Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · 2110.11031

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

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

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.

Explore related subjects

astro-ph.SRphysics.plasm-phphysics.space-ph

Keep this discovery

BibTeXRIS

Daniele Telloni, Vincenzo Andretta, Ester Antonucci, Alessandro Bemporad, Giuseppe E. Capuano, Silvano Fineschi, Silvio Giordano, Shadia Habbal, Denise Perrone, Rui F. Pinto, Luca Sorriso-Valvo, Daniele Spadaro, Roberto Susino, Lloyd D. Woodham, Gary P. Zank, Marco Romoli, Stuart D. Bale, Justin C. Kasper, Frédéric Auchère, Roberto Bruno, Gerardo Capobianco, Anthony W. Case, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Vania Da Deppo, Yara De Leo, Thierry Dudok de Wit, Federica Frassati, Fabio Frassetto, Keith Goetz, Salvo L. Guglielmino, Peter R. Harvey, Petr Heinzel, Giovanna Jerse, Kelly E. Korreck, Federico Landini, Davin Larson, Alessandro Liberatore, Roberto Livi, Robert J. MacDowall, Enrico Magli, David M. Malaspina, Giuseppe Massone, Mauro Messerotti, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Giuseppe Nisticò, Olga Panasenco, Maurizio Pancrazzi, Maria G. Pelizzo, Marc Pulupa, Fabio Reale, Paolo Romano, Clementina Sasso, Udo Schühle, Marco Stangalini, Michael L. Stevens, Leonard Strachan, Thomas Straus, Luca Teriaca, Michela Uslenghi, Marco Velli, Daniel Verscharen, Cosimo A. Volpicelli, Phyllis Whittlesey, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella. 2021-10-21. Exploring the Solar Wind from its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter - Parker Solar Probe Quadrature. https://doi.org/10.3847/2041-8213%2Fac282f

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Eclipse Properties and Superhump Evolution in the SU UMa-Type Dwarf Nova Z Cha

The advent of large-scale time-domain surveys provides both opportunities and challenges for understanding accretion disk evolution in cataclysmic variables (CVs). Using high-cadence photometry from the Transiting Exoplanet Survey Satellite (TESS), we investigate the eclipsing SU UMa-type dwarf nova Z Cha. Leveraging eclipses as a natural probe, we examine the evolution of the accretion disk through variations in eclipse depth, O--C of eclipse minima, and positive superhump (PSH) amplitude. During superoutbursts, all three quantities exhibit quasi-periodic modulations with a common period of $\sim$2 days, consistent with the precession period of an eccentric disk. We interpret these correlated variations as evidence of an eccentric, precessing disk: O--C traces the periodic shift of the system's brightness center, while eclipse depth and PSH amplitude vary with the orientation of the disk bulge relative to the line of sight. In quiescence (Sectors 13 and 93), PSHs with periods of $\sim$0.0762 days show linearly decreasing amplitudes and periods, indicating gradual shrinkage of the eccentric disk and a slowing precession. Remarkably, a coherent signal with a period of $\sim$0.0729~days ($\epsilon^{-}\approx-0.02$) appears in the same quiescent intervals. This signal may represent negative superhumps (NSHs) coexisting with PSHs, although an orbital sideband of the PSH cannot presently be excluded with the available data. If confirmed as NSHs, their coexistence with PSHs would challenge the classical tilted-disk model, and could be explained by retrograde apsidal precession of an eccentric disk, where the inner disk precesses retrogradely (NSHs) and the outer disk progradely (PSHs); this interpretation remains to be tested by further observations.

astro-ph.SR↗
arXiv2026

Classical Nova V1405 Cas Had $M_{\rm ejecta}$$>$$M_{\rm accreted}$ and so is Unlikely to be a Type Ia Supernova Progenitor

Nova 2021 Cassiopeia (V1405 Cas) was an ordinary J(175) neon nova with the white dwarf mass estimated to be $M_{\rm WD}$=0.60$\pm$0.10 $M_{\odot}$. I found an orbital period of $P$=0.1884 days, and have tracked 20 times of photometric minima from 2013--2025. I measure that $P$ increased from before to after the eruption with $P_{\rm pre}$=0.1883919$\pm$0.0000018 days and $P_{\rm post}$=0.1884043$\pm$0.0000018 days, for $\Delta P$/$P$=66$_{-18}^{+21}$ parts-per-million. With correction for the angular momentum loss by the binary during the eruption, I derive that the nova ejected $M_{\rm ejecta}$=7.5$\times$10$^{-4}$ $M_{\odot}$, with an extreme range of (2.9--40)$\times$10$^{-4}$ $M_{\odot}$. The mass accreted during the previous eruption cycle comes from the trigger mass, and is $M_{\rm accreted}$=(1.6$\pm$0.4)$\times$10$^{-4}$ $M_{\odot}$. V1405 Cas provides counterexamples against five claims about CV evolution that have dominated since the 1980s. First, V1405 Cas has positive $\dot{P}$, and this is contrary to the Magnetic Braking Model. Second, the $\Delta P$ is 20$\times$ too small to allow the system to fade into a hibernation state. Third, $M_{\rm WD}$ is decreasing over time, as shown by $M_{\rm ejecta}$$>$$M_{\rm accreted}$ and by being a neon nova. Fourth, V1405 Cas is not a Type Ia supernova progenitor, for the same reasons. Fifth, the orbital period of V1405 Cas increased by $+$75 ppm from 2013--2025, as a counterexample to the pervasive idea that cataclysmic variables are universally declining in period from evolution. V1405 Cas is the latest of recent measures of $\Delta P$ and $\dot{P}$ for 52 cataclysmic variables and 25 X-ray binaries that have together refuted all five claims.

astro-ph.SR↗
arXiv2026

A prolonged plateau-to-tail transition in the Type II supernova SN2025abyc

We present optical photometric and spectroscopic observations of the Type II supernova SN2025abyc. During the optically thick phase between approximately 10 and 70 d after explosion, its light curves show strongly wavelength-dependent decline rates of approximately 2.7, 2.1, 0.9, and 0.8 mag/100d in the g, c, r, and o bands, respectively. At approximately 70 d, the light curves begin to depart from their nearly linear plateau evolution and gradually transition toward the radioactive tail. A Fermi-Dirac fit to the well-sampled ATLAS o-band light curve yields a transition midpoint of t_PT ~ 100.5d. The interval between the end of the linear plateau and this transition midpoint is approximately 30 d, indicating a prolonged plateau-to-tail transition. This timescale is comparable to those measured for SN2013by, SN2013ej, and SN2014G. Spectroscopically, at +13 d post-explosion, the Halpha profile appears weak and broad, whereas Hbeta and Hgamma display clear P-Cygni profiles. This morphology can be explained by the normal early spectroscopic evolution of SNe II, although partial filling of the Halpha absorption trough by emission associated with circumstellar interaction cannot be excluded. SN2025abyc otherwise follows the general photospheric velocity evolution of SNe II, while remaining toward the high-velocity side of the comparison distribution in Halpha, Hbeta, and FeII. Exploratory light-curve modelling suggests a synthesized Ni mass of approximately 0.03-0.04 solar mass. We suggest that the extended circumstellar environment, Ni distribution, and hydrogen-envelope structure could all play a role in shaping the observed light-curve evolution, particularly the prolonged plateau-to-tail transition.

astro-ph.SR↗