G. Cozzo
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View article: On the Connection of Coronal Loop Plasma with the Ambient Magnetic Field
On the Connection of Coronal Loop Plasma with the Ambient Magnetic Field Open
Solar coronal loops are magnetically confined plasma structures whose properties are closely linked to the ambient magnetic field. Using 3D magnetohydrodynamic simulations of kink-unstable coronal flux tubes, we investigate how the intensi…
View article: Coronal energy release by MHD avalanches
Coronal energy release by MHD avalanches Open
Context. Outflows perpendicular to the guide field are believed to be a possible signature of magnetic reconnection in the solar corona. Specifically, outflows can help detect the occurrence of ubiquitous small-angle magnetic reconnection.…
View article: Coronal energy release by MHD avalanches III. Identification of a reconnection outflow from a nanoflare
Coronal energy release by MHD avalanches III. Identification of a reconnection outflow from a nanoflare Open
Outflows perpendicular to the guide field are believed to be a possible signature of magnetic reconnection in the solar corona and specifically a way to detect the occurrence of ubiquitous small-angle magnetic reconnection. The aim of this…
View article: Coronal energy release by MHD avalanches
Coronal energy release by MHD avalanches Open
Context. Magnetohydrodynamic (MHD) instabilities, such as the kink instability, can trigger the chaotic fragmentation of a twisted magnetic flux tube into small-scale current sheets that dissipate as aperiodic impulsive heating events. In …
View article: Coronal energy release by MHD avalanches II. EUV line emission from a multi-threaded coronal loop
Coronal energy release by MHD avalanches II. EUV line emission from a multi-threaded coronal loop Open
MHD kink instability can trigger the fragmentation of a twisted magnetic flux tube into small-scale current sheets that dissipate as aperiodic impulsive heating events. This instability propagates as an avalanche to nearby flux tubes and l…
View article: Coronal energy release by MHD avalanches
Coronal energy release by MHD avalanches Open
Context. A possible key element for large-scale energy release in the solar corona is a magnetohydrodynamic (MHD) kink instability in a single twisted magnetic flux tube. An initial helical current sheet progressively fragments in a turbul…
View article: Coronal energy release by MHD avalanches. Effects on a structured, active region, multi-threaded coronal loop
Coronal energy release by MHD avalanches. Effects on a structured, active region, multi-threaded coronal loop Open
A possible key element for large-scale energy release in the solar corona is an MHD kink instability in a single twisted magnetic flux tube. An initial helical current sheet fragments in a turbulent way into smaller-scale sheets, similarly…
View article: Asymmetric Twisting of Coronal Loops
Asymmetric Twisting of Coronal Loops Open
The bright solar corona entirely consists of closed magnetic loops rooted in the photosphere. Photospheric motions are important drivers of magnetic stressing, which eventually leads to energy release into heat. These motions are chaotic a…
View article: The GRAVITY young stellar object survey
The GRAVITY young stellar object survey Open
Context. Hot atomic hydrogen emission lines in pre-main sequence stars serve as tracers for physical processes in the innermost regions of circumstellar accretion disks, where the interaction between a star and disk is the dominant influen…
View article: The GRAVITY Young Stellar Object survey -- IX. Spatially resolved\n kinematics of hot hydrogen gas in the star/disk interaction region of T Tauri\n stars
The GRAVITY Young Stellar Object survey -- IX. Spatially resolved\n kinematics of hot hydrogen gas in the star/disk interaction region of T Tauri\n stars Open
Aims: We aim to spatially and spectrally resolve the Br-gamma hydrogen\nemission line with the methods of interferometry in order to examine the\nkinematics of the hydrogen gas emission region in the inner accretion disk of a\nsample of so…