F. La Forgia
A5038098898- Astro and Planetary Science
- Planetary Science and Exploration
- Isotope Analysis in Ecology
- Stellar, planetary, and galactic studies
- Astronomical and nuclear sciences
- Geology and Paleoclimatology Research
- Atmospheric Ozone and Climate
- Geological and Geochemical Analysis
- Astrophysics and Star Formation Studies
- Space Satellite Systems and Control
- Geomagnetism and Paleomagnetism Studies
- Nuclear Physics and Applications
- Astronomical Observations and Instrumentation
- Astronomy and Astrophysical Research
- High-pressure geophysics and materials
- Space exploration and regulation
- Radioactive Decay and Measurement Techniques
- Nuclear physics research studies
- Gamma-ray bursts and supernovae
- Spacecraft and Cryogenic Technologies
- Photocathodes and Microchannel Plates
- Ionosphere and magnetosphere dynamics
- Chemical Thermodynamics and Molecular Structure
- Atomic and Subatomic Physics Research
- Geophysics and Gravity Measurements
University of Padua
2011-2024
Osservatorio Astronomico di Padova
2015-2024
National Institute for Astrophysics
2024
Université Paris Cité
2023
Université de Versailles Saint-Quentin-en-Yvelines
2023
Sorbonne Université
2023
Observatoire de Paris
2023
Centre National de la Recherche Scientifique
2023
Laboratoire d’études spatiales et d’instrumentation en astrophysique
2023
Université Paris Sciences et Lettres
2023
Images from the OSIRIS scientific imaging system onboard Rosetta show that nucleus of 67P/Churyumov-Gerasimenko consists two lobes connected by a short neck. The has bulk density less than half water. Activity at distance Sun >3 astronomical units is predominantly neck, where jets have been seen consistently. rotates about principal axis momentum. surface morphology suggests removal larger volumes material, possibly via explosive release subsurface pressure or creation overhangs sublimation,...
Images of comet 67P/Churyumov-Gerasimenko acquired by the OSIRIS (Optical, Spectroscopic and Infrared Remote Imaging System) imaging system onboard European Space Agency’s Rosetta spacecraft at scales better than 0.8 meter per pixel show a wide variety different structures textures. The data importance airfall, surface dust transport, mass wasting, insolation weathering for cometary evolution, they offer some support subsurface fluidization models loss through ejection large chunks material.
Context. We investigate the formation and evolution of comet nuclei other trans-Neptunian objects (TNOs) in solar nebula primordial disk prior to giant planet orbit instability foreseen by Nice model.
Some active asteroids have been proposed to be formed as a result of impact events1. Because are generally discovered by chance only after their tails fully formed, the process how ejecta evolve into tail has, our knowledge, not directly observed. The Double Asteroid Redirection Test (DART) mission NASA2, in addition having successfully changed orbital period Dimorphos3, demonstrated activation an asteroid resulting from under precisely known conditions. Here we report observations DART with...
Abstract NASA's Double Asteroid Redirection Test (DART) mission was the first to demonstrate asteroid deflection, and mission's Level 1 requirements guided its planetary defense investigations. Here, we summarize DART's achievement of those requirements. On 2022 September 26, DART spacecraft impacted Dimorphos, secondary member Didymos near-Earth binary system, demonstrating an autonomously navigated kinetic impact into with limited prior knowledge for defense. Months subsequent Earth-based...
Aims. The OSIRIS camera onboard the Rosetta spacecraft has been acquiring images of comet 67P/Churyumov-Gerasimenko (67P)'s nucleus at spatial resolutions down to ~0.17 m/px ever since Aug. 2014. These have yielded unprecedented insight into morphological diversity comet's surface. This paper presents an overview regional morphology 67P.
Context. We present an investigation of the surface properties areas on nucleus comet 67P/Churyumov-Gerasimenko.
Context. The Rosetta mission of the European Space Agency has been orbiting comet 67P/Churyumov-Gerasimenko (67P) since August 2014 and is now in its escort phase. A large complement scientific experiments designed to complete most detailed study a ever attempted are onboard Rosetta.
Aims.We derive for the first time size-frequency distribution of boulders on a comet, 67P/Churyumov-Gerasimenko (67P), computed from images taken by Rosetta/OSIRIS imaging system.We highlight possible physical processes that lead to these boulder size distributions.Methods.We used acquired OSIRIS Narrow Angle Camera, NAC, 5 and 6 August 2014.The scale (2.44-2.03m/px) is such ≥7 m can be identified manually extracted datasets with software ArcGIS.We derived both global localized...
Since OSIRIS started acquiring high-resolution observations of the surface nucleus comet 67P/Churyumov-Gerasimenko, over one hundred meter-sized bright spots have been identified in numerous types geomorphologic regions, but mostly located areas receiving low insolation. The are either clustered, debris fields close to decameter-high cliffs, or isolated without structural relation surrounding terrain. They can be up ten times brighter than average at visible wavelengths and display a...
