Results 101 to 110 of about 17,020 (222)
Trajectories of ballistic impact ejecta on a rotating Earth [PDF]
On an airless, slowly rotating planetary body like the Moon, ejecta particles from an impact follow simple ballistic trajectories. If gaseous interactions in the fireball are ignored, ejecta particles follow elliptical orbits with the center of the ...
Alvarez, W.
core
We present 1800 multiwavelength Type Ib/c supernovae light-curve models obtained by running the radiation transport code Sedona and varying the mass distribution, velocity profile, and abundance ejecta profiles of helium star progenitors.
S. Karthik Yadavalli +5 more
doaj +1 more source
Delivery of DART Impact Ejecta to Mars and Earth: Opportunity for Meteor Observations
NASA’s Double Asteroid Redirection Test (DART) and ESA’s Hera missions offer a unique opportunity to investigate the delivery of impact ejecta to other celestial bodies. We performed ejecta dynamical simulations using 3 million particles categorized into
Eloy Peña-Asensio +3 more
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Ejecta Mass Estimates from the DART Impact Plume Inferred from LICIACube Images
We report ejecta mass estimates produced by the Double Asteroid Redirection Test impact with Dimorphos, the secondary of the Didymos asteroid binary system.
Ramin Lolachi +13 more
doaj +1 more source
Probing Shocked Ejecta in SN 1987A: A Novel Diagnostic Approach Using XRISM-Resolve
Supernova (SN) 1987A is one of the best candidates to exploit the capabilities of the freshly launched XRISM satellite. This celestial object offers the unique opportunity to study the evolution of an SN into a young supernova remnant. To date, the X-ray
Vincenzo Sapienza +12 more
doaj +1 more source
Nonthermal Ionization of Kilonova Ejecta: Observable Impacts
The characteristic rapid rise and decline at optical wavelengths of a kilonova is the product of the low ejecta mass (≲0.05 M _⊙ ) and high ejecta velocity (≳0.1 c ). We show that, even at very early times (≲2 days), regions of ejecta fall below critical
R. Margutti +7 more
core +1 more source
Origin of α-poor Very Metal-poor Stars
Among very metal-poor (VMP) stars, α -poor VMP ( α -PVMP) stars that have subsolar values of [X/Fe] for Mg and other α elements are rare and are thought to have been formed from gas polluted by Type 1a supernova (SN 1a). However, recent analyses indicate
S. K. Jeena, Projjwal Banerjee
doaj +1 more source
The martian tropical water ice spatial and temporal distribution was characterized using impact crater ejecta type, location, size, and age in one of two epochs, ≤3.4 Ga and >3.4 Ga, using statistical models designed for spatial and temporal correlation ...
Jamie D. Riggs, Michelle R. Kirchoff
doaj +1 more source
Contemporaneous formation of self-secondaries and layered ejecta deposits on Mars
Self-secondaries are secondary craters formed in cogenetic ejecta deposits. Bearing important information on cratering mechanics and the applicability of remote age-determination technique using crater statistics, the spatial distribution of self ...
Fanglu Luo +7 more
doaj +1 more source

