 figures, accepted in ApJ

Published
2018
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14. The 17 February 2013 sunquake in the context of the active region's magnetic field configuration

Author

Green, Lucie M., Valori, Gherardo, Zuccarello, Francesco P., Zharkov, Sergei, Matthews, Sarah, and Guglielmino, Salvo L.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Sunquakes are created by the hydrodynamic response of the lower atmosphere to a sudden deposition of energy and momentum. In this study we investigate a sunquake that occurred in NOAA active region 11675 on 17 February 2013. Observations of the corona, chromosphere and photosphere are brought together for the first time with a non-linear force-free model of the active region's magnetic field in order to probe the magnetic environment in which the sunquake was initiated. We find that the sunquake was associated with the destabilization of a flux rope and an associated M-class GOES flare. Active region 11675 was in its emergence phase at the time of the sunquake and photospheric motions caused by the emergence heavily modified the flux rope and its associated quasi-separatrix layers, eventually triggering the flux rope's instability. The flux rope was surrounded by an extended envelope of field lines rooted in a small area at the approximate position of the sunquake. We argue that the configuration of the envelope, by interacting with the expanding flux rope, created a "magnetic lens" that may have focussed energy in one particular location the photosphere, creating the necessary conditions for the initiation of the sunquake., Comment: 20 pages, 16 Figures. Some figures have lower resolution than published version

Published
2017
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15. Observational Evidence of a Flux Rope within a Sunspot Umbra

Author

Guglielmino, Salvo L., Romano, Paolo, and Zuccarello, Francesca

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We observed an elongated filamentary bright structure inside the umbra of the big sunspot in active region NOAA 12529, which differs from the light bridges usually observed in sunspots for its morphology, magnetic configuration, and velocity field. We used observations taken with the Solar Dynamic Observatory satellite to characterize this feature. Its lifetime is 5 days, during which it reaches a maximum length of about 30". In the maps of the vertical component of the photospheric magnetic field, a portion of the feature has a polarity opposite to that of the hosting sunspot. At the same time, in the entire feature the horizontal component of the magnetic field is about 2000 G, substantially stronger than in the surrounding penumbral filaments. Doppler velocity maps reveal the presence of both upward and downward plasma motions along the structure at the photospheric level. Moreover, looking at the chromospheric level, we noted that it is located in a region corresponding to the edge of a small filament which seems rooted in the sunspot umbra. Therefore, we interpreted the bright structure as the photospheric counterpart of a flux rope touching the sunspot and giving rise to penumbral-like filaments in the umbra., Comment: 6 pages, 3 figures, accepted for ApJL

Published
2017
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16. The Solar Particle Acceleration Radiation and Kinetics (SPARK) Mission Concept

Author

Hamish A. S. Reid, Sophie Musset, Daniel F. Ryan, Vincenzo Andretta, Frédéric Auchère, Deborah Baker, Federico Benvenuto, Philippa Browning, Éric Buchlin, Ariadna Calcines Rosario, Steven D. Christe, Alain Jody Corso, Joel Dahlin, Silvia Dalla, Giulio Del Zanna, Carsten Denker, Jaroslav Dudík, Robertus Erdélyi, Ilaria Ermolli, Lyndsay Fletcher, Andrzej Fludra, Lucie M. Green, Mykola Gordovskyy, Salvo L. Guglielmino, Iain Hannah, Richard Harrison, Laura A. Hayes, Andrew R. Inglis, Natasha L. S. Jeffrey, Jana Kašparová, Graham S. Kerr, Christian Kintziger, Eduard P. Kontar, Säm Krucker, Timo Laitinen, Philippe Laurent, Olivier Limousin, David M. Long, Shane A. Maloney, Paolo Massa, Anna Maria Massone, Sarah Matthews, Tomasz Mrozek, Valery M. Nakariakov, Susanna Parenti, Michele Piana, Vanessa Polito, Melissa Pesce-Rollins, Paolo Romano, Alexis P. Rouillard, Clementina Sasso, Albert Y. Shih, Marek Stęślicki, David Orozco Suárez, Luca Teriaca, Meetu Verma, Astrid M. Veronig, Nicole Vilmer, Christian Vocks, and Alexander Warmuth

Subjects
particle acceleration, magnetic reconnection, instrumentation, corona, coronal mass ejections (CMEs), flares, Motor vehicles. Aeronautics. Astronautics, TL1-4050
Abstract

Particle acceleration is a fundamental process arising in many astrophysical objects, including active galactic nuclei, black holes, neutron stars, gamma-ray bursts, accretion disks, solar and stellar coronae, and planetary magnetospheres. Its ubiquity means energetic particles permeate the Universe and influence the conditions for the emergence and continuation of life. In our solar system, the Sun is the most energetic particle accelerator, and its proximity makes it a unique laboratory in which to explore astrophysical particle acceleration. However, despite its importance, the physics underlying solar particle acceleration remain poorly understood. The SPARK mission will reveal new discoveries about particle acceleration through a uniquely powerful and complete combination of γ-ray, X-ray, and EUV imaging and spectroscopy at high spectral, spatial, and temporal resolutions. SPARK’s instruments will provide a step change in observational capability, enabling fundamental breakthroughs in our understanding of solar particle acceleration and the phenomena associated with it, such as the evolution of solar eruptive events. By providing essential diagnostics of the processes that drive the onset and evolution of solar flares and coronal mass ejections, SPARK will elucidate the underlying physics of space weather events that can damage satellites and power grids, disrupt telecommunications and GPS navigation, and endanger astronauts in space. The prediction of such events and the mitigation of their potential impacts are crucial in protecting our terrestrial and space-based infrastructure.

