Results 21 to 30 of about 5,220,245 (377)
The Astrophysical Journal Letters, 2023 We present a U-corrected Pb–Pb age of 4566.19 ± 0.20 Ma (1.11 ± 0.26 Myr after t _0 ) for the moderately volatile element rich, andesitic meteorite Erg Chech 002 (EC002). Our Al–Mg isochron defines a ^26 Al/ ^27 Al initial ratio of (8.65 ± 0.09) × 10 ^−6
J. N. Connelly +5 more
doaj +1 more source
The Astrophysical Journal, 2023 In protostellar cores, sulfur species are effective probes for the energetic environments, such as shocked regions. With the majority of sulfur depleted on dust grains, sulfur-bearing molecules could be liberated back to gas phase by shocks associated ...
Ziwei E. Zhang +7 more
doaj +1 more source
A tale of planet formation: from dust to planets [PDF]
Research in Astronomy and Astrophysics, 2020 The characterization of exoplanets and their birth protoplanetary disks has enormously advanced in the last decade. Benefitting from that, our global understanding of the planet formation processes has been substantially improved.
Beibei Liu, J. Ji
semanticscholar +1 more source
A New Window into Planet Formation and Migration: Refractory-to-Volatile Elemental Ratios in Ultra-hot Jupiters [PDF]
, 2020 A primary goal of exoplanet characterization is to use a planet’s current composition to understand how that planet formed. For example, the C/O ratio has long been recognized as carrying important information on the chemistry of volatile species ...
J. Lothringer +5 more
semanticscholar +1 more source
Silicate Melting and Vaporization During Rocky Planet Formation [PDF]
Journal of Geophysical Research: Planets, 2020 Collisions that induce melting and vaporization can have a substantial effect on the thermal and geochemical evolution of planets. However, the thermodynamics of major minerals are not well known at the extreme conditions attained during planet formation.
E. Davies +6 more
semanticscholar +1 more source
A Case of Simultaneous Star and Planet Formation [PDF]
Astrophysical Journal, 2020 While it is widely accepted that planets are formed in protoplanetary disks, there is still much debate on when this process happens. In a few cases protoplanets have been directly imaged, but for the vast majority of systems, disk gaps and cavities—seen
F. Alves +7 more
semanticscholar +1 more source
Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc [PDF]
, 2020 We explore the impact of outer stellar companions on the occurrence rate of giant planets detected with radial velocities. We searched for stellar and planetary companions to a volume-limited sample of solar-type stars within 25 pc. Using adaptive optics
L. Hirsch +12 more
semanticscholar +1 more source
A giant exoplanet orbiting a very-low-mass star challenges planet formation models [PDF]
Science, 2019 A small star hosts a big planet M dwarfs, the most common type of star, are low-mass objects that emit most of their faint light in the near-infrared, making it difficult to detect any orbiting exoplanets. Morales et al.
J. C. Morales +209 more
semanticscholar +1 more source
The Role of Early Giant-planet Instability in Terrestrial Planet Formation [PDF]
, 2020 The terrestrial planets are believed to have formed by violent collisions of tens of lunar- to Mars-size protoplanets at time t < 200 Myr after the protoplanetary gas disk dispersal (t 0).
D. Nesvorný, F. Roig, R. Deienno
semanticscholar +1 more source
Effect of pebble flux-regulated planetesimal formation on giant planet formation [PDF]
Astronomy & Astrophysics, 2020 Context. The formation of gas giant planets by the accretion of 100 km diameter planetesimals is often thought to be inefficient. A diameter of this size is typical for planetesimals and results from self-gravity.
O. Voelkel +4 more
semanticscholar +1 more source