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3 results on '"Volpicelli, Cosimo"'

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. 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
Full Text
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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

Froment, C., Krasnoselskikh, V., Agapitov, O., Fargette, N., Lavraud, B., Larosa, A., Kretzschmar, M., Jagarlamudi, V., Velli, Marco, Malaspina, David, Whittlesey, Phyllis, Bale, Stuart, Case, Anthony, Goetz, Keith, Kasper, Justin, Korreck, Kelly, Larson, Davin, MacDowall, Robert, Mozer, F., Pulupa, Marc, Revillet, C., Stevens, Michael, Telloni, Daniele, Andretta, Vincenzo, Antonucci, Ester, Bemporad, Alessandro, Capuano, Giuseppe, Fineschi, Silvano, Giordano, Silvio, Habbal, Shadia, Perrone, Denise, Pinto, Rui, Sorriso-Valvo, Luca, Spadaro, Daniele, Susino, Roberto, Woodham, Lloyd, Zank, Gary, Romoli, Marco, Auchère, Frédéric, Bruno, Roberto, Capobianco, Gerardo, Casini, Chiara, Casti, Marta, Chioetto, Paolo, Corso, Alain, Da Deppo, Vania, De Leo, Yara, Dudok De Wit, Thierry, Frassati, Federica, Frassetto, Fabio, Guglielmino, Salvo, Harvey, Peter, Heinzel, Petr, Jerse, Giovanna, Landini, Federico, Liberatore, Alessandro, Livi, Roberto, Magli, Enrico, Massone, Giuseppe, Messerotti, Mauro, Moses, John, Naletto, Giampiero, Nicolini, Gianalfredo, Nisticò, Giuseppe, Panasenco, Olga, Pancrazzi, Maurizio, Pelizzo, Maria, Reale, Fabio, Romano, Paolo, Sasso, Clementina, Schühle, Udo, Stangalini, Marco, Strachan, Leonard, Straus, Thomas, Teriaca, Luca, Uslenghi, Michela, Verscharen, Daniel, Volpicelli, Cosimo, Zangrilli, Luca, Zimbardo, Gaetano, Zuppella, Paola, 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, Dudok de Wit, Thierry, 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, Thoma, Teriaca, Luca, Uslenghi, Michela, Velli, Marco, Verscharen, Daniel, Volpicelli, Cosimo A., Whittlesey, Phylli, Zangrilli, Luca, Zimbardo, Gaetano, Zuppella, Paola, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, Solar wind, FOS: Physical sciences, Solar radius, Solar corona, Astrophysics, 01 natural sciences, law.invention, Current sheet, Orbiter, Magnetohydrodynamics, Interplanetary turbulence, Heliosphere, Physics - Space Physics, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Coronagraph, Solar and Stellar Astrophysics (astro-ph.SR), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Space plasmas, Astronomy and Astrophysics, Plasma, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Corona, Space Physics (physics.space-ph), [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Physics - Plasma Physics, Plasma Physics (physics.plasm-ph), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-DATA-AN]Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an]
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
Full Text
View/download PDF

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