Published
2023
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17. Coronal Heating Rate in the Slow Solar Wind

Author

Daniele Telloni, Marco Romoli, Marco Velli, Gary P. Zank, Laxman Adhikari, Cooper Downs, Aleksandr Burtovoi, Roberto Susino, Daniele Spadaro, Lingling Zhao, Alessandro Liberatore, Chen Shi, Yara De Leo, Lucia Abbo, Federica Frassati, Giovanna Jerse, Federico Landini, Gianalfredo Nicolini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Arkadiusz Berlicki, Roberto Bruno, Gerardo Capobianco, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D’Amicis, Michele Fabi, Fabio Frassetto, Marina Giarrusso, Silvio Giordano, Salvo L. Guglielmino, Enrico Magli, Giuseppe Massone, Mauro Messerotti, Giuseppe Nisticò, Maria G. Pelizzo, Fabio Reale, Paolo Romano, Udo Schühle, Sami K. Solanki, Thomas Straus, Rita Ventura, Cosimo A. Volpicelli, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella, Stuart D. Bale, and Justin C. Kasper

Subjects
Magnetohydrodynamics, Magnetohydrodynamical simulations, Interplanetary turbulence, Solar corona, Solar coronal heating, Solar wind, Astrophysics, QB460-466
Abstract

This Letter reports the first observational estimate of the heating rate in the slowly expanding solar corona. The analysis exploits the simultaneous remote and local observations of the same coronal plasma volume, with the Solar Orbiter/Metis and the Parker Solar Probe instruments, respectively, and relies on the basic solar wind magnetohydrodynamic equations. As expected, energy losses are a minor fraction of the solar wind energy flux, since most of the energy dissipation that feeds the heating and acceleration of the coronal flow occurs much closer to the Sun than the heights probed in the present study, which range from 6.3 to 13.3 R _⊙ . The energy deposited to the supersonic wind is then used to explain the observed slight residual wind acceleration and to maintain the plasma in a nonadiabatic state. As derived in the Wentzel–Kramers–Brillouin limit, the present energy transfer rate estimates provide a lower limit, which can be very useful in refining the turbulence-based modeling of coronal heating and subsequent solar wind acceleration.

Published
2023
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18. The Canadian Hypoglycemia During Hospitalization Score Is Externally Valid in the Australian Diabetes IN-hospital: Glucose & Outcomes (DINGO) Cohort

Author

Di Salvo, L, Barmanray, RD, Andrews, E, Kyi, M, Fazio, TN, Lowe, J, Fourlanos, S, Di Salvo, L, Barmanray, RD, Andrews, E, Kyi, M, Fazio, TN, Lowe, J, and Fourlanos, S

Abstract

OBJECTIVES: The Hypoglycemia During Hospitalization (HyDHo) score predicts hypoglycemia in a population of Canadian inpatients by assigning various weightings to 5 key clinical criteria known at the time of admission, in particular age, recent presentation to an emergency department, insulin use, use of oral hypoglycemic agents, and chronic kidney disease. Our aim in this study was to externally validate the HyDHo score by applying this risk calculator to an Australian population of inpatients with diabetes. METHODS: This study was a retrospective data analysis of a subset of the Diabetes IN-hospital: Glucose & Outcomes (DINGO) cohort. The HyDHo score was applied based on clinical information known at the time of admission to stratify risk of inpatient hypoglycemia. RESULTS: The HyDHo score was applied to 1,015 patients, generating a receiver-operating characteristic c-statistic of 0.607. A threshold of ≥9, as per the original study, generated a sensitivity of 83% and a specificity of 20%. A threshold of ≥10, to better suit this Australian population, generated a sensitivity of 90% and a specificity of 34%. The HyDHo score has been externally valid in a geographically different population; in fact, it outperformed the original study after accounting for local hypoglycemia rates. CONCLUSIONS: Our findings support the external validity of the HyDHo score in a geographically different population. Application of this simple and accessible tool can serve as an adjunct to predict an inpatient's risk of hypoglycemia and guide more appropriate glucose monitoring and diabetes management.

Published
2024

24. Computer simulation of the microstructure and rheology of semi-solid alloys under shear

Author

Perez, M., Barbe, J-C., Neda, Z., Brechet, Y., and Salvo, L.

Subjects
Condensed Matter - Materials Science, Condensed Matter - Soft Condensed Matter
Abstract

The rheological behavior of metallic alloys containing both solid and liquid phases is investigated in the low solid fraction range (<50%). This behavior depends on both the solid fraction and the shear rate. The concept of Effective Volume Fraction (EVF) is used to decorrelate the influence of these two parameters. At high shear rate the slurry behaves like a suspension of hard spheres, whereas at lower shear rate, particles tend to aggregate in clusters, entrapping liquid and thus, increasing the EVF and the viscosity. A lattice model is introduced to simulate the aggregation / break-up processes within a slurry under shear. When the steady state is reached, the entrapped liquid fraction is calculated, leading to a viscosity estimation. Simulation results for the viscosity and 3D cluster structure are in good agreement with experimental results., Comment: 30 pages, 17 figures, to be published in Acta Mater

Published
2000

25. Coronal Heating Rate in the Slow Solar Wind

Author

Telloni, Daniele, primary, Romoli, Marco, additional, Velli, Marco, additional, Zank, Gary P., additional, Adhikari, Laxman, additional, Downs, Cooper, additional, Burtovoi, Aleksandr, additional, Susino, Roberto, additional, Spadaro, Daniele, additional, Zhao, Lingling, additional, Liberatore, Alessandro, additional, Shi, Chen, additional, De Leo, Yara, additional, Abbo, Lucia, additional, Frassati, Federica, additional, Jerse, Giovanna, additional, Landini, Federico, additional, Nicolini, Gianalfredo, additional, Pancrazzi, Maurizio, additional, Russano, Giuliana, additional, Sasso, Clementina, additional, Andretta, Vincenzo, additional, Da Deppo, Vania, additional, Fineschi, Silvano, additional, Grimani, Catia, additional, Heinzel, Petr, additional, Moses, John D., additional, Naletto, Giampiero, additional, Stangalini, Marco, additional, Teriaca, Luca, additional, Uslenghi, Michela, additional, Berlicki, Arkadiusz, additional, Bruno, Roberto, additional, Capobianco, Gerardo, additional, Capuano, Giuseppe E., additional, Casini, Chiara, additional, Casti, Marta, additional, Chioetto, Paolo, additional, Corso, Alain J., additional, D’Amicis, Raffaella, additional, Fabi, Michele, additional, Frassetto, Fabio, additional, Giarrusso, Marina, additional, Giordano, Silvio, additional, Guglielmino, Salvo L., additional, Magli, Enrico, additional, Massone, Giuseppe, additional, Messerotti, Mauro, additional, Nisticò, Giuseppe, additional, Pelizzo, Maria G., additional, Reale, Fabio, additional, Romano, Paolo, additional, Schühle, Udo, additional, Solanki, Sami K., additional, Straus, Thomas, additional, Ventura, Rita, additional, Volpicelli, Cosimo A., additional, Zangrilli, Luca, additional, Zimbardo, Gaetano, additional, Zuppella, Paola, additional, Bale, Stuart D., additional, and Kasper, Justin C., additional

