A5011303839- Solar and Space Plasma Dynamics
- Ionosphere and magnetosphere dynamics
- Stellar, planetary, and galactic studies
- Atmospheric Ozone and Climate
- Astro and Planetary Science
- Astronomical Observations and Instrumentation
- Gamma-ray bursts and supernovae
- Astronomy and Astrophysical Research
- Calibration and Measurement Techniques
- Geophysics and Gravity Measurements
- Laser-induced spectroscopy and plasma
- Planetary Science and Exploration
- Photocathodes and Microchannel Plates
- Surface Roughness and Optical Measurements
- History and Developments in Astronomy
- Color Science and Applications
- Electrostatics and Colloid Interactions
- Lightning and Electromagnetic Phenomena
- Astrophysics and Cosmic Phenomena
- Mobile Learning in Education
- Isotope Analysis in Ecology
- Fluid Dynamics and Turbulent Flows
- Atmospheric and Environmental Gas Dynamics
- Oceanographic and Atmospheric Processes
- Plasma and Flow Control in Aerodynamics
Osservatorio Astrofisico di Torino
1998-2023
National Institute for Astrophysics
2017-2021
University of Turin
1995-1999
We present a self-consistent empirical model for several plasma parameters of polar coronal hole near solar minimum, derived from observations with the Solar and Heliospheric Observatory Ultraviolet Coronagraph Spectrometer. The describes radial distribution density electrons, H0, O5 + outflow velocity unresolved most probable velocities H0 during period between 1996 November 1997 April. In this Letter, we compare H I Lyα O VI λλ1032, 1037 emission lines spatial models parameters, iterate...
We present a comprehensive and self-consistent empirical model for several plasma parameters in the extended solar corona above polar coronal hole. The is derived from observations with SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) during period between 1996 November 1997 April. compare of H I Lyα O VI λλ1032, 1037 emission lines detailed three-dimensional models iterate optimal consistency measured synthesized observable quantities. Empirical constraints are obtained radial...
ABSTRACT Two meteorite pieces have been recovered in Italy, near the town of Cavezzo (Modena), on 2020 January 4th. The associated fireball was observed evening New Year’s Day by eight all-sky cameras PRISMA network, a partner FRIPON. computed trajectory had an inclination angle approximately 68° and velocity at infinity 12.8 km s−1. Together with relatively low terminal height, estimated as 21.5 km, those values were indicating significant possibility dropping event, additionally confirmed...
view Abstract Citations (13) References (19) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Interpretation of the Observed Plasma ``Turbulent'' Velocities as a Result Magnetic Reconnection in Solar Flares Antonucci, Ester ; Benna, Carlo Somov, Boris V. One distinctive features magnetic reconnection current sheets, which has been proposed primary energy source solar flares, is presence fast plasma outflows, or jets, whose velocities are nearly equal to Alfvén...
The comet C/1996Y1, a member of the Kreutz family Sun-grazing comets, was observed with Ultraviolet Coronagraph Spectrometer (UVCS) aboard Solar and Heliospheric Observatory (SOHO) satellite. Lyα line profile spatial distribution are interpreted in terms theory bow shocks driven by mass-loading. At time observation, 6.8 R☉ from Sun region high-speed wind, difficult to observe directly SOHO instruments but an important for testing models solar wind acceleration heating. We find speed below...
The Ultraviolet Coronagraph Spectrometer is one of the instruments on board Solar and Heliospheric Observatory spacecraft, which was launched in December, 1995. instrument designed to make ultraviolet spectrometric measurements visible polarimetric extended solar corona. Prior launch laboratory were carried out determine system level values for many key performance parameters. Further have been since launch. Presented are descriptions measurement techniques representative results.
Context: Until recently, camera networks designed for monitoring fireballs worldwide were not fully automated, implying that in case of a meteorite fall, the recovery campaign was rarely immediate. This an important limiting factor as most fragile - hence precious meteorites must be recovered rapidly to avoid their alteration. Aims: The Fireball Recovery and InterPlanetary Observation Network (FRIPON) scientific project overcome this limitation. network comprises automated radio deployed...
The Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO) observed a spectacular coronal mass ejection (CME) caused by prominence eruption on 1996 December 23. evolution of ejected material was followed for 1 hr 50 minutes. observation consists series 5 minute exposures, at fixed heliocentric distance 1.5 R in several spectral ranges. Lyman lines hydrogen brighten more than 2 orders magnitude during CME. C III 977.02 Å line is very bright, many...
This Letter presents the observations of first two coronal mass ejections (CMEs) obtained with Ultraviolet Coronagraph Spectrometer SOHO. Both CMEs were observed at high spectral resolution in ultraviolet domain. The event on 1996 June 6-7 was H I Lyα λ1216 and Lyβ λ1026, O VI λλ1032 1037, Si XII λλ499 521 imaged within 1.5 5 R☉. second December 23 several lines cool such as C III λ977, N λλ990-992, V λ630. analysis line profiles has allowed us to determine line-of-sight velocities extended...
The Solar and Heliospheric Observatory (SOHO) Ultraviolet Coronagraph Spectrometer is used to observe the interplanetary He focusing cone within 1 AU. Taken over 2 yr from differing orbit positions, series of observations includes measurements I 584 Å Lyβ intensities. itself spatially well defined, intensity was ~45 R in 1996 December, compared with ~1 for lines sight outward Between December 1998 June, dimmed by a factor 3.3 as level solar activity rose. This first time that interstellar...
We report on a Coronal Mass Ejection (CME) observed June 27, 1999 by the UltraViolet Coronagraph Spectrometer (UVCS) telescope operating board SOHO spacecraft. The CME was also Large Angle Spectroscopic (LASCO). Emission of hot material has been recorded UVCS propagating in front an opening system loops generated CME. evolution structure is highly correlated with loop. data reveal excess broadening doublet lines and enhancement intensity due to motion expanding gas. gas emission seems be...
Abstract The Solar Physics Group at the INAF-Turin Astrophysical Observatory (OATo) is actually involved in different Space Weather (SW) projects and missions. In particular, this currently providing for ESA SWESNET portal two new data analysis tools aimed (1) automated identification of magnetic flux ropes from situ (CME effectiveness tool) (2) arrival prediction CMEs remote sensing propagation forecast tool). also developing numerical future applications interest SW under project...
This study aims to assess the properties and classification of 62 variable stars in Cygnus, little studied since their discovery originally reported Information Bulletin on Variable Stars (IBVS) 1302. Using data from previous studies several astronomical databases, we performed our analysis mainly utilizing a period software comparing photometric characteristics variables Colour-Absolute Magnitude Diagram. For all stars, variability is confirmed. We discovered new significant results for...
This study aims to assess the properties and classification of 40 variable stars in Sagittarius, little studied since their discovery reported Information Bulletin on Variable Stars (IBVS) 985 update. Using data from previous studies several astronomical databases, we performed our analysis mainly utilizing a period software comparing photometric characteristics variables Colour-Absolute Magnitude Diagram. For all stars, variability is confirmed. We discovered new significant results for...