Context. OSIRIS, the scientific imaging system onboard ESA Rosetta spacecraft, has been nucleus of comet 67P/Churyumov-Gerasimenko and its dust gas environment since March 2014. The images serve different goals, from morphology composition studies surface, to motion trajectories grains, general structure coma, intensity jets, distribution, mass loss, production rates.
Context. Since August 2014, the OSIRIS Narrow Angle Camera (NAC) onboard Rosetta spacecraft has acquired high spatial resolution images of nucleus comet 67P/Churyumov-Gerasimenko, down to decimeter scale. This paper focuses on Imhotep region, located largest lobe nucleus, near equator.
This paper describes the spectral modeling of surface Phobos in wavelength range between 0.25 and 4.0 μm. We use complementary data to cover this range: OSIRIS (Optical, Spectroscopic, Infrared Remote Imaging System on board ESA Rosetta spacecraft) reflectance spectrum that Pajola et al. merged with VSK-KRFM-ISM (Videospectrometric Camera (VSK)–Combined Radiometer Photometer for Mars (KRFM)–Imaging Spectrometer (ISM) USSR 2 spectra by Murchie & Erard IRTF (NASA Telescope Facility, Hawaii,...
Aims. 67P/Churyumov-Gerasimenko is the target comet of ESA’s Rosetta mission. After commissioning at end March 2014, Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) onboard Rosetta, started imaging its dust environment to investigate how they change evolve while approaching Sun.
Aims. We provide a detailed morphological analysis of the Aswan site on comet 67P/Churyumov-Gerasimenko (67P). derive size-frequency distribution boulders ≥2 m and correlate this with gravitational slopes for first time comet. perform spectral region to understand if possible surface variegation is related thedifferent textures observable different units.
The study of dust, the most abundant material in cometary nuclei, is pivotal understanding original materials forming Solar system. Measuring coma phase function provides a tool to investigate nature dust. Rosetta/OSIRIS sampled comet 67P/Churyumov–Gerasimenko, covering large angle range small amount time. Twelve series were acquired period from 2015 March 2016 February for this scientific purpose. These data allowed, after stray light removal, measuring shape, its reddening, and reddening...
The Martian satellite Phobos has been observed on 2007 February 24 and 25, during the pre- post-Mars closest approach (CA) of ESA Rosetta spacecraft Mars swing-by. goal observations was determination surface composition different areas Phobos, in order to obtain new clues regarding its nature origin. Near-ultraviolet, visible near-infrared (263.5–992.0 nm) images Phobos's were acquired using Narrow Angle Camera OSIRIS instrument onboard Rosetta. six multi-wavelength sets allowed a...
Context. On 12 November 2014 the European mission Rosetta succeeded in delivering a lander, named Philae, on surface of one smallest, low-gravity and most primitive bodies solar system, comet 67P/Churyumov-Gerasimenko (67P).
Context. During the most recent perihelion passage in 2009 of comet 67P/Churyumov-Gerasimenko (67P), ground-based observations showed an anisotropic dust coma where jet-like features were detected at ~ 1.3 AU from Sun. The current is exceptional as Rosetta spacecraft monitoring nucleus activity since March 2014, when a clear was already surrounding 4.3 Subsequently, OSIRIS camera also witnessed outburst between April 27 and 30, mid-July, rh 3.7−3.6 preperihelion clearly non-isotropic,...
We present experimental phase function and degree of linear polarization curves for seven samples cometary dust analogues namely: ground pieces Allende, DaG521, FRO95002 FRO99040 meteorites, Mg-rich olivine pyroxene, a sample organic tholins. The have been obtained at the IAA Cosmic Dust Laboratory wavelength 520 nm covering angle range from 3{\deg} to 175{\deg}. also provide values backscattering enhancement (BCE) our analogue samples. final goal this work is compare with observational data...
The Wide Angle Camera of the OSIRIS instrument on board Rosetta spacecraft is equipped with several narrowband filters that are centered emission lines and bands various fragment species. These used to determine evolution production spatial distribution gas in inner coma comet 67P time heliocentric distance, here between 2.6 - 1.3 AU pre-perihelion. Our observations indicate observed OH, OI, CN, NH, NH2 mostly produced by dissociative electron impact excitation different parent We conclude...
Abstract The Didymos binary asteroid was the target of Double Asteroid Redirection Test (DART) mission, which intentionally impacted Dimorphos, smaller member system. We used Near-Infrared Spectrograph and Mid-Infrared Instrument instruments on JWST to measure 0.6–5 5–20 μ m spectra approximately two months after DART impact. These observations confirm that belongs S class is most consistent with LL chondrite composition, as previously determined from its 0.6–2.5 reflectance spectrum....