Published
2023
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26. Firefly: The Case for a Holistic Understanding of the Global Structure and Dynamics of the Sun and the Heliosphere

Author

Raouafi, Nour E., primary, Hoeksema, J. Todd, additional, Newmark, Jeffrey S., additional, Gibson, Sarah, additional, Berger, Thomas E., additional, Upton, Lisa A., additional, Vourlidas, Angelos, additional, Hassler, Donald M., additional, Kinnison, James, additional, Ho, George C., additional, Mason, Glenn M., additional, Vievering, Juliana T., additional, Viall, Nicholeen M., additional, Szabo, Adam, additional, Casti, Marta, additional, Case, Anthony W., additional, Lepri, Susan T., additional, Velli, Marco, additional, Georgoulis, Manolis K., additional, Bourouaine, Sofiane, additional, Jagarlamudi, Vamsee K., additional, Laming, John M., additional, Mason, James P., additional, Harra, Louise, additional, Madjarska, Maria, additional, Chitta, Lakshmi Pradeep, additional, Duran, J. Sebastian Castellanos, additional, Korpi-Lagg, Andreas, additional, Badman, Samuel, additional, Chifu, Iulia, additional, Lario, David, additional, Wing, Simon, additional, Bale, Stuart, additional, Paouris, Evangelos, additional, Narayanamurthy, Smitha, additional, Sinjan, Jonas, additional, Bernasconi, Pietro, additional, Krivova, Natalie, additional, Gizon, Laurent, additional, Leamon, Robert J., additional, Gosain, Sanjay, additional, Kazachenko, Maria, additional, Petrie, Gordon, additional, Pillet, Valentin Martinez, additional, Jain, Kiran, additional, Luhmann, Janet, additional, Bertello, Luca, additional, Toriumi, Shin, additional, Jiang, Chen, additional, Vasko, Ivan, additional, Harvey, John W., additional, Schad, Thomas A., additional, Jebaraj, Immanuel C., additional, Scherrer, Philip, additional, Hofmeister, Stefan, additional, Tiwari, Sanjiv, additional, Wang, Haimin, additional, Roth, Markus, additional, Panesar, Navdeep, additional, Sekii, Takashi, additional, Magyar, Norbert, additional, Guglielmino, Salvo L., additional, Parenti, Susanna, additional, Tremblay, Benoit, additional, Tziotziou, Kostas, additional, Toma, Giuliana de, additional, Chen, Bin, additional, Katsukawa, Yukio, additional, Pontieu, Bart De, additional, Cheng, Xin, additional, Cheung, Mark, additional, Kosovichev, Alexander, additional, Jiang, Jie, additional, Schunker, Hannah, additional, Kawabata, Yusuke, additional, Oba, Takayoshi, additional, Cameron, Robert, additional, Mathew, Shibu K., additional, Rodriguez, Jaime de la Cruz, additional, Kusano, Kanya, additional, Temmer, Manuela, additional, Andretta, Vincenzo, additional, Sven, Wedemeyer, additional, Samara, Evangelia, additional, Heinemann, Stephan G., additional, Warmuth, Alexander, additional, Jafarzadeh, Shahin, additional, Mackay, Duncan H., additional, Fludra, Andrzej, additional, Rubio, Luis Bellot, additional, Suárez, David Orozco, additional, Chen, Thomas Y., additional, Kontogiannis, Ioannis, additional, Yardley, Stephanie, additional, Veronig, Astrid, additional, Joshi, Jayant, additional, Spadaro, Daniele, additional, Kubo, Masahito, additional, Bose, Souvik, additional, González, Nazaret Bello, additional, Solanki, Sami, additional, Denker, Carsten, additional, Verma, Meetu, additional, Vocks, Christian, additional, Borrero, Juan Manuel, additional, Mathews, Nathaniel H., additional, Cury, Shannon, additional, Sasso, Clementina, additional, Stenborg, Guillermo, additional, Tibebu, Getachew, additional, Battams, Karl, additional, Wijsen, Nicolas, additional, Bruno, Alessandro, additional, Peter, Hardi, additional, I., Mason Emily, additional, M., Caplan Ronald, additional, Martinez-Sykora, Juan, additional, Seaton, Daniel, additional, Airapetian, Vladimir, additional, Jian, Lan, additional, Thompson, William T., additional, Ofman, Leon, additional, Wallace, Samantha, additional, Kucera, Therese, additional, Desai, Ravindra, additional, Richardson, Ian, additional, Burkepile, Joan, additional, Cranmer, Steven, additional, Strauss, R. Du Toit, additional, Murabito, Mariarita, additional, Alfred, De Wijn, additional, Xie, Hong, additional, Rempel, Matthias, additional, Webber, Shea Hess, additional, Reeves, Katharine K., additional, Hurlburt, Neal, additional, Berrilli, Francesco, additional, DeLuca, Edward, additional, Egeland, Ricky, additional, Ko, Yuan-Kuen, additional, Kee, Nathaniel Dylan, additional, Mahajan, Sushant S., additional, Craig, DeForest, additional, Wood, Brian E., additional, Chris, Chaston, additional, Nigro, Giuseppina, additional, Shaik, Shaheda Begum, additional, Gosic, Milan, additional, Shimizu, Toshifumi, additional, Zuccarello, Francesca, additional, Nitta, Nariaki, additional, Chatzistergos, Theodosios, additional, Fan, Yuhong, additional, Zhang, Jie, additional, Fehlmann, Andre, additional, Palmerio, Erika, additional, Ishikawa, Ryohtaroh T., additional, Danilovic, Sanja, additional, Skan, Moa, additional, Froment, Clara, additional, Baso, Carlos José Díaz, additional, Liang, Zhi-Chao, additional, Wit, Thierry Dudok de, additional, Barczynski, Krzysztof, additional, Johnston, Craig, additional, Pariat, Etienne, additional, Hadid, Lina, additional, Aulanier, Guillaume, additional, Brun, Allan