Abstract The snowlines of various volatile species in protoplanetary disks are associated with abrupt changes gas composition and dust physical properties. Volatiles may affect growth, as they cover grains icy mantles that can change the fragmentation velocity grains. In turn, coagulation, fragmentation, drift through disk contribute to redistribution volatiles between ice phases. Here we prese...

The atmospheric chemical composition of a hot Jupiter can lead to insights into where in its natal protoplanetary disk it formed and subsequent migration pathway. We use 1-D kinetics code compute suite models across range elemental abundances investigate the resultant key molecules jupiter atmospheres. Our parameter sweep spans metallicities between 0.1x 10x solar values for C/H, O/H N/H ratios...

Abstract To date, at least three comets—2I/Borisov, C/2016 R2 (PanSTARRS), and C/2009 P1 (Garradd)—have been observed to have unusually high CO concentrations compared water. We attempt explain these observations by modeling the effect of drifting solid (ice dust) material on ice compositions in protoplanetary disks. find that, independent exact disk model parameters, we always obtain a region ...

Remote sensing methods to derive snow properties using both optical and SAR data are presented. The assimilation of the remote sensing products in the water balance and rainfall-runoff model LARSIM is demonstrated. The flood forecast centre in Karlsruhe applies LARSIM for the operational runoff forecast of the Neckar in the South West of Germany. A fully automatic algorithm to derive snow cover...

Abstract This study investigates stagnation conditions of the Pensilungpa glacier, western Himalaya. Multiple glacier parameters (length, area, debris extent and thickness, snowline altitude (SLA), velocity, downwasting ice cliffs) were studied using field measurements (2016–18), high-resolution imagery from GoogleEarth (2013–17) spaceborne Landsat, ASTER SRTM data (1993–2017) to comprehend gla...

Incremental particle growth in turbulent protoplanetary nebulae is limited by a combination of barriers that can slow or stall growth. Moreover, particles grow massive enough to decouple from the gas are subject inward radial drift which could lead depletion most disk solids before planetesimals form. Compact probably not realistic. Rather, it more likely grains as fractal aggregates may overco...

Abstract Submillimeter spectral line and continuum emission from the protoplanetary disks envelopes of protostars is a powerful probe their structure, chemistry, dynamics. Here we present benchmark study our modeling code, RadChemT, that for first time uses chemical model to reproduce ALMA C 18 O (2–1), CARMA 12 CO (1–0) N 2 H + observations L1527; this allows us distinguish disk, infalling env...

Context. There are numerous extrasolar giant planets which orbit close to their central stars. These ‘hot-Jupiters’ probably formed in the outer, cooler regions of their protoplanetary disks, and migrated inward to ∼ 0.1 AU. Since these giant planets must have migrated through their inner systems at an early time, it is uncertain whether they could have formed or retained terrestrial planets. A...