Sacha, additional, Athanasios, Kouloumvakos, additional, Cauzzi, Gianna, additional, Dredger, Pauline, additional, French, Ryan, additional, Christian, Damian, additional, Linton, Mark, additional, Ireland, Jack, additional, Tarr, Lucas, additional, Strugarek, Antoine, additional, Uritsky, Vadim, additional, DeRosa, Marc, additional, Kretzschmar, Matthieu, additional, García, Rafael A., additional, Monteiro, Mario J. P. F. G., additional, Mathur, Savita, additional, Breton, Sylvain N., additional, Pinto, Rui F., additional, Oliveros, Juan Carlos Martinez, additional, Loper, Robert, additional, Auchère, Frédéric, additional, Wang, Tongjiang, additional, Reginald, Nelson, additional, Cunha, Margarida S., additional, Teriaca, Luca, additional, Chintzoglou, Georgios, additional, Lynch, Benjamin J., additional, Linker, Jon, additional, Beck, Paul, additional, Shannon, Jackson, additional, Clare, Benjamin, additional, Krupiarz, Christopher, additional, Whiting, Ian D., additional, Byerly, Adam, additional, Bushman, Stewart, additional, Carrelli, David, additional, Kijewski, Seth, additional, Englander, Jacob, additional, Mizes, Adam, additional, Porter, Jamie, additional, O’Neill, Michael, additional, Chattopadhyay, Debarati, additional, Albers, Joshua, additional, Rast, Mark, additional, Ermolli, Ilaria, additional, Tzeng, Nigel, additional, Hudson, James F., additional, Giunta, Alessandra, additional, Buchlin, Éric, additional, Bommier, Véronique, additional, Duncan, Nicole, additional, Janvier, Miho, additional, Strecker, Hanna, additional, Siu, Azaymi, additional, Perri, Barbara, additional, Maksimovic, Milan, additional, Vilmer, Nicole, additional, Toledo-Redondo, Sergio, additional, Kuckein, Christoph, additional, Alberti, Tommaso, additional, Antolin, Patrick, additional, Cuadrado, Regina Aznar, additional, Berghmans, David, additional, Brigitte, Schmieder, additional, Bucik, Radoslav, additional, Calchetti, Daniele, additional, Caspi, Amir, additional, Cohen, Christina, additional, Corbard, Thierry, additional, Cremades, Hebe, additional, Cummings, Alan, additional, Dhakal, Suman, additional, Dolla, Laurent, additional, Dominique, Marie, additional, Emslie, Gordon, additional, Ferrente, Fabiana, additional, Finley, Adam J., additional, Fletcher, Lyndsay, additional, Fraschetti, Federico, additional, Gafeira, Ricardo, additional, Gissot, Samuel, additional, Hegde, Dinesha, additional, Hu, Qiang, additional, Innocenti, Maria Elena, additional, Jin, Meng, additional, Klein, Kristopher, additional, Kumar, Pankaj, additional, Lacatus, Daniela, additional, Liewer, Paulett, additional, Magdalenic, Jasmina, additional, Mandal, Sudip, additional, Mandrini, Cristina H., additional, Mierla, Marilena, additional, Miralles, Mari Paz, additional, Moore, Ron, additional, Neville, Jonathan, additional, Niembro, Tatiana, additional, Nikou, Eleni, additional, Nindos, Alexander, additional, Papaioannou, Athanasios, additional, Rajaguru, S. Paul, additional, Reville, Victor, additional, Rochus, Pierre, additional, Rodriguez, Luciano, additional, Romoli, Marco, additional, Shestov, Sergei, additional, Shi, Chen, additional, Sorriso-Valvo, Luca, additional, St. Cyr, O. C., additional, Sterling, Alphohse, additional, Stevens, Michael L., additional, Susino, Roberto, additional, Swisdak, Marc, additional, Thompson, Barbara J., additional, Valliappan, Senthamizh Pavai, additional, Verbeeck, Francis, additional, Bothmer, Volker, additional, Xudong, Sun, additional, Zhukov, Andrei, additional, Katsiyannis, Thanassis, additional, Owen, Christopher, additional, Karna, Nishu, additional, Janssens, Jan, additional, Khomenko, Elena, additional, Gary, Dale, additional, Bandyopadhyay, Riddhi, additional, Chhiber, Rohit, additional, Tenerani, Anna, additional, Rouillard, Alexis, additional, Patsourakos, Spiros, additional, Anastasiadis, Anastasios, additional, Bocchialini, Karine, additional, Moraitis, Kostas, additional, Rivera, Yeimy, additional, Drake, James, additional, Baudin, Frédéric, additional, Chandran, Benjamin, additional, Dayeh, Maher, additional, Reardon, Kevin, additional, Cairns, Iver, additional, Bizien, Nina, additional, Wexler, David, additional, Bahauddin, Shah, additional, Rodriguez-Pacheco, Javier, additional, Yu, Sijie, additional, Lee, Jeongwoo, additional, Gontikakis, Costis, additional, Koukras, Alexandros, additional, Contel, Olivier Le, additional, Pezzi, Oreste, additional, Kintziger, Christian, additional, Boumier, Patrick, additional, Balasis, Georgios, additional, Dikpati, Mausumi, additional, Pesnell, W. Dean, additional, Chai, Yi, additional, Nandy, Dibyendu, additional, Charles, Arge, additional, Corti, Claudio, additional, Zhao, Lulu, additional, Matthaeus, William H., additional, Gilly, Chris R., additional, Erlandson, Robert E., additional, Derouich, Moncef, additional, Zhao, Lingling, additional, Poedts, Stefaan, additional, Vieira, Luis, additional, Adhikari, Laxman, additional, Buitrago-Casas, Juan Camilo, additional, Huang, Jia, additional, Moestl, Christian, additional, Liu, Mingzhe, additional, Oloketuyi, Jacob, additional, Zhuang, Bin, additional, Rodríguez-García, Laura, additional, Perez, Jean Carlos, additional, Xu, Zigong, additional, Kooi, Jason, additional, Woodham, Lloyd D., additional, Tripathi, Durgesh, additional, Young, Peter, additional, López-Portela, Cynthia, additional, Cuesta, Manuel Enrique, additional, and Wilson, Lynn, additional

Published
2023
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30. The Solar Particle Acceleration Radiation and Kinetics (SPARK) Mission Concept

Author

Reid, Hamish A. S., Musset, Sophie, Ryan, Daniel F., Andretta, Vincenzo, Auchère, Frédéric, Baker, Deborah, Benvenuto, Federico, Browning, Philippa, Buchlin, Éric, Calcines Rosario, Ariadna, Christe, Steven D., Corso, Alain Jody, Dahlin, Joel, Dalla, Silvia, Del Zanna, Giulio, Denker, Carsten, Dudík, Jaroslav, Erdélyi, Robertus, Ermolli, Ilaria, Fletcher, Lyndsay, Fludra, Andrzej, Green, Lucie M., Gordovskyy, Mykola, Guglielmino, Salvo L., Hannah, Iain, Harrison, Richard, Hayes, Laura A., Inglis, Andrew R., Jeffrey, Natasha L. S., Kašparová, Jana, Kerr, Graham S., Kintziger, Christian, Kontar, Eduard P., Krucker, Säm, Laitinen, Timo, Laurent, Philippe, Limousin, Olivier, Long, David M., Maloney, Shane A., Massa, Paolo, Massone, Anna Maria, Matthews, Sarah, Mrozek, Tomasz, Nakariakov, Valery M., Parenti, Susanna, Piana, Michele, Polito, Vanessa, Pesce-Rollins, Melissa, Romano, Paolo, Rouillard, Alexis P., Sasso, Clementina, Shih, Albert Y., Stęślicki, Marek, Orozco Suárez, David, Teriaca, Luca, Verma, Meetu, Veronig, Astrid M., Vilmer, Nicole, Vocks, Christian, Warmuth, Alexander, Reid, Hamish A. S., Musset, Sophie, Ryan, Daniel F., Andretta, Vincenzo, Auchère, Frédéric, Baker, Deborah, Benvenuto, Federico, Browning, Philippa, Buchlin, Éric, Calcines Rosario, Ariadna, Christe, Steven D., Corso, Alain Jody, Dahlin, Joel, Dalla, Silvia, Del Zanna, Giulio, Denker, Carsten, Dudík, Jaroslav, Erdélyi, Robertus, Ermolli, Ilaria, Fletcher, Lyndsay, Fludra, Andrzej, Green, Lucie M., Gordovskyy, Mykola, Guglielmino, Salvo L., Hannah, Iain, Harrison, Richard, Hayes, Laura A., Inglis, Andrew R., Jeffrey, Natasha L. S., Kašparová, Jana, Kerr, Graham S., Kintziger, Christian, Kontar, Eduard P., Krucker, Säm, Laitinen, Timo, Laurent, Philippe, Limousin, Olivier, Long, David M., Maloney, Shane A., Massa, Paolo, Massone, Anna Maria, Matthews, Sarah, Mrozek, Tomasz, Nakariakov, Valery M., Parenti, Susanna, Piana, Michele, Polito, Vanessa, Pesce-Rollins, Melissa, Romano, Paolo, Rouillard, Alexis P., Sasso, Clementina, Shih, Albert Y., Stęślicki, Marek, Orozco Suárez, David, Teriaca, Luca, Verma, Meetu, Veronig, Astrid M., Vilmer, Nicole, Vocks, Christian, and Warmuth, Alexander

Abstract

Particle acceleration is a fundamental process arising in many astrophysical objects, including active galactic nuclei, black holes, neutron stars, gamma-ray bursts, accretion disks, solar and stellar coronae, and planetary magnetospheres. Its ubiquity means energetic particles permeate the Universe and influence the conditions for the emergence and continuation of life. In our solar system, the Sun is the most energetic particle accelerator, and its proximity makes it a unique laboratory in which to explore astrophysical particle acceleration. However, despite its importance, the physics underlying solar particle acceleration remain poorly understood. The SPARK mission will reveal new discoveries about particle acceleration through a uniquely powerful and complete combination of γ-ray, X-ray, and EUV imaging and spectroscopy at high spectral, spatial, and temporal resolutions. SPARK’s instruments will provide a step change in observational capability, enabling fundamental breakthroughs in our understanding of solar particle acceleration and the phenomena associated with it, such as the evolution of solar eruptive events. By providing essential diagnostics of the processes that drive the onset and evolution of solar flares and coronal mass ejections, SPARK will elucidate the underlying physics of space weather events that can damage satellites and power grids, disrupt telecommunications and GPS navigation, and endanger astronauts in space. The prediction of such events and the mitigation of their potential impacts are crucial in protecting our terrestrial and space-based infrastructure.

Published
2023

33. IRIS Observations of Magnetic Interactions in the Solar Atmosphere Between Preexisting and Emerging Magnetic Fields. II. UV Emission Properties

Author

Guglielmino, Salvo L, Young, Peter R, and Zuccarello, Francesca

Subjects
Solar Physics
Abstract

Multiwavelength ultraviolet (UV) observations by the Interface Region Imaging Spectrograph satellite in active region NOAA 12529 have recently pointed out the presence of long-lasting brightenings, akin to UV bursts, and simultaneous plasma ejections occurring in the upper chromosphere and transition region during secondary flux emergence. These signatures have been interpreted as evidence of small-scale, recurrent magnetic reconnection episodes between the emerging flux region (EFR) and the preexisting plage field. Here we characterize the UV emission of these strong, intermittent brightenings and study the surge activity above the chromospheric arch filament system (AFS) overlying the EFR. We analyze the surges and the cospatial brightenings observed at different wavelengths. We find an asymmetry in the emission between the blue and red wings of the Si iv λ1402 Å and Mg ii k λ2796.3 lines, which clearly outlines the dynamics of the structures above the AFS that form during the small-scale eruptive phenomena. We also detect a correlation between the Doppler velocity and skewness of the Si iv λλ1394 and 1402 line profiles in the UV burst pixels. Finally, we show that genuine emission in the Fe xii λ1349.4 line is cospatial to the Si iv brightenings. This definitely reveals a pure coronal counterpart to the reconnection event.

Published
2019
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39. Linking Small-scale Solar Wind Properties with Large-scale Coronal Source Regions through Joint Parker Solar Probe–Metis/Solar Orbiter Observations

Author

Telloni, Daniele, primary, Zank, Gary P., additional, Sorriso-Valvo, Luca, additional, D’Amicis, Raffaella, additional, Panasenco, Olga, additional, Susino, Roberto, additional, Bruno, Roberto, additional, Perrone, Denise, additional, Adhikari, Laxman, additional, Liang, Haoming, additional, Nakanotani, Masaru, additional, Zhao, Lingling, additional, Hadid, Lina Z., additional, Sánchez-Cano, Beatriz, additional, Verscharen, Daniel, additional, Velli, Marco, additional, Grimani, Catia, additional, Marino, Raffaele, additional, Carbone, Francesco, additional, Mancuso, Salvatore, additional, Biondo, Ruggero, additional, Pagano, Paolo, additional, Reale, Fabio, additional, Bale, Stuart D., additional, Kasper, Justin C., additional, Case, Anthony W., additional, de Wit, Thierry Dudok, additional, Goetz, Keith, additional, Harvey, Peter R., additional, Korreck, Kelly E., additional, Larson, Davin, additional, Livi, Roberto, additional, MacDowall, Robert J., additional, Malaspina, David M., additional, Pulupa, Marc, additional, Stevens, Michael L., additional, Whittlesey, Phyllis, additional, Romoli, Marco, additional, Andretta, Vincenzo, additional, Deppo, Vania Da, additional, Fineschi, Silvano, additional, Heinzel, Petr, additional, Moses, John D., additional, Naletto, Giampiero, additional, Nicolini, Gianalfredo, additional, Spadaro, Daniele, additional, Stangalini, Marco, additional, Teriaca, Luca, additional, Capobianco, Gerardo, additional, Capuano, Giuseppe E., additional, Casini, Chiara, additional, Casti, Marta, additional, Chioetto, Paolo, additional, Corso, Alain J., additional, Leo, Yara De, additional, Fabi, Michele, additional, Frassati, Federica, additional, Frassetto, Fabio, additional, Giordano, Silvio, additional, Guglielmino, Salvo L., additional, Jerse, Giovanna, additional, Landini, Federico, additional, Liberatore, Alessandro, additional, Magli, Enrico, additional, Massone, Giuseppe, additional, Messerotti, Mauro, additional, Pancrazzi, Maurizio, additional, Pelizzo, Maria G., additional, Romano, Paolo, additional, Sasso, Clementina, additional, Schühle, Udo, additional, Slemer, Alessandra, additional, Straus, Thomas, additional, Uslenghi, Michela, additional, Volpicelli, Cosimo A., additional, Zangrilli, Luca, additional, Zuppella, Paola, additional, Abbo, Lucia, additional, Auchère, Frédéric, additional, Cuadrado, Regina Aznar, additional, Berlicki, Arkadiusz, additional, Ciaravella, Angela, additional, Lamy, Philippe, additional, Lanzafame, Alessandro, additional, Malvezzi, Marco, additional, Nicolosi, Piergiorgio, additional, Nisticò, Giuseppe, additional, Peter, Hardi, additional, Solanki, Sami K., additional, Strachan, Leonard, additional, Tsinganos, Kanaris, additional, Ventura, Rita, additional, Vial, Jean-Claude, additional, Woch, Joachim, additional, and Zimbardo, Gaetano, additional

Published
2022
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41. Linking Small-scale Solar Wind Properties with Large-scale Coronal Source Regions through Joint Parker Solar Probe-Metis/Solar Orbiter Observations

Author

Telloni, Daniele, Zank, Gary P., Sorriso-Valvo, Luca, D'Amicis, Raffaella, Panasenco, Olga, Susino, Roberto, Bruno, Roberto, Perrone, Denise, Adhikari, Laxman, Liang, Haoming, Nakanotani, Masaru, Zhao, Lingling, Hadid, Lina Z., Sanchez-Cano, Beatriz, Verscharen, Daniel, Velli, Marco, Grimani, Catia, Marino, Raffaele, Carbone, Francesco, Mancuso, Salvatore, Biondo, Ruggero, Pagano, Paolo, Reale, Fabio, Bale, Stuart D., Kasper, Justin C., Case, Anthony W., de Wit, Thierry Dudok, Goetz, Keith, Harvey, Peter R., Korreck, Kelly E., Larson, Davin, Livi, Roberto, MacDowall, Robert J., Malaspina, David M., Pulupa, Marc, Stevens, Michael L., Whittlesey, Phyllis, Romoli, Marco, Andretta, Vincenzo, Da Deppo, Vania, Fineschi, Silvano, Heinzel, Petr, Moses, John D., Naletto, Giampiero, Nicolini, Gianalfredo, Spadaro, Daniele, Stangalini, Marco, Teriaca, Luca, Capobianco, Gerardo, Capuano, Giuseppe E., Casini, Chiara, Casti, Marta, Chioetto, Paolo, Corso, Alain J., De Leo, Yara, Fabi, Michele, Frassati, Federica, Frassetto, Fabio, Giordano, Silvio, Guglielmino, Salvo L., Jerse, Giovanna, Landini, Federico, Liberatore, Alessandro, Magli, Enrico, Massone, Giuseppe, Messerotti, Mauro, Pancrazzi, Maurizio, Pelizzo, Maria G., Romano, Paolo, Sasso, Clementina, Schuhle, Udo, Slemer, Alessandra, Straus, Thomas, Uslenghi, Michela, Volpicelli, Cosimo A., Zangrilli, Luca, Zuppella, Paola, Abbo, Lucia, Auchere, Frederic, Cuadrado, Regina Aznar, Berlicki, Arkadiusz, Ciaravella, Angela, Lamy, Philippe, Lanzafame, Alessandro, Malvezzi, Marco, Nicolosi, Piergiorgio, Nistico, Giuseppe, Peter, Hardi, Solanki, Sami K., Strachan, Leonard, Tsinganos, Kanaris, Ventura, Rita, Vial, Jean-Claude, Woch, Joachim, Zimbardo, Gaetano, Telloni, Daniele, Zank, Gary P., Sorriso-Valvo, Luca, D'Amicis, Raffaella, Panasenco, Olga, Susino, Roberto, Bruno, Roberto, Perrone, Denise, Adhikari, Laxman, Liang, Haoming, Nakanotani, Masaru, Zhao, Lingling, Hadid, Lina Z., Sanchez-Cano, Beatriz, Verscharen, Daniel, Velli, Marco, Grimani, Catia, Marino, Raffaele, Carbone, Francesco, Mancuso, Salvatore, Biondo, Ruggero, Pagano, Paolo, Reale, Fabio, Bale, Stuart D., Kasper, Justin C., Case, Anthony W., de Wit, Thierry Dudok, Goetz, Keith, Harvey, Peter R., Korreck, Kelly E., Larson, Davin, Livi, Roberto, MacDowall, Robert J., Malaspina, David M., Pulupa, Marc, Stevens, Michael L., Whittlesey, Phyllis, Romoli, Marco, Andretta, Vincenzo, Da Deppo, Vania, Fineschi, Silvano, Heinzel, Petr, Moses, John D., Naletto, Giampiero, Nicolini, Gianalfredo, Spadaro, Daniele, Stangalini, Marco, Teriaca, Luca, Capobianco, Gerardo, Capuano, Giuseppe E., Casini, Chiara, Casti, Marta, Chioetto, Paolo, Corso, Alain J., De Leo, Yara, Fabi, Michele, Frassati, Federica, Frassetto, Fabio, Giordano, Silvio, Guglielmino, Salvo L., Jerse, Giovanna, Landini, Federico, Liberatore, Alessandro, Magli, Enrico, Massone, Giuseppe, Messerotti, Mauro, Pancrazzi, Maurizio, Pelizzo, Maria G., Romano, Paolo, Sasso, Clementina, Schuhle, Udo, Slemer, Alessandra, Straus, Thomas, Uslenghi, Michela, Volpicelli, Cosimo A., Zangrilli, Luca, Zuppella, Paola, Abbo, Lucia, Auchere, Frederic, Cuadrado, Regina Aznar, Berlicki, Arkadiusz, Ciaravella, Angela, Lamy, Philippe, Lanzafame, Alessandro, Malvezzi, Marco, Nicolosi, Piergiorgio, Nistico, Giuseppe, Peter, Hardi, Solanki, Sami K., Strachan, Leonard, Tsinganos, Kanaris, Ventura, Rita, Vial, Jean-Claude, Woch, Joachim, and Zimbardo, Gaetano

Abstract

The solar wind measured in situ by Parker Solar Probe in the very inner heliosphere is studied in combination with the remote-sensing observation of the coronal source region provided by the METIS coronagraph aboard Solar Orbiter. The coronal outflows observed near the ecliptic by Metis on 2021 January 17 at 16:30 UT, between 3.5 and 6.3 R (circle dot) above the eastern solar limb, can be associated with the streams sampled by PSP at 0.11 and 0.26 au from the Sun, in two time intervals almost 5 days apart. The two plasma flows come from two distinct source regions, characterized by different magnetic field polarity and intensity at the coronal base. It follows that both the global and local properties of the two streams are different. Specifically, the solar wind emanating from the stronger magnetic field region has a lower bulk flux density, as expected, and is in a state of well-developed Alfvenic turbulence, with low intermittency. This is interpreted in terms of slab turbulence in the context of nearly incompressible magnetohydrodynamics. Conversely, the highly intermittent and poorly developed turbulent behavior of the solar wind from the weaker magnetic field region is presumably due to large magnetic deflections most likely attributed to the presence of switchbacks of interchange reconnection origin.

Published
2022
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44. On the Evolution of a Sub-C Class Flare: A Showcase for the Capabilities of the Revamped Catania Solar Telescope

Author

Paolo Romano, Salvo L. Guglielmino, Pierfrancesco Costa, Mariachiara Falco, Salvatore Buttaccio, Alessandro Costa, Eugenio Martinetti, Giovanni Occhipinti, Daniele Spadaro, Rita Ventura, Giuseppe E. Capuano, Francesca Zuccarello, and ITA

Subjects
Astrophysics - Solar and Stellar Astrophysics, Flares, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Instrumentation and data management, Dynamics
Abstract

Solar flares are occasionally responsible for severe space-weather events, which can affect space-borne and ground-based infrastructures, endangering anthropic technological activities and even human health and safety. Thus, an essential activity in the framework of space-weather monitoring is devoted to the observation of the activity level on the Sun. In this context, the acquisition system of the Catania Solar Telescope has been recently upgraded in order to improve its contribution to the European Space Agency (ESA) - Space Weather Service Network through the ESA Portal, which represents the main asset for space weather in Europe. Here, we describe the hardware and software upgrades of the Catania Solar Telescope and the main data products provided by this facility, which include full-disk images of the photosphere and chromosphere, together with a detailed characterization of sunspot groups. As a showcase of the observational capabilities of the revamped Catania Solar Telescope, we report the analysis of a B5.4 class flare that occurred on 7 December 2020, simultaneously observed by the Interface Region Imaging Spectrograph and the Solar Dynamics Observatory satellites....

Published
2022

45. Linking Small-scale Solar Wind Properties with Large-scale Coronal Source Regions through Joint Parker Solar Probe–Metis/Solar Orbiter Observations

Author

Daniele Telloni, Gary P. Zank, Luca Sorriso-Valvo, Raffaella D’Amicis, Olga Panasenco, Roberto Susino, Roberto Bruno, Denise Perrone, Laxman Adhikari, Haoming Liang, Masaru Nakanotani, Lingling Zhao, Lina Z. Hadid, Beatriz Sánchez-Cano, Daniel Verscharen, Marco Velli, Catia Grimani, Raffaele Marino, Francesco Carbone, Salvatore Mancuso, Ruggero Biondo, Paolo Pagano, Fabio Reale, Stuart D. Bale, Justin C. Kasper, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, David M. Malaspina, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey, Marco Romoli, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Marco Stangalini, Luca Teriaca, Gerardo Capobianco, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Yara De Leo, Michele Fabi, Federica Frassati, Fabio Frassetto, Silvio Giordano, Salvo L. Guglielmino, Giovanna Jerse, Federico Landini, Alessandro Liberatore, Enrico Magli, Giuseppe Massone, Mauro Messerotti, Maurizio Pancrazzi, Maria G. Pelizzo, Paolo Romano, Clementina Sasso, Udo Schühle, Alessandra Slemer, Thomas Straus, Michela Uslenghi, Cosimo A. Volpicelli, Luca Zangrilli, Paola Zuppella, Lucia Abbo, Frédéric Auchère, Regina Aznar Cuadrado, Arkadiusz Berlicki, Angela Ciaravella, Philippe Lamy, Alessandro Lanzafame, Marco Malvezzi, Piergiorgio Nicolosi, Giuseppe Nisticò, Hardi Peter, Sami K. Solanki, Leonard Strachan, Kanaris Tsinganos, Rita Ventura, Jean-Claude Vial, Joachim Woch, Gaetano Zimbardo, Telloni D., Zank G.P., Sorriso-Valvo L., D'amicis R., Panasenco O., Susino R., Bruno R., Perrone D., Adhikari L., Liang H., Nakanotani M., Zhao L., Hadid L.Z., Sanchez-Cano B., Verscharen D., Velli M., Grimani C., Marino R., Carbone F., Mancuso S., Biondo R., Pagano P., Reale F., Bale S.D., Kasper J.C., Case A.W., De Wit T.D., Goetz K., Harvey P.R., Korreck K.E., Larson D., Livi R., Macdowall R.J., Malaspina D.M., Pulupa M., Stevens M.L., Whittlesey P., Romoli M., Andretta V., Deppo V.D., Fineschi S., Heinzel P., Moses J.D., Naletto G., Nicolini G., Spadaro D., Stangalini M., Teriaca L., Capobianco G., Capuano G.E., Casini C., Casti M., Chioetto P., Corso A.J., Leo Y.D., Fabi M., Frassati F., Frassetto F., Giordano S., Guglielmino S.L., Jerse G., Landini F., Liberatore A., Magli E., Massone G., Messerotti M., Pancrazzi M., Pelizzo M.G., Romano P., Sasso C., Schuhle U., Slemer A., Straus T., Uslenghi M., Volpicelli C.A., Zangrilli L., Zuppella P., Abbo L., Auchere F., Cuadrado R.A., Berlicki A., Ciaravella A., Lamy P., Lanzafame A., Malvezzi M., Nicolosi P., Nistico G., Peter H., Solanki S.K., Strachan L., Tsinganos K., Ventura R., Vial J.-C., Woch J., and Zimbardo G.

Subjects
Magnetohydrodynamics (694), Settore FIS/05 - Astronomia E Astrofisica, Astronomi, astrofysik och kosmologi, Space and Planetary Science, Solar corona (1483), Space plasmas (1544), Solar wind (1534), Interplanetary turbulence (830), Astronomy, Astrophysics and Cosmology, Astronomy and Astrophysics, Alfven waves (23), Heliosphere (711)
Abstract

The solar wind measured in situ by Parker Solar Probe in the very inner heliosphere is studied in combination with the remote-sensing observation of the coronal source region provided by the METIS coronagraph aboard Solar Orbiter. The coronal outflows observed near the ecliptic by Metis on 2021 January 17 at 16:30 UT, between 3.5 and 6.3 R ⊙ above the eastern solar limb, can be associated with the streams sampled by PSP at 0.11 and 0.26 au from the Sun, in two time intervals almost 5 days apart. The two plasma flows come from two distinct source regions, characterized by different magnetic field polarity and intensity at the coronal base. It follows that both the global and local properties of the two streams are different. Specifically, the solar wind emanating from the stronger magnetic field region has a lower bulk flux density, as expected, and is in a state of well-developed Alfvénic turbulence, with low intermittency. This is interpreted in terms of slab turbulence in the context of nearly incompressible magnetohydrodynamics. Conversely, the highly intermittent and poorly developed turbulent behavior of the solar wind from the weaker magnetic field region is presumably due to large magnetic deflections most likely attributed to the presence of switchbacks of interchange reconnection origin.

Published
2022

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